Author name code: berger ADS astronomy entries on 2022-09-14 author:"Berger, Thomas E." OR author:"Berger, Tom" ------------------------------------------------------------------------ Title: 4π Heliospheric Observing System - 4π-HeliOS: Exploring the Heliosphere from the Solar Interior to the Solar Wind Authors: Raouafi, Nour E.; Gibson, Sarah; Ho, George; Laming, J. Martin; Georgoulis, Manolis K.; Szabo, Adam; Vourlidas, Angelos; Mason, Glenn M.; Hoeksema, J. Todd; Velli, Marco; Berger, Thomas; Hassler, Donald M.; Kinnison, James; Viall, Nicholeen; Case, Anthony; Newmark, Jeffrey; Lepri, Susan; Krishna Jagarlamudi, Vamsee; Raouafi, Nour; Bourouaine, Sofiane; Vievering, Juliana T.; Englander, Jacob A.; Shannon, Jackson L.; Perez, Rafael M.; Chattopadhyay, Debarati; Mason, James P.; Leary, Meagan L.; Santo, Andy; Casti, Marta; Upton, Lisa A. Bibcode: 2022cosp...44.1530R Altcode: The 4$\pi$ Heliospheric Observing System (4$\pi$-HeliOS) is an innovative mission concept study for the next Solar and Space Physics Decadal Survey to fill long-standing knowledge gaps in Heliophysics. A constellation of spacecraft will provide both remote sensing and in situ observations of the Sun and heliosphere from a full 4$\pi$-steradian field of view. The concept implements a holistic observational philosophy that extends from the Sun's interior, to the photosphere, through the corona, and into the solar wind simultaneously with multiple spacecraft at multiple vantage points optimized for continual global coverage over much of a solar cycle. The mission constellation includes two spacecraft in the ecliptic and two flying as high as $\sim$70$^\circ$ solar latitude. 4$\pi$-HeliOS will provide new insights into the fundamental processes that shape the whole heliosphere. The overarching goals of the 4$\pi$-HeliOS concept are to understand the global structure and dynamics of the Sun's interior, the generation of solar magnetic fields, the origin of the solar cycle, the causes of solar activity, and the structure and dynamics of the corona as it creates the heliosphere. The mission design study is underway at the Johns Hopkins Applied Physics Laboratory Concurrent Engineering Laboratory (ACE Lab), a premier mission design center, fostering rapid and collaborative mission design evolutions. Title: Thermospheric Drag Sondes: on-demand probes of the lower Thermosphere/Mesosphere system Authors: Berger, Thomas; Pilinski, Marcin; Nock, Kerry; Sutton, Eric; Bernstein, Research Valerie; Aaron, Kim; Warnecke, Mark; Thayer, Jeffrey Bibcode: 2022cosp...44..804B Altcode: The Thermospheric Drag Sonde (TDS) is a system concept designed to provide multiple, affordable, and expendable thermosphere/mesosphere probes in a compact format that can be stored on space stations, like the International Space Station (ISS), and launched on demand. The motivation for the concept is the lack of data on the lower ionosphere/thermosphere/mesosphere (ITM) system (~100 - 300 km AMSL) and the difficulty in sustaining orbital platforms at these very Low Earth Orbit (VLEO) altitudes for periods sufficient to sample a wide variety of conditions in geospace. The TDS concept takes its inspiration from upper atmospheric radiosondes that are launched on demand on balloons to provide critical data for terrestrial weather forecasting models. The recent loss of forty SpaceX Starlink satellites due to unexpectedly large atmospheric drag increases at their staging altitude of 210 km during a minor geomagnetic storm emphasizes the need for improved forecasting and nowcasting information at VLEO altitudes. Probe-on-demand systems such as the TDS would fill a key gap in ITM science and data assimilation in forecasting models. A single TDS consists of a compact storage format that deploys into large, lightweight satellite equipped with one or more accelerometers to directly measure drag effects, a dual-frequency GNSS receiver, a compact radio link, and a passive de-orbit system that enables prompt re-entry after deployment from the ISS. Utilizing innovative spherical profile technology to simplify coefficient of drag calculations, TDS deployments will obtain acceleration and GPS Precise Orbit Determination (POD) data during descent and re-entry, providing neutral density profiles for novel science investigations of the ITM system, forecast model data assimilation, and nowcasting data to inform launch operations. The concept is in development with a notional deployment to the ISS in the 2026 timeframe. Title: Space Weather with Quantified Uncertainty (SWQU): Ensemble Learning for Accurate and Reliable Uncertainty Quantification Authors: Camporeale, Enrico; Bortnik, Jacob; Berger, Thomas; Guedes dos Santos, Luiz Fernando; Hu, Andong Bibcode: 2022cosp...44..865C Altcode: We give an overview of the NASA/NSF funded "Ensemble Learning for Accurate and Reliable Uncertainty Quantification" SWQU project. The objective of the project is to create the algorithmic prototype that will combine a small number of high-fidelity (low error, but computationally expensive) runs from physics-based models with a large number of (possibly) less accurate but faster runs from machine learning models. The goal is to obtain a more accurate overall prediction than any individual model, and an estimation of the associated uncertainties. We showcase application examples ranging from geomagnetic index predictions to solar wind, radiation belt fluxes, and ground based magnetic field forecasting. The core engine of the probabilistic predictions is the Accurate and Reliable Uncertainty Estimate (ACCRUE) model, that is briefly discussed. ACCRUE is able to estimate uncertainties associated to deterministic predictions, by solving a deep learning semi-supervised regression problem. Title: ESA's Human Interplanetary Exploration Radiation Risk Assessment System (HIERRAS) Authors: Heynderickx, Daniel; Berger, Thomas; Jiggens, Piers; Vainio, Rami; Matthiä, Daniel; Lei, Fan; Raukunen, Osku; Sandberg, Ingmar; Clucas, Simon; Truscott, Pete Bibcode: 2022cosp...44.2708H Altcode: The Human Interplanetary Exploration Radiation Risk Assessment System (HIERRAS, ESA Contract No 4000127129/19/NL/HK) is a chain of tools for calculation of human radiological and equipment radiation effects for future interplanetary missions within helio-radii 0.9-1.6 AU. The system uses existing software tools and models rather than creating new tools and focusses on seamless and intuitive interfaces between software modules in order to minimise user intervention in the model chains. This presentation will describe the overall HIERRAS system architecture and the following components: \begin{itemize} \item Development of a Python based application framework to collect user requests, execute model runs and return the results to the users. Data are passed internally as json structures which include a standardised set of descriptive metadata. This HIERRAS framework uses the SPECTIRES Python software to run environment and effects analysis models and tools locally as well as through ESA's Network of Models (NoM) infrastructure. Information on registered users and on run requests and results is maintained in an SQL database. \item Development of a GUI to allow users to set up model configurations, execute model runs and collect the results on a series of web pages. The GUI communicates with the application framework by exchanging json structures. Extensive background information and a user manual are provided as well. \item Use of a response function type approach to handle atmospheric transport and geometry shielding of the primary radiation environment and derivation of radiation quantities inside (and outside) space vehicles and habitats. \item HIERRAS uses the Geant4 GRAS software to simulate 3D particle interactions with planetary atmospheres and surfaces in addition to spacecraft structures, equipment and astronauts. A GRAS pre-processor software tool (GRAPPA, abstract submitted to Scientific Event F2.3) was developed to define position- and epoch-dependent planetary surface geometries based on the Mars Climate Database (MCD v5.3), LIP's SOILCOMPI dataset for Mars's surface composition, and Lunar Prospector gamma-ray spectrometer data for the Moon's surface composition. \item Re-processing and re-calibration of the GOES HEPAD high energy proton flux time series. The data were used to extend the SEPEM reference data with three energy channels (up to 875 MeV). A new background identification and removal algorithm was applied to the dataset. The SAPPHIRE SEP model was updated accordingly. \item Definition of validation and verification procedures using interplanetary mission datasets and outputs from the ROSSINI3 study (ESA Contract No 4000125785/18/NL/GLC). \item Updates to the Geant4 space applications and setting up of docker containers for easy distribution, bypassing Geant4 installation. \end{itemize} Title: Poster Presentation and Discussion Authors: Berger, Thomas Bibcode: 2022cosp...44.2707B Altcode: Poster Presentation and Discussion Title: The Dosis 3D Project On-Board the International Space Sta- Tion - Status and Science Overview of 10 Years of Measurements (2012 - 2022) Authors: Berger, Thomas Bibcode: 2022cosp...44.2691B Altcode: The radiation environment encountered in space differs in nature from that on Earth, consisting mostly of highly energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on Earth for occupational radiation workers. Since the beginning of the space era the radiation exposure during space missions has been monitored with various passive and active radiation instruments. Also, on-board the International Space Station (ISS) a number of area monitoring devices provide data related to the spatial and temporal variation of the radiation field in - and outside the ISS. The aim of the DOSIS 3D (2012 - ongoing) experiment is the measurement of the radiation environment within the European Columbus Laboratory of the ISS. These measurements are, on the one hand, performed with passive radiation detectors mounted at eleven locations within Columbus for the determination of the spatial distribution of the radiation field parameters and, on the other hand, with two active radiation detectors (DOSTEL) mounted at a fixed position inside Columbus for the determination of the temporal variation of the radiation field parameters. The talk will give an overview of the current results of the data evaluation performed for the passive and active radiation detectors for DOSIS 3D in the years 2012 to 2022 and further focus on the work in progress for data comparison with other passive and active radiation detector systems measuring on-board the ISS. Acknowledgments: The participation of the Technische Universität Wien, Atominstitut (ATI), Vienna, Austria in the DOSIS-1 and -2 experiments was supported by the Austrian Space Applications Programme (ASAP) under contract no. 819643. The Polish contribution for the Institute of Nuclear Physics (IFJ), Krakow, Poland was supported by the National Science Center (project No DEC-2012/06/M/ST9/00423). EK greatly acknowledges the possibility to participate in the project to DLR and to the ESA PECS for the financial grant No. PECS4000108464. The participation of the Nuclear Physics Institute of the Czech Academy of Sciences has been supported by the grant of Czech Science Foundation (GACR) No. 15-16622Y. The CAU, University of Kiel was supported by DLR under grants 50WB0826, 50WB1026, 50WB1232, 50WB1533 and 50WB1817. Title: SEP Measurements on the Surface of Mars with the Radiation Assessment Detector (RAD) aboard the Curiosity rover Authors: Ehresmann, Bent; Berger, Thomas; Reitz, Guenther; Guo, Jingnan; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Matthiä, Daniel; Hassler, Donald M. Bibcode: 2022cosp...44.1174E Altcode: Exposure to space radiation remains one of the major risks for human space exploration. Besides the ever-present Galactic Cosmic Radiation (GCR), spontaneous Solar Energetic Particles (SEPs) emitted from the Sun during Coronal Mass Ejections (CMEs) or solar flares, can dominate planetary and interplanetary radiation fields and increase the radiation dose by potentially orders of magnitudes. To better understand SEP propagation throughout the heliosphere and their radial and longitudinal dependencies, space weather monitoring at various location throughout the heliosphere is required. On the surface of Mars, the Radiation Assessment Detector (RAD) aboard NASA's Curiosity rover has been analyzing the radiation environment in Gale crater since 2012. Besides characterizing the radiation dose, RAD is also capable of measuring energy spectra and integral fluxes of charged and neutral particles. For the example of charged particles, RAD can distinguish between different ion species and for low-Z particles also between the different isotopes. RAD's location on the surface of Mars allows for unique space weather observations at 1.5 AU that are directly relevant to understanding particle propagation through the inner heliosphere, and the impact of space weather on future human explorers of the Red Planet. RAD's detailed measurements of SEP events, and other interesting observations, such as arrival times and duration of Forbush Decreases, CMEs, or the occurrence of Co-Rotating Interaction Regions (CIRs) provide valuable data for inter-comparison with measurements from other instrument at Earth and throughout the heliosphere. To contextualize the RAD SEP measurements, it is important to consider that Mars possesses an, albeit thin, atmosphere that can filter out lower-energy particles. Thus, protons need about 150 - 170 MeV to propagate through the atmosphere, reach the surface, and be detected by RAD. During the first nine years of its mission, RAD detected five moderate SEP events on the surface of Mars. As the solar cycle is now progressing towards the next solar maximum, strong SEP events are more likely to occur. Consequently, RAD has measured the two strongest events yet encountered, in the past four months. In this presentation, we will provide an overview of 10 years of SEP event observations on the surface of Mars with the RAD instrument. We will then focus on the last two strongest SEP events: the October 28, 2021 event where dose rates increased by a factor of 2.25; and the February 16, 2022 event where dose rates increased by a factor of 3.5 during the event. Title: Development of the Internal Dosimetry Array for Gateway Authors: Zabori, Balazs; Berger, Thomas; Hirn, Attila; Nagamatsu, Aiko; Gutay, Gergely; Fetter, Viktor; Granja, Carlos; Boersma, Nadine Bibcode: 2022cosp...44.2698Z Altcode: The Gateway space station, to be built in orbit around the Moon in the mid-2020s, will not be protected by the Earth's magnetic field or the atmosphere; hence, astronauts could be exposed to up to 700 times the radiation dose of an average human on Earth from space radiation. The Internal Dosimeter Array (IDA) instrument suite is the very first internal ESA experiment on board Gateway. The IDA payload is accommodated inside the US HALO module within a Payload Bank and it is composed of the following already existing and flight proven instruments: - TRITEL 3D silicon detector telescope provided by Centre for Energy Research (EK); - European Active Dosimeter (EAD) provided by German Aerospace Center (DLR); - Medipix (MPX) detector provided by Advacam s.r.o. (AVD); - PADLES and D-SPACE provided by Japanese Space Agency (JAXA). IDA instruments provide, based on measurements of energy deposition and particle track analysis, particle fluxes and fluences, LET spectra, mean quality factors, absorbed dose and dose equivalent rates, as well as intergrated absorbed dose and dose equivalent from the charged particle component of space radiation. Besides charged particles (electrons, protons, He ions and HZE particles), X-rays and gamma-rays are also measured. The IDA instrument suite covers an overall LET range up to 1470 keV/$\mu$m in water (including the full range of 0.1 - 150 keV/$\mu$m relevant relevant to radiation protection from space radiation), and an absorbed dose rate range between nGy/h and a few hundred mGy/h. IDA data acquisition will start soon after HALO launch and will continue on a long term, including transit and on the final halo-like orbit around the Moon. This final orbit will also pass through the Van Allen radiation belts. Operations will be continuous even during uncrewed periods. The scientific radiation data provided by IDA will help the space dosimetry community to improve radiation physics models for cancer and non-cancer (cardio-vascular system, central nervous system) effects. These are of utmost importance in supporting crew risk assessment for deep space exploration missions, not only in the frame of the Artemis programme but for the future plans of human missions to Mars. Radiation data provided by the Instruments will serve also as inputs for studying radiation effects on electronics in deep space. The present paper gives a brief descripton of the scientific instruments in IDA and an overview of the system level concept of the IDA payload to integrate all required instruments within a Gateway Payload Bank and to provide a system interface between the instrumentation and Gateway onboard system from electrical and software point of view. Title: Solar flare prediction with reduced false positives using a hybrid CNN-ERT machine learning model Authors: Berger, Thomas; Flyer, Natasha; Deshmukh, Varad; van der Sande, Kiera Bibcode: 2022AAS...24043102B Altcode: Solar flare prediction using modern machine learning models has been an active field of research for the past several years. Due to the impulsive, episodic, nature of solar flares, the datasets used to train the models, whether from solar magnetic field or atmospheric imaging instruments, are highly imbalanced: there are always many more "non-flare" data than "flare" data for any given prediction window. This dataset imbalance has two major impacts: one, it forces adaption of training algorithms or model parameters that lead to unacceptably high false-positive rates (FPR); and two, it skews the skill metrics used to evaluate predictive performance of any model.

Here we demonstrate a hybrid Convolutional Neural Network (CNN) and Extremely Randomized Trees (ERT) model that is trained and tested on fully imbalanced Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager (HMI) vector magnetic field data but which achieves a 48% reduction in FPR relative to traditional single-architecture models for a 12-hour forecasting window. The reduction in FPR is accompanied by only a slight reduction in true positive rate (-12%), leading to a slight decrease in the True Skill Score (TSS), but a large increase in the Heidke Skill Score (HSS) and F1 score. The addition of the ERT stage to the "deep learning" CNN model has the added advantage of enabling ranking of magnetogram features used to achieve a high skill flare prediction. We find that the probability of flaring provided by the CNN model is the most predictive input, followed by the Schrijver R-parameter, measures of magnetic field topological complexity, and then the total unsigned vertical current and helicity. The resulting model could be transitioned to operations to increase the short-term forecasting skill of human-in-the-loop solar flare prediction systems currently in use in space weather forecasting offices.

We also demonstrate that the SDO Atmospheric Imaging Assembly (AIA) extreme ultraviolet (EUV) images that are concurrent with the HMI magnetic field data can be used to both replace the NOAA GOES X-ray flare catalog as a source for supervised learning data labels, and as an additional data source for increasing the skill of ML flare prediction models. Title: Decreasing False-alarm Rates in CNN-based Solar Flare Prediction Using SDO/HMI Data Authors: Deshmukh, Varad; Flyer, Natasha; van der Sande, Kiera; Berger, Thomas Bibcode: 2022ApJS..260....9D Altcode: 2021arXiv211110704D A hybrid two-stage machine-learning architecture that addresses the problem of excessive false positives (false alarms) in solar flare prediction systems is investigated. The first stage is a convolutional neural network (CNN) model based on the VGG-16 architecture that extracts features from a temporal stack of consecutive Solar Dynamics Observatory Helioseismic and Magnetic Imager magnetogram images to produce a flaring probability. The probability of flaring is added to a feature vector derived from the magnetograms to train an extremely randomized trees (ERT) model in the second stage to produce a binary deterministic prediction (flare/no-flare) in a 12 hr forecast window. To tune the hyperparameters of the architecture, a new evaluation metric is introduced: the "scaled True Skill Statistic." It specifically addresses the large discrepancy between the true positive rate and the false positive rate in the highly unbalanced solar flare event training data sets. Through hyperparameter tuning to maximize this new metric, our two-stage architecture drastically reduces false positives by ≍48% without significantly affecting the true positives (reduction by ≍12%), when compared with predictions from the first-stage CNN alone. This, in turn, improves various traditional binary classification metrics sensitive to false positives, such as the precision, F1, and the Heidke Skill Score. The end result is a more robust 12 hr flare prediction system that could be combined with current operational flare-forecasting methods. Additionally, using the ERT-based feature-ranking mechanism, we show that the CNN output probability is highly ranked in terms of flare prediction relevance. Title: Zodiacal exoplanets in time (ZEIT) XII: a directly imaged planetary-mass companion to a young Taurus M dwarf star Authors: Gaidos, E.; Hirano, T.; Kraus, A. L.; Kuzuhara, M.; Zhang, Z.; Lee, R. A.; Salama, M.; Berger, T. A.; Grunblatt, S. K.; Ansdell, M.; Liu, M. C.; Harakawa, H.; Hodapp, K. W.; Jacobson, S.; Konishi, M.; Kotani, T.; Kudo, T.; Kurokawa, T.; Nishikawa, J.; Omiya, M.; Serizawa, T.; Tamura, M.; Ueda, A.; Vievard, S. Bibcode: 2022MNRAS.512..583G Altcode: 2021arXiv211008655G; 2021MNRAS.tmp.2819G We report the discovery of a resolved (0.9 arcsec) substellar companion to a member of the 1-5 Myr Taurus star-forming region. The host star (2M0437) is a single mid-M type (Teff ≍ 3100 K) dwarf with a position, space motion, and colour-magnitude that support Taurus membership, and possible affiliation with a ~2.5-Myr-old subgroup. A comparison with stellar models suggests a 2-5 Myr age and a mass of 0.15-0.18M. Although K2 detected quasi-periodic dimming from close-in circumstellar dust, the star lacks detectable excess infrared emission from a circumstellar disc and its H α emission is not commensurate with accretion. Astrometry based on 3 yr of AO imaging shows that the companion (2M0437b) is comoving, while photometry of two other sources at larger separation indicates that they are likely heavily reddened background stars. A comparison of the luminosity of 2M0437b with models suggests a mass of 3-5 MJUP, well below the deuterium burning limit, and an effective temperature of 1400-1500 K, characteristic of a late L spectral type. The H - K colour is redder than the typical L dwarf, but comparable to other directly detected young planets, e.g. those around HR 8799. The discovery of a super-Jupiter around a very young, very low-mass star challenges models of planet formation by either core accretion (which requires time) or disc instability (which requires mass). We also detected a second, comoving, widely separated (75 arcsec) object that appears to be a heavily extincted star. This is certainly a fellow member of this Taurus subgroup and statistically likely to be a bound companion. Title: Passive Radiometry of Subsurface Temperatures Using the Mars 2020 Rimfax Instrument Authors: Siegler, M. A.; White, M. N.; Brovoll, S.; Hamran, S.; Russell, P.; Mellon, M.; Berger, T.; Paige, D. A.; Hausrath, E.; Martinez, G.; Rimfax; Mars 2020 Team Bibcode: 2022LPICo2678.1491S Altcode: We are using a passive radiometry model of the Mars 2020 RIMFAX ground penetrating radar instrument to constrain temperatures and properties of the subsurface. Title: Dielectric Permittivity and Density of the Shallow Martian Subsurface in Jezero Crater Authors: Casademont, T. M.; Hamran, S. -E.; Amundsen, H. E. F.; Eide, S.; Dypvik, H.; Berger, T.; Russell, P. Bibcode: 2022LPICo2678.1513C Altcode: RIMFAX estimates of local radar wave propagation velocity by hyperbola matching. With that, relative dielectric permittivity and bulk rock density are derived. Title: Machine Learning Approaches to Solar-Flare Forecasting: Is Complex Better? Authors: Deshmukh, Varad; Baskar, Srinivas; Bradley, Elizabeth; Berger, Thomas; Meiss, James D. Bibcode: 2022arXiv220208776D Altcode: Recently, there has been growing interest in the use of machine-learning methods for predicting solar flares. Initial efforts along these lines employed comparatively simple models, correlating features extracted from observations of sunspot active regions with known instances of flaring. Typically, these models have used physics-inspired features that have been carefully chosen by experts in order to capture the salient features of such magnetic field structures. Over time, the sophistication and complexity of the models involved has grown. However, there has been little evolution in the choice of feature sets, nor any systematic study of whether the additional model complexity is truly useful. Our goal is to address these issues. To that end, we compare the relative prediction performance of machine-learning-based, flare-forecasting models with varying degrees of complexity. We also revisit the feature set design, using topological data analysis to extract shape-based features from magnetic field images of the active regions. Using hyperparameter training for fair comparison of different machine-learning models across different feature sets, we show that simpler models with fewer free parameters \textit{generally perform better than more-complicated models}, ie., powerful machinery does not necessarily guarantee better prediction performance. Secondly, we find that \textit{abstract, shape-based features contain just as much useful information}, for the purposes of flare prediction, as the set of hand-crafted features developed by the solar-physics community over the years. Finally, we study the effects of dimensionality reduction, using principal component analysis, to show that streamlined feature sets, overall, perform just as well as the corresponding full-dimensional versions. Title: Classification of Solar Flare Magnitudes Using SDO/AIA Movies with 4D Convolutional Neural Networks Authors: van der Sande, Kiera; Berger, Thomas; Flyer, Natasha; Deshmukh, Varad Bibcode: 2021AGUFMNG45B0571V Altcode: Currently, solar flares are labeled with a magnitude based on a single global measurement of the sun -- the peak X-ray intensity over the flaring event, as measured by the GOES satellite. Given that solar flares are local events, human forecasters are then tasked with labeling the active region on the sun associated with the flare. This has potential for errors since it mandates using at least two separate observational systems. Interest has been growing in using imaging instruments to classify flare intensity and location simultaneously. In addition, imaging instruments such as the Solar Dynamics Observatory (SDO) Atmospheric Imaging Assembly (AIA), which provides full-Sun images in ultraviolet and extreme ultraviolet wavelengths, are increasingly used in machine learning (ML) solar flare prediction models, as these images may reveal more features associated with flaring than the photospheric magnetic field data that has been mostly used to date. We demonstrate the use of AIA image cutouts of solar active regions to characterize the peak X-ray magnitude of solar flares via ML regression to the GOES measurements, offering an alternative to using the GOES flare catalog for event location and data labelling. We use a 4D Convolutional Neural Network (CNN) algorithm trained on a temporal series of AIA images in various wavelengths, with the corresponding outputs being the GOES flare magnitude for the event. However, a challenge is that solar flare peak times and the length of flaring vary as a function of wavelength, e.g., the flare peak time in the SDO/AIA 171 Angstrom bandpass (as determined, e.g., by the maximum size of saturated pixels in the flare region) can be as much as 40 minutes after the flare peak in the GOES data). We will address this complication in constructing training databases for the ML algorithm and present preliminary results of our regression modeling. Title: The SWx TREC Space Weather Data Portal: bringing data from diverse sources to the community Authors: Knuth, Jenny; Lucas, Greg; Pankratz, Christopher; Berger, Thomas Bibcode: 2021AGUFMSM52A..08K Altcode: An obstacle to understanding, viewing, and communicating space weather is accessing relevant data. Users spend hours collecting data from disparate sources and repositories. The learning curve for finding relevant data is high, and only the most dedicated make the leap. Datasets are viewed in separate repositories or downloaded and visualized locally with a custom script. It takes specialized skills to bring space weather data together for analysis. This results in space weather often seeming cryptic, invisible, and difficult to grasp. The University of Colorado at Boulders Space Weather Technology, Research, and Education Center (SWx TREC), is working to lower these barriers. SWx TRECs Space Weather Data Portal found at https://lasp.colorado.edu/space-weather-portal, provides uniform access to data housed in various remote repositories. In this presentation I will show how the SWx Data Portal can address the needs of a broad spectrum of end users: from space weather enthusiasts to educators, scientists, and operational professionals. The SWx Data Portal enables users to quickly view and download disparate data relevant to past space weather events, all in one place. The selected data can be easily compared, overplotted, curated, saved, downloaded, and shared. For example, we will demonstrate how the SWx Data Portal can be used to watch the unfolding of a space weather event from its initiation on the Sun to its journey through space to its impacts on the Earth. The relevant coronagraphs and solar images can be easily selected and aligned in time with X-ray flux and particle data. The solar winds speed, density, and temperature along with magnetic field direction and strength can be traced alongside models of satellite drag, D-Region Absorption, and geomagnetically induced currents. All of these data products can be synced and viewed on one screen. Events can be saved, shared, and submitted to the Data Portal's community Event Library. The SWx Data Portal can help bridge the gap between scientists, forecasters, and stakeholders by allowing graphical exploration of space weather data and events. Such tools that connect disparate space weather data will speed understanding and enable clearer communication to policy makers and the public, ultimately protecting against space weathers social and economic impacts. Title: University of Colorado SWx TREC Model Staging Platform: Facilitating Model/Algorithm R2O and O2R Development within a Cloud Computing Environment Authors: Craft, James; Lucas, Greg; Pankratz, Christopher; Berger, Thomas; Sutton, Eric Bibcode: 2021AGUFMSM52A..04C Altcode: The Space Weather Technology, Research and Education Center (SWx TREC) is an emerging national center of excellence in cross-disciplinary research, technology, innovation, and education, intended to facilitate evolving space weather research and forecasting needs. Within this center, we are developing a Space Weather Model Staging Platform (MSP) to facilitate the R2O and O2R pipelines. The MSP leverages cloud computing to provide a managed computational environment for independent science teams to deploy their processing software into an operational-like system. Using cloud computing for the environment enables traditional defined-cadence (daily, hourly) model runs to be scheduled while also providing the ability to submit on-demand runs during storm times with no additional bulk hardware purchases that would otherwise sit idle most of the time. In this presentation, we demonstrate the ways that the MSP is being utilized. First, in the R2O pipeline, we have implemented code from the USGS to produce electric field maps at a set cadence to demonstrate that the code can be run in an operational mode. Second, in the O2R pipeline, we are taking operational codes such as the Enlil Solar Wind Model and the NOAA Whole Atmosphere Model (WAM), and enabling researchers to investigate new data assimilation techniques that can supplement and enhance current operational code capabilities. Finally, we demonstrate the use of cloud resources to generate automatic flare forecasts from satellite images. Title: A New Interactive 3-Dimensional Data Viewer for the Enlil Solar Wind Model Authors: Pankratz, Christopher; Lucas, Greg; Knuth, Jenny; Odstrcil, Dusan; Craft, James; Berger, Thomas Bibcode: 2021AGUFMSM53B..05P Altcode: One of the critical models in space weather forecasting is the Enlil solar wind prediction model that can inform space weather forecasters the direction and speed of coronal mass ejections CMEs. The Enlil code calculates the propagation of the solar wind throughout the 3D heliosphere, but current visualization capabilities in the forecasting offices are restricted to 2D planes intersecting Earth. This limits forecasters to only be able to view CME properties that are traveling directly in the plane of the Earth. Here, we present a new visualization capability being developed to take advantage of the full Enlil 3D data volume and interactively visualize the CME expansion out of the plane of the Earth. This is designed to give forecasters and researchers the full view of the heliosphere in a manner that can be tailored to these different types of users. To accomplish this, we are deploying the Enlil solar wind model into a scalable Cloud-based model staging platform computing environment, which will allow the full 3D Enlil output to reside in-situ with the visualization engine. We will discuss our progress in deploying and running the Enlil model in the Cloud-based testbed environment, the process of interacting with space weather forecasters to design a new interactive 3D visualization tool that meets their needs, and will demonstrate use of the visualization tool itself. Title: From 1973 to the 2020s, from SKYLAB to 3D vector magnetic fields in prominences Authors: Lacatus, Daniela; Judge, Philip; Gilbert, Holly; Paraschiv, Alin; Berger, Thomas Bibcode: 2021AGUFMSH42B..05L Altcode: Routine measurement of the vector magnetic fields threading prominences would mark a significant advance in our ability to determine the dynamics of the Sun's corona. Gilbert et al. (AGU abstract #849653) have identified the near-UV (250-281 nm) as a prime region for measurements of magnetic fields within the chromosphere and lower transition region. Here, we perform an in depth analysis of the near UV spectra of all prominences observed by the SKYLAB SO82B instrument during 1973, for the first time. Using over 100 spectral lines we process the photographic data from scratch, and solve for plasma properties of several prominences. Given the known complexity of the thermal and dynamical conditions within prominence plasma, we develop a model to find mean electron temperatures, densities and mass columns which capture each spectrums essential characteristics. Prominence plasmas are optically thick in the cores of many spectral lines of Fe II and Mg II present in this spectral region. The different optical depths probe different surfaces along the line-of-sight, so that near-UV spectro-polarimetry will uniquely determine vector magnetic fields within the 3D volume of prominences. Therefore, we show that this technique offers the best future method for answering critical problems related to coronal dynamics, not only above active regions as shown by Gilbert et al., but also in prominence plasmas. Title: New Insights into the Martian Radiation Environment gained with the MSL/RAD Investigation Authors: Ehresmann, Bent; Hassler, Don; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Loeffler, Sven; Guo, Jingnan; Khaksarighiri, Salman; Matthiae, Daniel; Berger, Thomas; Reitz, Gunther Bibcode: 2021AGUFM.P24A..02E Altcode: The Mars Science Laboratory / Radiation Assessment Detector (MSL/RAD) has been conducting detailed measurements of the radiation environment in Gale crater on Mars for more than 9 years. Understanding of this radiation field, its composition, and its temporal evolution are vital for the preparation of human exploration missions to Mars. Thereby, protecting astronauts from the effects of space radiation remains a critical step for the exploration of Mars. Long-term exposure to radiation can lead to severe health effects and affects allowable mission duration. Astronauts need to be protected from exposure to both the long-term Galactic Cosmic Ray (GCR)-induced radiation, as well as from short-term, but highly intense Solar Energetic Particles (SEPs). Here, we provide new insights into the changes the Martian radiation field has undergone since the beginning of the MSL mission in mid-2012 (close to solar maximum of solar cycle 24) throughout the deepest part of the solar minimum of cycle 24. We present how the evolving solar cycle has affected dosimetric quantities, such as the RAD-measured absorbed dose rate, Linear Energy Transfer (LET) spectrum, and the biologically highly-important dose equivalent rate. From these measurements, we make estimates of how much radiation astronauts would be exposed to under different mission scenarios and timing. Furthermore, we present new analysis of the natural radiation shielding effect of Martian terrain, measured for the first-time in-situ by MSL/RAD. We find that natural terrain, such as cliff sides or buttes, when high enough, block out part of the incoming GCR radiation, leading to an overall decrease in the measured dose rate. We present data from 5 occasions where such a shielding effect was observed by MSL/RAD and analyze how the angle of vertical obstruction of the natural terrain affects the measured decrease in dose. These first-ever in-situ measurements of the radiation shielding effect are crucial for the planning of radiation shelters for future Mars explorers by providing insight into the angular distribution of the radiation environment on the Martian surface. These measurements are vital to validate radiation transport models used to calculate the effectiveness of proposed radiation shelter designs. Title: Directionality of the Martian Surface Radiation and Derivation of the Upward Albedo Radiation Authors: Guo, Jingnan; Khaksarighiri, Salman; Wimmer-Schweingruber, Robert F.; Hassler, Donald M.; Ehresmann, Bent; Zeitlin, Cary; Löffler, Sven; Matthiä, Daniel; Berger, Thomas; Reitz, Günther; Calef, Fred Bibcode: 2021GeoRL..4893912G Altcode: Since 2012 August, the Radiation Assessment Detector (RAD) on the Curiosity rover has been characterizing the Martian surface radiation field which is essential in preparation for future crewed Mars missions. RAD observed radiation dose is influenced by variable topographical features as the rover traverses through the terrain. In particular, while Curiosity was parked near a butte in the Murray Buttes area, we find a decrease of the dose rate by (5 ± 1)% as 19% of the sky was obstructed, versus 10% in an average reference period. Combining a zenith-angle-dependent radiation model and the rover panoramic visibility map leads to a predicted reduction of the downward dose by ∼12% due to the obstruction, larger than the observed decrease. With the hypothesis that this difference is attributable to albedo radiation coming from the butte, we estimate the (flat-terrain) albedo radiation to be about 19% of the total surface dose. Title: Measuring the Magnetic Origins of Solar Flares, Coronal Mass Ejections, and Space Weather Authors: Judge, Philip; Rempel, Matthias; Ezzeddine, Rana; Kleint, Lucia; Egeland, Ricky; Berdyugina, Svetlana V.; Berger, Thomas; Bryans, Paul; Burkepile, Joan; Centeno, Rebecca; de Toma, Giuliana; Dikpati, Mausumi; Fan, Yuhong; Gilbert, Holly; Lacatus, Daniela A. Bibcode: 2021ApJ...917...27J Altcode: 2021arXiv210607786J We take a broad look at the problem of identifying the magnetic solar causes of space weather. With the lackluster performance of extrapolations based upon magnetic field measurements in the photosphere, we identify a region in the near-UV (NUV) part of the spectrum as optimal for studying the development of magnetic free energy over active regions. Using data from SORCE, the Hubble Space Telescope, and SKYLAB, along with 1D computations of the NUV spectrum and numerical experiments based on the MURaM radiation-magnetohydrodynamic and HanleRT radiative transfer codes, we address multiple challenges. These challenges are best met through a combination of NUV lines of bright Mg II, and lines of Fe II and Fe I (mostly within the 4s-4p transition array) which form in the chromosphere up to 2 × 104 K. Both Hanle and Zeeman effects can in principle be used to derive vector magnetic fields. However, for any given spectral line the τ = 1 surfaces are generally geometrically corrugated owing to fine structure such as fibrils and spicules. By using multiple spectral lines spanning different optical depths, magnetic fields across nearly horizontal surfaces can be inferred in regions of low plasma β, from which free energies, magnetic topology, and other quantities can be derived. Based upon the recently reported successful sub-orbital space measurements of magnetic fields with the CLASP2 instrument, we argue that a modest space-borne telescope will be able to make significant advances in the attempts to predict solar eruptions. Difficulties associated with blended lines are shown to be minor in an Appendix. Title: VizieR Online Data Catalog: A list of ~330000 stars Kepler missed (Wolniewicz+, 2021) Authors: Wolniewicz, L. M.; Berger, T. A.; Huber, D. Bibcode: 2021yCat..51610231W Altcode: In this paper we have analyzed the Kepler mission's target selection function by using Gaia DR2 as the ground truth to characterize the ~500000 stars that Kepler could have observed, and compared this population to the sample of ~200000 stars that were selected for observations.

We started with a subset of 2.4million targets within the KIC that are located in the Kepler field of view, which we downloaded from the Mikulski Archive for Space Telescopes (MAST). As a first step, we cross-matched the KIC with Gaia DR2 to obtain Gaia information for each star in the KIC. To do this, we used the Centre de Donnees astronomiques de Strasbourg (CDS) cross-match.

We conducted a positional match with a matching radius of 5", because the astrometric offsets between the KIC and Gaia have not been well characterized. We removed duplicates by only selecting the Kepler and Gaia ID associated with the most similar magnitudes in the Kepler passband Kp and Gaia passband. We then extracted Gaia Re-normalized unit weight error (RUWE) values for all sources.

(1 data file). Title: Solar Prominence Bubbles and Associated Plasma Instabilities: IRIS and SDO/AIA Observations Authors: Liu, W.; Berger, T. Bibcode: 2021AAS...23811311L Altcode: Solar prominences are cool and dense plasma in the hot corona. The so-called prominence bubbles are mysterious, dome-shaped, apparently void structures residing in the lower portions of prominences. Such bubbles are associated with various plasma instabilities, such as the Rayleigh-Taylor (RT) and Kelvin-Helmholtz (KH) instabilities. The former is manifested in plumes that are often produced at the top boundary of a bubble and intrude upward into the dense prominence material. The latter is found to be triggered by shear flows at the bubble boundaries. We present recent observations of prominence bubbles by IRIS and SDO/AIA, focusing on the diagnostic potential of RT and KH instabilities on the physical conditions of the prominence and its supporting magnetic field. We search for evidence of magnetic flux emergence as the origin of prominence bubbles. We discuss their role in mass ad magnetic flux transport in the solar atmosphere. Title: Rotation Distributions around the Kraft Break with TESS and Kepler: The Influences of Mass, Metallicity, and Binarity Authors: Avallone, E. A.; Tayar, J.; Van Saders, J.; Berger, T.; Claytor, Z. Bibcode: 2021AAS...23831407A Altcode: The year-long lightcurves observed in the southern continuous viewing zone (SCVZ) of the Transiting Exoplanet Survey Satellite (TESS) and the abundance of rotation periods measured with the Kepler Space Telescope provide the ideal laboratory to understand stellar rotation across the main sequence. Here, we find that while we can measure rotation periods from lightcurves in the TESS SCVZ and use TESS lightcurves to identify other classes of stellar variability (e.g. pulsations), instrument systematics prevent the detection of rotation signals longer than the TESS orbital period of 13.7 days. Due to this detection limit, we combine more traditional methods of measuring rotation from spectroscopic data with data from TESS and Kepler to conduct our analysis. Using rotation periods derived from rotational velocities measured by the APOGEE spectroscopic survey and radii inferred using the Gaia mission, we find that we can trace rotation as a function of evolutionary state and analyze the distribution of rotation periods as a function of binarity around the Kraft Break. Additionally, the distribution of detected stars in Kepler and TESS reveals key differences between stellar populations probed by these two missions, with TESS probing a significant population of young stars that were not present in the Kepler sample. Title: Critical Science Plan for the Daniel K. Inouye Solar Telescope (DKIST) Authors: Rast, Mark P.; Bello González, Nazaret; Bellot Rubio, Luis; Cao, Wenda; Cauzzi, Gianna; Deluca, Edward; de Pontieu, Bart; Fletcher, Lyndsay; Gibson, Sarah E.; Judge, Philip G.; Katsukawa, Yukio; Kazachenko, Maria D.; Khomenko, Elena; Landi, Enrico; Martínez Pillet, Valentín; Petrie, Gordon J. D.; Qiu, Jiong; Rachmeler, Laurel A.; Rempel, Matthias; Schmidt, Wolfgang; Scullion, Eamon; Sun, Xudong; Welsch, Brian T.; Andretta, Vincenzo; Antolin, Patrick; Ayres, Thomas R.; Balasubramaniam, K. S.; Ballai, Istvan; Berger, Thomas E.; Bradshaw, Stephen J.; Campbell, Ryan J.; Carlsson, Mats; Casini, Roberto; Centeno, Rebecca; Cranmer, Steven R.; Criscuoli, Serena; Deforest, Craig; Deng, Yuanyong; Erdélyi, Robertus; Fedun, Viktor; Fischer, Catherine E.; González Manrique, Sergio J.; Hahn, Michael; Harra, Louise; Henriques, Vasco M. J.; Hurlburt, Neal E.; Jaeggli, Sarah; Jafarzadeh, Shahin; Jain, Rekha; Jefferies, Stuart M.; Keys, Peter H.; Kowalski, Adam F.; Kuckein, Christoph; Kuhn, Jeffrey R.; Kuridze, David; Liu, Jiajia; Liu, Wei; Longcope, Dana; Mathioudakis, Mihalis; McAteer, R. T. James; McIntosh, Scott W.; McKenzie, David E.; Miralles, Mari Paz; Morton, Richard J.; Muglach, Karin; Nelson, Chris J.; Panesar, Navdeep K.; Parenti, Susanna; Parnell, Clare E.; Poduval, Bala; Reardon, Kevin P.; Reep, Jeffrey W.; Schad, Thomas A.; Schmit, Donald; Sharma, Rahul; Socas-Navarro, Hector; Srivastava, Abhishek K.; Sterling, Alphonse C.; Suematsu, Yoshinori; Tarr, Lucas A.; Tiwari, Sanjiv; Tritschler, Alexandra; Verth, Gary; Vourlidas, Angelos; Wang, Haimin; Wang, Yi-Ming; NSO and DKIST Project; DKIST Instrument Scientists; DKIST Science Working Group; DKIST Critical Science Plan Community Bibcode: 2021SoPh..296...70R Altcode: 2020arXiv200808203R The National Science Foundation's Daniel K. Inouye Solar Telescope (DKIST) will revolutionize our ability to measure, understand, and model the basic physical processes that control the structure and dynamics of the Sun and its atmosphere. The first-light DKIST images, released publicly on 29 January 2020, only hint at the extraordinary capabilities that will accompany full commissioning of the five facility instruments. With this Critical Science Plan (CSP) we attempt to anticipate some of what those capabilities will enable, providing a snapshot of some of the scientific pursuits that the DKIST hopes to engage as start-of-operations nears. The work builds on the combined contributions of the DKIST Science Working Group (SWG) and CSP Community members, who generously shared their experiences, plans, knowledge, and dreams. Discussion is primarily focused on those issues to which DKIST will uniquely contribute. Title: RIMFAX GPR on the MARS 2020 Investigation at Jezero Crater Authors: Hamran, S. -E.; Paige, D. A.; Amundsen, H. E. F.; Berger, T.; Brovoll, S.; Carter, L.; Damsgård, L.; Dypvik, H.; Eide, S.; Ghent, R.; Kohler, J.; Mellon, M.; Nunes, D. C.; Plettemeier, D.; Russell, P. Bibcode: 2021LPI....52.1223H Altcode: The Radar Imager for Mars' Subsurface Experiment (RIMFAX) is a Ground Penetrating Radar on the Mars 2020 mission's Perseverance rover, which is planned to land in Jezero Crater on February 18, 2021. Title: VizieR Online Data Catalog: 117 exoplanets in habitable zone with Kepler DR25 (Bryson+, 2021) Authors: Bryson, S.; Kunimoto, M.; Kopparapu, R. K.; Coughlin, J. L.; Borucki, W. J.; Koch, D.; Aguirre, V. S.; Allen, C.; Barentsen, G.; Batalha, N. M.; Berger, T.; Boss, A.; Buchhave, L. A.; Burke, C. J.; Caldwell, D. A.; Campbell, J. R.; Catanzarite, J.; Chandrasekaran, H.; Chaplin, W. J.; Christiansen, J. L.; Christensen-Dalsgaard, J.; Ciardi, D. R.; Clarke, B. D.; Cochran, W. D.; Dotson, J. L.; Doyle, L. R.; Duarte, E. S.; Dunham, E. W.; Dupree, A. K.; Endl, M.; Fanson, J. L.; Ford, E. B.; Fujieh, M.; Gautier, T. N., III; Geary, J. C.; Gilliland, R. L.; Girouard, F. R.; Gould, A.; Haas, M. R.; Henze, C. E.; Holman, M. J.; Howard, A. W.; Howell, S. B.; Huber, D.; Hunter, R. C.; Jenkins, J. M.; Kjeldsen, H.; Kolodziejczak, J.; Larson, K.; Latham, D. W.; Li, J.; Mathur, S.; Meibom, S.; Middour, C.; Morris, R. L.; Morton, T. D.; Mullally, F.; Mullally, S. E.; Pletcher, D.; Prsa, A.; Quinn, S. N.; Quintana, E. V.; Ragozzine, D.; Ramirez, S. V.; Sanderfer, D. T.; Sasselov, D.; Seader, S. E.; Shabram, M.; Shporer, A.; Smith, J. C.; Steffen, J. H.; Still, M.; Torres, G.; Troeltzsch, J.; Twicken, J. D.; Uddin, A. K.; van Cleve, J. E.; Voss, J.; Weiss, L. M.; Welsh, W. F.; Wohler, B.; Zamudio, K. A. Bibcode: 2021yCat..51610036B Altcode: We present the occurrence rates for rocky planets in the habitable zones (HZs) of main-sequence dwarf stars based on the Kepler DR25 planet candidate catalog and Gaia-based stellar properties. We provide the first analysis in terms of star-dependent instellation flux, which allows us to track HZ planets. We define {eta}{Earth} as the HZ occurrence of planets with radii between 0.5 and 1.5 R{Earth} orbiting stars with effective temperatures between 4800 and 6300K. We find that {eta}{Earth} for the conservative HZ is between 0.37-0.21+0.48 (errors reflect 68% credible intervals) and 0.60-0.36+0.90 planets per star, while the optimistic HZ occurrence is between 0.58-0.33+0.73 and 0.88-0.51+1.28 planets per star. These bounds reflect two extreme assumptions about the extrapolation of completeness beyond orbital periods where DR25 completeness data are available. The large uncertainties are due to the small number of detected small HZ planets. We find similar occurrence rates between using Poisson likelihood Bayesian analysis and using Approximate Bayesian Computation. Our results are corrected for catalog completeness and reliability. Both completeness and the planet occurrence rate are dependent on stellar effective temperature. We also present occurrence rates for various stellar populations and planet size ranges. We estimate with 95% confidence that, on average, the nearest HZ planet around G and K dwarfs is ~6pc away and there are ~4 HZ rocky planets around G and K dwarfs within 10pc of the Sun.

(1 data file). Title: The Stars Kepler Missed: Investigating the Biases Behind the Kepler Target Selection Function Authors: Wolniewicz, L. M.; Berger, T.; Huber, D. Bibcode: 2021AAS...23721104W Altcode: The Kepler Mission revolutionized exoplanet science by obtaining highly precise photometry of 170,000 stars over 4 years. A critical piece of information needed to accurately exploit Kepler data is the Kepler selection function, since nearly 200,000 targets had to be selected for observation from a sample of over a million stars positioned over the Kepler CCDs with minimal information of their evolutionary state, stellar multiplicity, or proper motions. In this talk I will explain how I use Gaia DR2 to reconstruct the Kepler selection function and explore its biases with respect to evolutionary state, stellar multiplicity, and proper motions. By comparing the stars positioned on the Kepler CCDs that were not chosen for observation to those that were, I will present the first evaluation of the biases of the Kepler target selection function. I find that Kepler was complete for stars brighter than Kp = 14 magnitude, unbiased with respect to proper motions, and that the selection function shows some bias against stellar multiplicity, in the sense that stars without companions were preferentially selected for observation. Title: Precise Demographics of Kepler Planets in the Gaia Era Authors: Berger, T. A.; Huber, D.; Van Saders, J.; Gaidos, E.; Tayar, J.; Weiss, L.; Kraus, A. Bibcode: 2021AAS...23731703B Altcode: A major bottleneck for transiting exoplanet demographics has been the lack of precise properties for most of the observed stars, as the transit method measures exoplanet radii relative to their host's radii. We live in a golden era of host star characterization because of access to Gaia Data Release 2 (DR2) photometry, parallaxes, and proper motions, large-scale spectroscopic surveys, and ground-based photometric and spectroscopic follow-up. In this talk, I will present a sharpened view of Kepler exoplanet demographics using Gaia DR2 parallaxes. First, I will present a comprehensive classification of main sequence, subgiant, and giant stars in Kepler target sample. Using revised planet radii and incident fluxes, I will identify the planet radius gap, planets within the hot sub-Neptunian desert, the hot Jupiter inflation trend, and present an updated census of habitable zone planets. I will also present the Gaia-Kepler Stellar Properties Catalog, the first homogeneous Kepler catalog to include stellar ages, in addition to precise radii, masses, and mean stellar densities for Kepler target stars. I will reveal the first observational evidence of a stellar age dependence of the planet radius gap, where sub-Neptunes become super-Earths on roughly Gyr timescales. In addition, I will show that the planet radius valley exhibits a stellar mass dependence and provide stringent constraints that will be required to discern between the theories of core-powered mass-loss and photoevaporation. Finally, I will reveal that most planets within the hot sub-Neptunian desert only entered recently because of their host's evolution, identify Jupiters with large radii at low incident fluxes, and demonstrate that planets in single and multiple transiting systems share the same age distribution. Title: On Cooling Condensation Near Magnetic Null Points and the Formation of Solar Coronal Rain and Prominences Authors: Liu, Wei; Titov, Viacheslav; Downs, Cooper; Antolin, Patrick; Luna, Manuel; Sun, Xudong; Berger, Thomas; Yu, Sijie; Yoffe, Luke Bibcode: 2021cosp...43E.975L Altcode: The Sun's outer atmosphere, the corona, is million-degrees hot and tenuous. Such hot plasma, under certain conditions, can enigmatically undergo a radiative cooling instability and condense into material of 100 times cooler in the form of coronal rain or prominences. Where, when, and how such cooling condensation takes place remain poorly understood. Answers to these questions are not only important in their own right, but also bear implications for the fundamental question of coronal heating and the chromosphere-corona mass cycle. Magnetic fields in the magnetized corona undoubtedly play a crucial role (e.g., by trapping the plasma), but where and how? We report recent imaging and spectroscopic observations from SDO/AIA/HMI and IRIS that can shed light on this puzzle. Through a systematic survey, we found that a large fraction of quiet-Sun condensations preferentially occur at the dips of coronal loops or funnels. Such dips are located at/near magnetic topological features, such as null points and quasi-separatrix layers (QSLs), which are regions characterized by high values of the squashing factor. We also identified evidence of magnetic reconnection at such locations, which can produce favorable conditions, e.g., density enhancement by compression and/or mass trapping in plasmoids, that can trigger run-away radiative cooling. We present proof-of-concept MHD simulations that demonstrate the role of reconnection in transporting cooled mass from overlying, long loops to underlying, short loops where it slides down as coronal rain. We will discuss the significance and broader implications of these results beyond the Sun. Title: The Dosis 3d Project On-Board the International Space Station - Status and Science Overview of 8 Years of Measurements (2012 - 2020) Authors: Berger, Thomas; Burmeister, Soenke Bibcode: 2021cosp...43E1878B Altcode: The radiation environment encountered in space differs in nature from that on Earth, consisting mostly of highly energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on Earth for occupational radiation workers. Since the beginning of the space era the radiation exposure during space missions has been monitored with various passive and active radiation instruments. Also on-board the International Space Station (ISS) a number of area monitoring devices provide data related to the spatial and temporal variation of the radiation field in - and outside the ISS. The aim of the DOSIS 3D (2012 - ongoing) experiment is the measurement of the radiation environment within the European Columbus Laboratory of the ISS. These measurements are, on the one hand, performed with passive radiation detectors mounted at eleven locations within Columbus for the determination of the spatial distribution of the radiation field parameters and, on the other hand, with two active radiation detectors (DOSTEL) mounted at a fixed position inside Columbus for the determination of the temporal variation of the radiation field parameters. The talk will give an overview of the current results of the data evaluation performed for the passive and active radiation detectors for DOSIS 3D in the years 2012 to 2020 and further focus on the work in progress for data comparison with other passive and active radiation detector systems measuring on-board the ISS. Acknowledgments: The participation of the Technische Universität Wien, Atominstitut (ATI), Vienna, Austria in the DOSIS-1 and -2 experiments was supported by the Austrian Space Applications Programme (ASAP) under contract no. 819643. The Polish contribution for the Institute of Nuclear Physics (IFJ), Krakow, Poland was supported by the National Science Center (project No DEC-2012/06/M/ST9/00423). MTA EK greatly acknowledges the possibility to participate in the project to DLR and to the ESA PECS for the financial grant No. PECS4000108464. The participation of the Nuclear Physics Institute of the Czech Academy of Sciences has been supported by the grant of Czech Science Foundation (GACR) No. 15-16622Y. The CAU, University of Kiel was supported by DLR under grants 50WB0826, 50WB1026, 50WB1232, 50WB1533 and 50WB1817. Title: A New Interactive 3-Dimensional Data Viewer for the Enlil Solar Wind Model Authors: Pankratz, C. K.; Lucas, G.; Odstrcil, D.; Craft, J.; Knuth, J.; Berger, T. E. Bibcode: 2020AGUFMSH0030017P Altcode: One of the critical models in space weather forecasting is the Enlil solar wind prediction model that can inform space weather forecasters the direction and speed of coronal mass ejections CMEs. The Enlil code calculates the propagation of the solar wind throughout the 3D heliosphere, but current visualization capabilities in the forecasting offices are restricted to 2D planes intersecting Earth. This limits forecasters to only be able to view CME properties that are traveling directly in the plane of the Earth. Here, we present a new visualization capability being developed to take advantage of the full Enlil 3D data volume and visualize the CME expansion out of the plane of the Earth that is designed to give forecasters the full view of the heliosphere. We will discuss our initial progress in deploying and running the Enlil model in an on-demand mode in a Cloud-based Testbed and will also describe the process of interacting with space weather forecasters to design a tool that meets their needs. Title: Solar Prominence Bubbles and Associated Plasma Instabilities: IRIS Observations and MHD Modeling Authors: Liu, W.; Berger, T. E.; Fan, Y. Bibcode: 2020AGUFMSH0010014L Altcode: Solar prominences are cool and dense plasma in the hot corona. The so-called prominence bubbles are mysterious, dome-shaped, apparently void structures residing in the lower portions of prominences. Such bubbles are associated with various plasma instabilities, such as the Rayleigh-Taylor (RT) and Kelvin-Helmholtz (KH) instabilities. The former is manifested in plumes that are often produced at the top boundary of a bubble and intrude upward into the dense prominence material. The latter is found to be triggered by shear flows at the bubble boundaries. We present recent observations of prominence bubbles by IRIS, focusing on the diagnostic potential of RT and KH instabilities on the physical conditions of the prominence and its supporting magnetic field. We search for evidence of magnetic flux emergence as the origin of prominence bubbles. We also present preliminary 3D MHD simulations of the interaction of a bipole, as a hypothetical bubble, emerging into an overlying prominence-carrying flux-rope system. The simulations can provide further clues to the origin and nature of prominence bubbles. We discuss their roll in mass ad magnetic flux transport in the solar atmosphere. Title: A Cloud-based Testbed environment to help make models more "useful" Authors: Lucas, G.; Pankratz, C. K.; Craft, J.; Knuth, J.; Berger, T. E. Bibcode: 2020AGUFMSA0040001L Altcode: In the quote "All models are wrong, but some are useful", a key point is that a model has to be made useful to the community in some way, even if it may be "wrong". Here, we present a new Cloud-based Modeling Testbed environment that is designed to help fill in the missing "useful" piece when transitioning research models into operational frameworks. We define the usefulness of the models by iteratively engaging with the end-user, space weather forecasters and researchers, during model development to assure that the end product meets the needs of the community. We will present several specific examples of research codes that we have transitioned to running in the Cloud and made available to the public and how community and user feedback has led to a better end product. Title: SWx TREC's Space Weather Data Portal: a launch pad for space weather research Authors: Knuth, J.; Lucas, G.; Pankratz, C. K.; Berger, T. E.; Clark, R. D.; Skov, T. M. Bibcode: 2020AGUFMSM0030018K Altcode: One obstacle to space weather research is the practical challenge of accessing relevant data. Space weather data are housed in disparate repositories, each with its own unique focus , be it solar, magnetospheric, atmospheric , or earth-based. Much of the effort spent acquiring data could instead be spent on space weather research and education.

To address this problem, the Space Weather Technology, Research, and Education Center (SWx TREC), at the University of Colorado, Boulder, in collaboration with the Laboratory for Atmospheric and Space Physics (LASP), has developed the Space Weather Data Portal (https://lasp.colorado.edu/space-weather-portal), a tool built by and for the space weather community.

Through the Data Portal, previously dispersed space weather data are in one unified place, accessible to scientists, students, and curious individuals. The focus is on the users and their ability to discover, display, compare, overplot, and download relevant data. A user can filter for past events then easily display and download data related to that event, from the moment it occurs on the Sun, as it travels through space and the atmosphere, to the impacts it has on the Earth.

Analysis of space weather events via the Data Portal has proved useful for forecaster training and online learning. The community-created Event Library is a short-cut to curated data collections that provide narratives for context and serve as launch pads for further space weather exploration. Title: Detecting spatiotemporal correlation in microflares for improved solar eruption forecasting Authors: Berger, T. E.; Deshmukh, V.; Flyer, N.; Poduval, B. Bibcode: 2020AGUFMSM047..04B Altcode: No abstract at ADS Title: Shape-based Feature Engineering for Solar Flare Prediction Authors: Deshmukh, Varad; Berger, Thomas; Meiss, James; Bradley, Elizabeth Bibcode: 2020arXiv201214405D Altcode: Solar flares are caused by magnetic eruptions in active regions (ARs) on the surface of the sun. These events can have significant impacts on human activity, many of which can be mitigated with enough advance warning from good forecasts. To date, machine learning-based flare-prediction methods have employed physics-based attributes of the AR images as features; more recently, there has been some work that uses features deduced automatically by deep learning methods (such as convolutional neural networks). We describe a suite of novel shape-based features extracted from magnetogram images of the Sun using the tools of computational topology and computational geometry. We evaluate these features in the context of a multi-layer perceptron (MLP) neural network and compare their performance against the traditional physics-based attributes. We show that these abstract shape-based features outperform the features chosen by the human experts, and that a combination of the two feature sets improves the forecasting capability even further. Title: Evidence for Top Quark Production in Nucleus-Nucleus Collisions Authors: Sirunyan, A. M.; Tumasyan, A.; Adam, W.; Ambrogi, F.; Bergauer, T.; Dragicevic, M.; Erö, J.; Escalante Del Valle, A.; Frühwirth, R.; Jeitler, M.; Krammer, N.; Lechner, L.; Liko, D.; Madlener, T.; Mikulec, I.; Rad, N.; Schieck, J.; Schöfbeck, R.; Spanring, M.; Templ, S.; Waltenberger, W.; Wulz, C. -E.; Zarucki, M.; Chekhovsky, V.; Litomin, A.; Makarenko, V.; Suarez Gonzalez, J.; Darwish, M. R.; De Wolf, E. A.; Di Croce, D.; Janssen, X.; Kello, T.; Lelek, A.; Pieters, M.; Rejeb Sfar, H.; Van Haevermaet, H.; Van Mechelen, P.; Van Putte, S.; Van Remortel, N.; Blekman, F.; Bols, E. S.; Chhibra, S. S.; D'Hondt, J.; De Clercq, J.; Lontkovskyi, D.; Lowette, S.; Marchesini, I.; Moortgat, S.; Python, Q.; Tavernier, S.; Van Doninck, W.; Van Mulders, P.; Beghin, D.; Bilin, B.; Clerbaux, B.; De Lentdecker, G.; Delannoy, H.; Dorney, B.; Favart, L.; Grebenyuk, A.; Kalsi, A. 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M.; Jayananda, MK; Kailasapathy, B.; Sonnadara, D. U. J.; Wickramarathna, DDC; Dharmaratna, W. G. D.; Liyanage, K.; Perera, N.; Wickramage, N.; Aarrestad, T. K.; Abbaneo, D.; Akgun, B.; Auffray, E.; Auzinger, G.; Baechler, J.; Baillon, P.; Ball, A. 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J.; Lammel, S.; Lewis, J.; Lincoln, D.; Lipton, R.; Liu, M.; Liu, T.; Lykken, J.; Maeshima, K.; Mason, D.; McBride, P.; Merkel, P.; Mrenna, S.; Nahn, S.; O'Dell, V.; Papadimitriou, V.; Pedro, K.; Pena, C.; Prokofyev, O.; Ravera, F.; Reinsvold Hall, A.; Ristori, L.; Schneider, B.; Sexton-Kennedy, E.; Smith, N.; Soha, A.; Spalding, W. J.; Spiegel, L.; Stoynev, S.; Strait, J.; Taylor, L.; Tkaczyk, S.; Tran, N. V.; Uplegger, L.; Vaandering, E. W.; Wang, M.; Weber, H. A.; Woodard, A.; Acosta, D.; Avery, P.; Bourilkov, D.; Cadamuro, L.; Cherepanov, V.; Errico, F.; Field, R. D.; Guerrero, D.; Joshi, B. M.; Kim, M.; Konigsberg, J.; Korytov, A.; Lo, K. H.; Matchev, K.; Menendez, N.; Mitselmakher, G.; Rosenzweig, D.; Shi, K.; Wang, J.; Wang, S.; Zuo, X.; Joshi, Y. R.; Adams, T.; Askew, A.; Diaz, D.; Habibullah, R.; Hagopian, S.; Hagopian, V.; Johnson, K. F.; Khurana, R.; Kolberg, T.; Martinez, G.; Prosper, H.; Schiber, C.; Yohay, R.; Zhang, J.; Baarmand, M. M.; Butalla, S.; Elkafrawy, T.; Hohlmann, M.; Noonan, D.; Rahmani, M.; Saunders, M.; Yumiceva, F.; Adams, M. R.; Apanasevich, L.; Becerril Gonzalez, H.; Cavanaugh, R.; Chen, X.; Dittmer, S.; Evdokimov, O.; Gerber, C. E.; Hangal, D. A.; Hofman, D. J.; Mills, C.; Oh, G.; Roy, T.; Tonjes, M. B.; Varelas, N.; Viinikainen, J.; Wang, H.; Wang, X.; Wu, Z.; Alhusseini, M.; Bilki, B.; Dilsiz, K.; Durgut, S.; Gandrajula, R. P.; Haytmyradov, M.; Khristenko, V.; Köseyan, O. K.; Merlo, J. -P.; Mestvirishvili, A.; Moeller, A.; Nachtman, J.; Ogul, H.; Onel, Y.; Ozok, F.; Penzo, A.; Snyder, C.; Tiras, E.; Wetzel, J.; Yi, K.; Amram, O.; Blumenfeld, B.; Corcodilos, L.; Eminizer, M.; Gritsan, A. V.; Kyriacou, S.; Maksimovic, P.; Mantilla, C.; Roskes, J.; Swartz, M.; Vámi, T. Á.; Baldenegro Barrera, C.; Baringer, P.; Bean, A.; Bylinkin, A.; Isidori, T.; Khalil, S.; King, J.; Krintiras, G.; Kropivnitskaya, A.; Lindsey, C.; Mcbrayer, W.; Minafra, N.; Murray, M.; Rogan, C.; Royon, C.; Sanders, S.; Schmitz, E.; Tapia Takaki, J. D.; Wang, Q.; Williams, J.; Wilson, G.; Duric, S.; Ivanov, A.; Kaadze, K.; Kim, D.; Maravin, Y.; Mendis, D. R.; Mitchell, T.; Modak, A.; Mohammadi, A.; Rebassoo, F.; Wright, D.; Adams, E.; Baden, A.; Baron, O.; Belloni, A.; Eno, S. C.; Feng, Y.; Hadley, N. J.; Jabeen, S.; Jeng, G. Y.; Kellogg, R. G.; Koeth, T.; Mignerey, A. C.; Nabili, S.; Seidel, M.; Skuja, A.; Tonwar, S. C.; Wang, L.; Wong, K.; Abercrombie, D.; Allen, B.; Bi, R.; Brandt, S.; Busza, W.; Cali, I. A.; Chen, Y.; D'Alfonso, M.; Gomez Ceballos, G.; Goncharov, M.; Harris, P.; Hsu, D.; Hu, M.; Klute, M.; Kovalskyi, D.; Krupa, J.; Lee, Y. -J.; Luckey, P. D.; Maier, B.; Marini, A. C.; Mcginn, C.; Mironov, C.; Narayanan, S.; Niu, X.; Paus, C.; Rankin, D.; Roland, C.; Roland, G.; Shi, Z.; Stephans, G. S. F.; Sumorok, K.; Tatar, K.; Velicanu, D.; Wang, J.; Wang, T. W.; Wang, Z.; Wyslouch, B.; Chatterjee, R. M.; Evans, A.; Guts, S.; Hansen, P.; Hiltbrand, J.; Jain, Sh.; Krohn, M.; Kubota, Y.; Lesko, Z.; Mans, J.; Revering, M.; Rusack, R.; Saradhy, R.; Schroeder, N.; Strobbe, N.; Wadud, M. A.; Acosta, J. G.; Oliveros, S.; Bloom, K.; Chauhan, S.; Claes, D. R.; Fangmeier, C.; Finco, L.; Golf, F.; González Fernández, J. R.; Kravchenko, I.; Siado, J. E.; Snow, G. R.; Stieger, B.; Tabb, W.; Agarwal, G.; Harrington, C.; Iashvili, I.; Kharchilava, A.; McLean, C.; Nguyen, D.; Parker, A.; Pekkanen, J.; Rappoccio, S.; Roozbahani, B.; Alverson, G.; Barberis, E.; Freer, C.; Haddad, Y.; Hortiangtham, A.; Madigan, G.; Marzocchi, B.; Morse, D. M.; Nguyen, V.; Orimoto, T.; Skinnari, L.; Tishelman-Charny, A.; Wamorkar, T.; Wang, B.; Wisecarver, A.; Wood, D.; Bhattacharya, S.; Bueghly, J.; Chen, Z.; Gilbert, A.; Gunter, T.; Hahn, K. A.; Odell, N.; Schmitt, M. H.; Sung, K.; Velasco, M.; Bucci, R.; Dev, N.; Goldouzian, R.; Hildreth, M.; Hurtado Anampa, K.; Jessop, C.; Karmgard, D. J.; Lannon, K.; Li, W.; Loukas, N.; Marinelli, N.; Mcalister, I.; Meng, F.; Mohrman, K.; Musienko, Y.; Ruchti, R.; Siddireddy, P.; Taroni, S.; Wayne, M.; Wightman, A.; Wolf, M.; Zygala, L.; Alimena, J.; Bylsma, B.; Cardwell, B.; Durkin, L. S.; Francis, B.; Hill, C.; Ji, W.; Lefeld, A.; Winer, B. L.; Yates, B. R.; Dezoort, G.; Elmer, P.; Greenberg, B.; Haubrich, N.; Higginbotham, S.; Kalogeropoulos, A.; Kopp, G.; Kwan, S.; Lange, D.; Lucchini, M. T.; Luo, J.; Marlow, D.; Mei, K.; Ojalvo, I.; Olsen, J.; Palmer, C.; Piroué, P.; Stickland, D.; Tully, C.; Malik, S.; Norberg, S.; Barnes, V. E.; Chawla, R.; Das, S.; Gutay, L.; Jones, M.; Jung, A. W.; Mahakud, B.; Negro, G.; Neumeister, N.; Peng, C. C.; Piperov, S.; Qiu, H.; Schulte, J. F.; Trevisani, N.; Wang, F.; Xiao, R.; Xie, W.; Cheng, T.; Dolen, J.; Parashar, N.; Baty, A.; Dildick, S.; Ecklund, K. M.; Freed, S.; Geurts, F. J. M.; Kilpatrick, M.; Kumar, A.; Li, W.; Padley, B. P.; Redjimi, R.; Roberts, J.; Rorie, J.; Shi, W.; Stahl Leiton, A. G.; Tu, Z.; Zhang, A.; Bodek, A.; de Barbaro, P.; Demina, R.; Dulemba, J. L.; Fallon, C.; Ferbel, T.; Galanti, M.; Garcia-Bellido, A.; Hindrichs, O.; Khukhunaishvili, A.; Ranken, E.; Taus, R.; Chiarito, B.; Chou, J. P.; Gandrakota, A.; Gershtein, Y.; Halkiadakis, E.; Hart, A.; Heindl, M.; Hughes, E.; Kaplan, S.; Karacheban, O.; Laflotte, I.; Lath, A.; Montalvo, R.; Nash, K.; Osherson, M.; Salur, S.; Schnetzer, S.; Somalwar, S.; Stone, R.; Thayil, S. A.; Thomas, S.; Acharya, H.; Delannoy, A. G.; Spanier, S.; Bouhali, O.; Dalchenko, M.; Delgado, A.; Eusebi, R.; Gilmore, J.; Huang, T.; Kamon, T.; Kim, H.; Luo, S.; Malhotra, S.; Marley, D.; Mueller, R.; Overton, D.; Perniè, L.; Rathjens, D.; Safonov, A.; Akchurin, N.; Damgov, J.; Hegde, V.; Kunori, S.; Lamichhane, K.; Lee, S. W.; Mengke, T.; Muthumuni, S.; Peltola, T.; Undleeb, S.; Volobouev, I.; Wang, Z.; Whitbeck, A.; Appelt, E.; Greene, S.; Gurrola, A.; Janjam, R.; Johns, W.; Maguire, C.; Melo, A.; Ni, H.; Padeken, K.; Romeo, F.; Sheldon, P.; Tuo, S.; Velkovska, J.; Verweij, M.; Ang, L.; Arenton, M. W.; Cox, B.; Cummings, G.; Hakala, J.; Hirosky, R.; Joyce, M.; Ledovskoy, A.; Neu, C.; Tannenwald, B.; Wang, Y.; Wolfe, E.; Xia, F.; Karchin, P. E.; Poudyal, N.; Sturdy, J.; Thapa, P.; Black, K.; Bose, T.; Buchanan, J.; Caillol, C.; Dasu, S.; De Bruyn, I.; Dodd, L.; Galloni, C.; He, H.; Herndon, M.; Hervé, A.; Hussain, U.; Lanaro, A.; Loeliger, A.; Loveless, R.; Madhusudanan Sreekala, J.; Mallampalli, A.; Pinna, D.; Ruggles, T.; Savin, A.; Shang, V.; Sharma, V.; Smith, W. H.; Teague, D.; Trembath-reichert, S.; Vetens, W.; CMS Collaboration Bibcode: 2020PhRvL.125v2001S Altcode: Ultrarelativistic heavy ion collisions recreate in the laboratory the thermodynamical conditions prevailing in the early universe up to 10-6 sec , thereby allowing the study of the quark-gluon plasma (QGP), a state of quantum chromodynamics (QCD) matter with deconfined partons. The top quark, the heaviest elementary particle known, is accessible in nucleus-nucleus collisions at the CERN LHC, and constitutes a novel probe of the QGP. Here, we report the first evidence for the production of top quarks in nucleus-nucleus collisions, using lead-lead collision data at a nucleon-nucleon center-of-mass energy of 5.02 TeV recorded by the CMS experiment. Two methods are used to measure the cross section for top quark pair production (σt t ¯ ) via the selection of charged leptons (electrons or muons) and bottom quarks. One method relies on the leptonic information alone, and the second one exploits, in addition, the presence of bottom quarks. The measured cross sections, σt t ¯=2.5 4-0.74+0.84 and 2.03-0.64+0.71 μ b , respectively, are compatible with expectations from scaled proton-proton data and QCD predictions. Title: Projected WIMP sensitivity of the XENONnT dark matter experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Angevaare, J. R.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Cimmino, B.; Clark, M.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; Depoian, A.; Di Gangi, P.; Di Giovanni, A.; Di Stefano, R.; Diglio, S.; Elykov, A.; Eurin, G.; Ferella, A. D.; Fulgione, W.; Gaemers, P.; Gaior, R.; Galloway, M.; Gao, F.; Grandi, L.; Hasterok, C.; Hils, C.; Hiraide, K.; Hoetzsch, L.; Howlett, J.; Iacovacci, M.; Itow, Y.; Joerg, F.; Kato, N.; Kazama, S.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Long, J.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Mancuso, A.; Manenti, L.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Martens, K.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Miuchi, K.; Mizukoshi, K.; Molinario, A.; Morå, K.; Moriyama, S.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Qin, J.; Qiu, H.; Ramírez García, D.; Reichard, S.; Rocchetti, A.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Semeria, F.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Takeda, A.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Valerius, K.; Vargas, M.; Volta, G.; Wang, H.; Wei, Y.; Weinheimer, C.; Weiss, M.; Wenz, D.; Wittweg, C.; Xu, Z.; Yamashita, M.; Ye, J.; Zavattini, G.; Zhang, Y.; Zhu, T.; Zopounidis, J. P. Bibcode: 2020JCAP...11..031A Altcode: 2020arXiv200708796T XENONnT is a dark matter direct detection experiment, utilizing 5.9 t of instrumented liquid xenon, located at the INFN Laboratori Nazionali del Gran Sasso. In this work, we predict the experimental background and project the sensitivity of XENONnT to the detection of weakly interacting massive particles (WIMPs). The expected average differential background rate in the energy region of interest, corresponding to (1, 13) keV and (4, 50) keV for electronic and nuclear recoils, amounts to 12.3 ± 0.6 (keV t y)-1 and (2.2± 0.5)× 10-3 (keV t y)-1, respectively, in a 4 t fiducial mass. We compute unified confidence intervals using the profile construction method, in order to ensure proper coverage. With the exposure goal of 20 t y, the expected sensitivity to spin-independent WIMP-nucleon interactions reaches a cross-section of 1.4×10-48 cm2 for a 50 GeV/c2 mass WIMP at 90% confidence level, more than one order of magnitude beyond the current best limit, set by XENON1T . In addition, we show that for a 50 GeV/c2 WIMP with cross-sections above 2.6×10-48 cm2 (5.0×10-48 cm2) the median XENONnT discovery significance exceeds 3σ (5σ). The expected sensitivity to the spin-dependent WIMP coupling to neutrons (protons) reaches 2.2×10-43 cm2 (6.0×10-42 cm2). Title: Main-Sequence Reinflation of Hot Jupiters Authors: Thorngren, D.; Lopez, E.; Fortney, J.; Berger, T.; Huber, D. Bibcode: 2020DPS....5221604T Altcode: The unexpectedly large radii of hot Jupiters is an open question in exoplanetary science for which a large number of explanations have been proposed. We leverage the strong relationship between hot Jupiter radii and incident fluxes to test these hypotheses by examining whether planets inflate as their parent stars brighten along the main sequence. To do this, we first study how the various observable parameters of the system can be used to predict the planetary radius. Next we show that stellar brightening is sufficient to cause detectable reinflation. We then argue that the predictors of radius, especially fractional age, flux, and ZAMS flux, point towards rapid reinflation that keeps pace with stellar brightening. We also find evidence for a delayed cooling effect in the first few gigayears of a planet's life, though it is not sufficient alone to explain the inflation phenomenon. Finally, we identify a negative relationship between stellar metallicity and planet radius (corrected for mass and flux), likely as a result of higher planetary metallicities. Title: Calibrating GONG Magnetograms with End-to-End Instrument Simulation II: Theory of Calibration Authors: Plowman, Joseph E.; Berger, Thomas E. Bibcode: 2020SoPh..295..142P Altcode: 2020arXiv200202490P This is the second of three papers describing an `absolute' calibration of the GONG magnetograph using an end-to-end simulation of its measurement process. In the first paper, we described the GONG instrument and our `end-to-end' simulation of its measurement process. In this paper, we consider the theory of calibration, and magnetograph comparison in general, identifying some of the significant issues and pitfalls. The calibration of a magnetograph is a function of whether or not it preserves flux, independent of its spatial resolution. However, we find that the one-dimensional comparison methods most often used for magnetograph calibration and comparison will show dramatic differences between two magnetograms with differing spatial resolution, even if they both preserve flux. Some of the apparent disagreement between magnetograms found in the literature are likely a result of these instrumental resolution differences rather than any intrinsic calibration differences. To avoid them, spatial resolution must be carefully matched prior to comparing magnetograms or making calibration curves. In the third paper, we apply the lessons learned here to absolute calibration of GONG using our `end-to-end' measurement simulation. Title: Calibrating GONG Magnetograms with End-to-end Instrument Simulation I: Background, the GONG Instrument, and End-to-end Simulation Authors: Plowman, Joseph E.; Berger, Thomas E. Bibcode: 2020SoPh..295..143P Altcode: 2020arXiv200202489P This is the first of three papers describing an `absolute' calibration of the GONG magnetograph using an end-to-end simulation of its measurement process. The input to this simulation is a MURaM 3D MHD photospheric simulation and the output is the corresponding set of simulated data numbers which would be recorded by the GONG detectors. These simulated data numbers are then used to produce `synthetic magnetograms' which can be compared with the simulation inputs. This paper describes the GONG instrument, the MURaM datacube, our instrument simulator, and calculation of synthetic magnetograms, setting the stage for the subsequent two papers. These will first lay groundwork for calibration (and magnetogram comparison in general), then apply them to calibration of GONG using the simulation results. Title: Calibrating GONG Magnetograms with End-to-End Instrument Simulation III: Comparison, Calibration, and Results Authors: Plowman, Joseph E.; Berger, Thomas E. Bibcode: 2020SoPh..295..144P Altcode: 2020arXiv200202486P This is the last of three papers describing an `absolute' calibration of the GONG magnetograph using and end-to-end simulation of its measurement process. The simulation begins with a MURaM 3D MHD datacube and ends with a `synthetic magnetogram' of the corresponding magnetic field values as they would be observed by GONG. We determine a calibration by comparing the synthetic magnetic field measurements with the MURaM magnetic field values that produced them. The previous two papers have described the GONG measurement process (both instrument and data processing), our simulation of it, and the theory of magnetogram comparison and calibration. In this paper, we address some final points on calibration, combine all of this work into a set of calibration curves, and consider the results. We also review the results of the previous two papers for locality of reference. Our calibration indicates that GONG magnetograms underestimate weak flux by a factor of ∼2 near disk center, but that factor decreases to ∼1 as the line-of-sight approaches the limb. A preliminary investigation of the generalizability of these results suggests other instruments will be affected in a similar way. We also find that some differences in previous magnetograph comparisons are artifacts of instrumental resolution which do not reflect an intrinsic calibration difference, and the measurements are more similar than sometimes thought. These results are directly applicable to question of solar wind prediction model accuracies, particularly in the search for the cause of the common discrepancy between predicted solar wind magnetic flux at 1 AU and values measured in situ by current satellite missions. Title: Excess electronic recoil events in XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Angevaare, J. R.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Cimmino, B.; Clark, M.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; Depoian, A.; di Gangi, P.; di Giovanni, A.; di Stefano, R.; Diglio, S.; Elykov, A.; Eurin, G.; Ferella, A. D.; Fulgione, W.; Gaemers, P.; Gaior, R.; Galloway, M.; Gao, F.; Grandi, L.; Hasterok, C.; Hils, C.; Hiraide, K.; Hoetzsch, L.; Howlett, J.; Iacovacci, M.; Itow, Y.; Joerg, F.; Kato, N.; Kazama, S.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Long, J.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Mancuso, A.; Manenti, L.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Martens, K.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Miuchi, K.; Mizukoshi, K.; Molinario, A.; Morâ, K.; Moriyama, S.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Qin, J.; Qiu, H.; Ramírez García, D.; Reichard, S.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Semeria, F.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Takeda, A.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Vargas, M.; Volta, G.; Wang, H.; Wei, Y.; Weinheimer, C.; Weiss, M.; Wenz, D.; Wittweg, C.; Xu, Z.; Yamashita, M.; Ye, J.; Zavattini, G.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Xenon Collaboration, Mougeot, X. Bibcode: 2020PhRvD.102g2004A Altcode: 2020arXiv200609721A We report results from searches for new physics with low-energy electronic recoil data recorded with the XENON1T detector. With an exposure of 0.65 tonne-years and an unprecedentedly low background rate of 76 ±2stat events /(tonne ×year ×keV ) between 1 and 30 keV, the data enable one of the most sensitive searches for solar axions, an enhanced neutrino magnetic moment using solar neutrinos, and bosonic dark matter. An excess over known backgrounds is observed at low energies and most prominent between 2 and 3 keV. The solar axion model has a 3.4 σ significance, and a three-dimensional 90% confidence surface is reported for axion couplings to electrons, photons, and nucleons. This surface is inscribed in the cuboid defined by gae<3.8 ×10-12 , gaeganeff<4.8 ×10-18 , and gaega γ<7.7 ×10-22 GeV-1 , and excludes either gae=0 or gaega γ=gaeganeff=0 . The neutrino magnetic moment signal is similarly favored over background at 3.2 σ , and a confidence interval of μν∈(1.4 ,2.9 )×10-11 μB (90% C.L.) is reported. Both results are in strong tension with stellar constraints. The excess can also be explained by β decays of tritium at 3.2 σ significance with a corresponding tritium concentration in xenon of (6.2 ±2.0 )×10-25 mol /mol . Such a trace amount can neither be confirmed nor excluded with current knowledge of its production and reduction mechanisms. The significances of the solar axion and neutrino magnetic moment hypotheses are decreased to 2.0 σ and 0.9 σ , respectively, if an unconstrained tritium component is included in the fitting. With respect to bosonic dark matter, the excess favors a monoenergetic peak at (2.3 ±0.2 ) keV (68% C.L.) with a 3.0 σ global (4.0 σ local) significance over background. This analysis sets the most restrictive direct constraints to date on pseudoscalar and vector bosonic dark matter for most masses between 1 and 210 keV /c2 . We also consider the possibility that 37Ar may be present in the detector, yielding a 2.82 keV peak from electron capture. Contrary to tritium, the 37Ar concentration can be tightly constrained and is found to be negligible. Title: VizieR Online Data Catalog: Gaia-Kepler stellar properties catalog. II. Planets (Berger+, 2020) Authors: Berger, T. A.; Huber, D.; Gaidos, E.; van Saders, J. L.; Weiss, L. M. Bibcode: 2020yCat..51600108B Altcode: We computed the updated planet radii utilizing the planet-to-star radius ratios provided in the KOI table from the NASA Exoplanet Archive and the stellar radii computed in Paper I (Berger+, 2020, J/AJ/159/280). In addition, we updated semimajor axes using the stellar masses in Paper I and the orbital periods in Thompson+, 2018, J/ApJS/235/38. Finally, we updated the incident fluxes for each planet by using the semimajor axes and stellar luminosities from Paper I.

(1 data file). Title: VizieR Online Data Catalog: Stellar parameters for 13196 Kepler dwarfs (Angus+, 2020) Authors: Angus, R.; Beane, A.; Price-Whelan, A. M.; Newton, E.; Curtis, J. L.; Berger, T.; van Saders, J.; Kiman, R.; Foreman-Mackey, D.; Lu, Y.; Anderson, L.; Faherty, J. K. Bibcode: 2020yCat..51600090A Altcode: We used the publicly available Kepler-Gaia DR2 crossmatched catalog to combine the McQuillan+ (2014, J/ApJS/211/24) catalog of stellar rotation periods, measured from Kepler light curves, with the Gaia DR2 catalog of parallaxes, proper motions, and apparent magnitudes.

(1 data file). Title: VizieR Online Data Catalog: Gaia-Kepler stellar properties catalog.I. KIC stars (Berger+, 2020) Authors: Berger, T. A.; Huber, D.; van Saders, J. L.; Gaidos, E.; Tayar, J.; Kraus, A. L. Bibcode: 2020yCat..51590280B Altcode: In this paper, we utilize Gaia DR2 parallaxes, homogeneous stellar g and Ks photometry, and spectroscopic metallicities, where available, to improve on previous analyses and present the most accurate, homogeneous, and precise analysis of stars in the Kepler field. We re-derive stellar Teff, logg, radii, masses, densities, luminosities, and ages for 186301 Kepler targets, and investigate the stellar properties of a number of noteworthy Kepler exoplanet-hosting stars.

(2 data files). Title: Energy resolution and linearity of XENON1T in the MeV energy range Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Angevaare, J.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Cimmino, B.; Clark, M.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; Depoian, A.; Di Gangi, P.; Di Giovanni, A.; Di Stefano, R.; Diglio, S.; Elykov, A.; Eurin, G.; Ferella, A. D.; Fulgione, W.; Gaemers, P.; Gaior, R.; Rosso, A. Gallo; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Hasterok, C.; Hils, C.; Hiraide, K.; Hoetzsch, L.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itow, Y.; Joerg, F.; Kato, N.; Kazama, S.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Fune, E. López; Macolino, C.; Mahlstedt, J.; Manenti, L.; Manfredini, A.; Marignetti, F.; Undagoitia, T. Marrodán; Martens, K.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Miuchi, K.; Molinario, A.; Morâ, K.; Moriyama, S.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Qin, J.; Qiu, H.; García, D. Ramírez; Reichard, S.; Rocchetti, A.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Lavina, L. Scotto; Selvi, M.; Semeria, F.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Takeda, A.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Vargas, M.; Volta, G.; Wack, O.; Wang, H.; Wei, Y.; Weinheimer, C.; Xu, M. Weiss; Wenz, D.; Wittweg, C.; Wulf, J.; Xu, Z.; Yamashita, M.; Ye, J.; Zavattini, G.; Zhang, Y.; Zhu, T.; Zopounidis, J. P. Bibcode: 2020EPJC...80..785A Altcode: 2020arXiv200303825A Xenon dual-phase time projection chambers designed to search for weakly interacting massive particles have so far shown a relative energy resolution which degrades with energy above ∼ 200 keV due to the saturation effects. This has limited their sensitivity in the search for rare events like the neutrinoless double-beta decay of 136Xe at its Q value, Qβ β≃2.46 MeV . For the XENON1T dual-phase time projection chamber, we demonstrate that the relative energy resolution at 1 σ /μ is as low as (0.80 ±0.02 ) % in its one-ton fiducial mass, and for single-site interactions at Qβ β. We also present a new signal correction method to rectify the saturation effects of the signal readout system, resulting in more accurate position reconstruction and indirectly improving the energy resolution. The very good result achieved in XENON1T opens up new windows for the xenon dual-phase dark matter detectors to simultaneously search for other rare events. Title: The Lunar Lander Neutron and Dosimetry (LND) Experiment on Chang'E 4 Authors: Wimmer-Schweingruber, Robert F.; Yu, Jia; Böttcher, Stephan I.; Zhang, Shenyi; Burmeister, Sönke; Lohf, Henning; Guo, Jingnan; Xu, Zigong; Schuster, Björn; Seimetz, Lars; Freiherr von Forstner, Johan L.; Ravanbakhsh, Ali; Knierim, Violetta; Kolbe, Stefan; Woyciechowski, Hauke; Kulkarni, Shrinivasrao R.; Yuan, Bin; Shen, Guohong; Wang, Chunqing; Chang, Zheng; Berger, Thomas; Hellweg, Christine E.; Matthiä, Daniel; Hou, Donghui; Knappmann, Alke; Büschel, Charlotte; Hou, Xufeng; Ren, Baoguo; Fu, Qiang Bibcode: 2020SSRv..216..104W Altcode: 2020arXiv200111028W Chang'E 4 is the first mission to the far side of the Moon and consists of a lander, a rover, and a relay spacecraft. Lander and rover were launched at 18:23 UTC on December 7, 2018 and landed in the von Kármán crater at 02:26 UTC on January 3, 2019. Here we describe the Lunar Lander Neutron & Dosimetry experiment (LND) which is part of the Chang'E 4 Lander scientific payload. Its chief scientific goal is to obtain first active dosimetric measurements on the surface of the Moon. LND also provides observations of fast neutrons which are a result of the interaction of high-energy particle radiation with the lunar regolith and of their thermalized counterpart, thermal neutrons, which are a sensitive indicator of subsurface water content. Title: Long term variations of galactic cosmic radiation on board the International Space Station, on the Moon and on the surface of Mars Authors: Berger, Thomas; Matthiä, Daniel; Burmeister, Sönke; Zeitlin, Cary; Rios, Ryan; Stoffle, Nicholas; Schwadron, Nathan A.; Spence, Harlan E.; Hassler, Donald M.; Ehresmann, Bent; Wimmer-Schweingruber, Robert F. Bibcode: 2020JSWSC..10...34B Altcode: The radiation environment in free space and the related radiation exposure is seen as one of the main health detriments for future long-duration human exploration missions beyond Low Earth Orbit (LEO). The steady flux of energetic particles in the galactic cosmic radiation (GCR) produces a low dose-rate radiation exposure, which is heavily influenced by several factors including the solar cycle, the presence of an atmosphere, relevant magnetic fields (as on Earth) and of course by the relevant spacecraft shielding. Investigations of the GCR variations over the course of a solar cycle provide valuable data for exploration mission planning and for the determination of the radiation load received due to the GCR environment. Within the current work these investigations have been performed applying three datasets generated on board the International Space Station (ISS) with the DOSTEL instruments in the frame of the DOSIS and DOSIS-3D projects, with the CRaTER instrument in a Moon orbit and with the MSL-RAD instrument on the way to and on the surface of Mars. To derive GCR dose contributions on board the ISS two procedures have been developed separating the contributions from GCR from passing's through the South Atlantic Anomaly (SAA), as well as ways to extrapolate the GCR dose measured on board the ISS to free space based on various ranges of the McIlwain L-shell parameter. At the end we provide a dataset spanning the timeframe for GCR measurements on the ISS (2009-2011 & 2012-2019), Moon (2009-2019) and Mars (2012-2019), thereby covering the time span from the deep minimum of solar cycle 23, the ascending phase and maximum of solar cycle 24, and the descending phase of cycle 24, which is ongoing at the time of this writing. Title: Feasibility of Near-Real-Time GOLD Data Products Authors: Codrescu, S. M.; Rowland, W. F.; Plummer, T. M.; Vanier, B. A.; Berger, T. E.; Codrescu, M. V. Bibcode: 2020JGRA..12527819C Altcode: A primary limitation for accurate specification and forecasting of the thermosphere-ionosphere (TI) system is uncertainty in the system forcing. This significantly impacts users who have operational and real-time interests in the current and future state of the TI system. Since Global-Scale Observations of the Limb and Disk (GOLD) observations are expected to provide information about both the current state and forcing of the TI system, GOLD products could be an operational asset if they could be provided in near real time. Production of GOLD data products requires knowledge of the satellite pointing and location. The current scientific processing implementation contains an operationally significant delay to await definitive location and as-flown pointing. We present the results of a demonstration low-latency processing system that assumes the nominal satellite position and pointing to produce low-latency GOLD data products. The resulting products are reasonably similar to the scientific version but are available within minutes rather than hours. Title: Zodiacal exoplanets in time - X. The orbit and atmosphere of the young 'neptune desert'-dwelling planet K2-100b Authors: Gaidos, E.; Hirano, T.; Mann, A. W.; Owens, D. A.; Berger, T. A.; France, K.; Vanderburg, A.; Harakawa, H.; Hodapp, K. W.; Ishizuka, M.; Jacobson, S.; Konishi, M.; Kotani, T.; Kudo, T.; Kurokawa, T.; Kuzuhara, M.; Nishikawa, J.; Omiya, M.; Serizawa, T.; Tamura, M.; Ueda, A. Bibcode: 2020MNRAS.495..650G Altcode: 2020MNRAS.tmp..180G; 2020arXiv200312940G We obtained high-resolution infrared spectroscopy and short-cadence photometry of the 600-800 Myr Praesepe star K2-100 during transits of its 1.67-d planet. This Neptune-size object, discovered by the NASA K2 mission, is an interloper in the 'desert' of planets with similar radii on short-period orbits. Our observations can be used to understand its origin and evolution by constraining the orbital eccentricity by transit fitting, measuring the spin-orbit obliquity by the Rossiter-McLaughlin effect, and detecting any extended, escaping the hydrogen-helium envelope with the 10 830 -Å line of neutral helium in the 2s3S triplet state. Transit photometry with 1-min cadence was obtained by the K2 satellite during Campaign 18 and transit spectra were obtained with the IRD spectrograph on the Subaru telescope. While the elevated activity of K2-100 prevented us from detecting the Rossiter-McLaughlin effect, the new photometry combined with revised stellar parameters allowed us to constrain the eccentricity to e < 0.15/0.28 with 90/99 per cent confidence. We modelled atmospheric escape as an isothermal, spherically symmetric Parker wind, with photochemistry driven by ultraviolet radiation, which we estimate by combining the observed spectrum of the active Sun with calibrations from observations of K2-100 and similar young stars in the nearby Hyades cluster. Our non-detection (<5.7 m Å) of a transit-associated He I line limits mass-loss of a solar-composition atmosphere through a T ≤ 10000 K wind to <0.3 M Gyr-1. Either K2-100b is an exceptional desert-dwelling planet, or its mass-loss is occurring at a lower rate over a longer interval, consistent with a core accretion-powered scenario for escape. Title: A Probabilistic Approach to Kepler Completeness and Reliability for Exoplanet Occurrence Rates Authors: Bryson, S.; Coughlin, J.; Batalha, N. M.; Berger, T.; Huber, D.; Burke, C.; Dotson, J.; Mullally, S. E. Bibcode: 2020AJ....159..279B Altcode: 2019arXiv190603575B Exoplanet catalogs produced by surveys suffer from a lack of completeness (not every planet is detected) and less than perfect reliability (not every planet in the catalog is a true planet), particularly near the survey's detection limit. Exoplanet occurrence rate studies based on such a catalog must be corrected for completeness and reliability. The final Kepler data release, DR25, features a uniformly vetted planet candidate catalog and data products that facilitate corrections. We present a new probabilistic approach to the characterization of Kepler completeness and reliability, making full use of the Kepler DR25 products. We illustrate the impact of completeness and reliability corrections with a Poisson-likelihood occurrence rate method, using a recent stellar properties catalog that incorporates Gaia stellar radii and essentially uniform treatment of the stellar population. Correcting for reliability has a significant impact: the exoplanet occurrence rate for orbital period and radius within 20% of Earth's around GK dwarf stars, corrected for reliability, is ${0.015}_{-0.007}^{+0.011}$ , whereas not correcting results in ${0.034}_{-0.012}^{+0.018}$ —correcting for reliability reduces this occurrence rate by more than a factor of two. We further show that using Gaia-based versus DR25 stellar properties impacts the same occurrence rate by a factor of two. We critically examine the the DR25 catalog and the assumptions behind our occurrence rate method. We propose several ways in which confidence in both the Kepler catalog and occurrence rate calculations can be improved. This work provides an example of how the community can use the DR25 completeness and reliability products. Title: Energetic particles measurements on the lunar far-side by Lunar Lander Neutron and Dosimetry(LND) experiment Authors: Xu, Zigong; Wimmer-Schweingruber, Robert F.; Guo, Jingnan; Yu, Jia; Zhang, Shenyi; Berger, Thomas; Matthiae, Daniel; Burmeister, Soenke; Boettcher, Stephan; Heber, Bernd Bibcode: 2020EGUGA..2221246X Altcode: After Chang'E 4 successfully landed on the far side of the moon on Jan 3rd, 2019, the Lunar Lander Neutron and Dosimetry experiment has been working for 13 lunar days from January, 2019 to January, 2020, sending back the measurements of dose, linear energy transfer (LET) spectrum, neutrons, and charged particles. Here, we show observations of charged particles especially protons and Helium ions during quiet time. We also present two solar energetic particle events registered by LND in May 2019, which are also the first such measurements on the far-side surface of the moon. The temporal variations of particle fluxes on the far side of the moon detected by LND provide a new observation site in space and can be helpful to improve our understanding of particle propagation and transport in the heliosphere. Title: RIMFAX Ground Penetrating Radar Field Tests in the Western USA Authors: Russell, P. S.; Nunes, D.; Hamran, S. -E.; Paige, D. A.; Berger, T.; Amundsen, H. E. F.; Brovoll, S.; Carter, L. M.; Dypvik, H.; Ghent, R.; Kohler, J.; Mellon, M. T.; Plettemeier, D. Bibcode: 2020LPI....51.3012R Altcode: The RIMFAX GPR on Mars2020 was tested for performance and for insight into Mars subsurfaces in several locations, lithologies, and structures in the western US. Title: Leveraging the mathematics of shape for solar magnetic eruption prediction Authors: Deshmukh, Varad; Berger, Thomas E.; Bradley, Elizabeth; Meiss, James D. Bibcode: 2020JSWSC..10...13D Altcode: 2020arXiv200305827D Current operational forecasts of solar eruptions are made by human experts using a combination of qualitative shape-based classification systems and historical data about flaring frequencies. In the past decade, there has been a great deal of interest in crafting machine-learning (ML) flare-prediction methods to extract underlying patterns from a training set - e.g. a set of solar magnetogram images, each characterized by features derived from the magnetic field and labeled as to whether it was an eruption precursor. These patterns, captured by various methods (neural nets, support vector machines, etc.), can then be used to classify new images. A major challenge with any ML method is the featurization of the data: pre-processing the raw images to extract higher-level properties, such as characteristics of the magnetic field, that can streamline the training and use of these methods. It is key to choose features that are informative, from the standpoint of the task at hand. To date, the majority of ML-based solar eruption methods have used physics-based magnetic and electric field features such as the total unsigned magnetic flux, the gradients of the fields, the vertical current density, etc. In this paper, we extend the relevant feature set to include characteristics of the magnetic field that are based purely on the geometry and topology of 2D magnetogram images and show that this improves the prediction accuracy of a neural-net based flare-prediction method. Title: Flying Through Uncertainty Authors: Berger, T. E.; Holzinger, M. J.; Sutton, E. K.; Thayer, J. P. Bibcode: 2020SpWea..1802373B Altcode: Space weather is the main source of uncertainty in the position of all objects in low Earth orbit (LEO) below about 1,000 km. The main impact is strong variation in the neutral density of the thermosphere as it responds to radiative inputs from the Sun in the extreme ultraviolet wavelength range, energetic particle precipitation in the high-latitude auroral zones, and global-scale electrical currents generated during geomagnetic storms. Waves and instabilities from the lower atmosphere can also influence thermospheric density in complex ways. The variation in neutral density leads to variable drag forces on satellites flying through the thermosphere, which in turn causes orbital track changes. We currently lack the ability to accurately model and predict the neutral density changes in the thermosphere in response to space weather inputs. Operational empirical models of thermospheric density are inaccurate during space weather events, and mandate that LEO orbital tracks carry large "error ellipsoids" around all objects to account for positional uncertainty. This leads to many more "conjunction" warnings than necessary as large error ellipsoids are frequently calculated to intersect in orbit. As the LEO domain becomes more crowded with the advent of commercial "megaconstellations" we face a growing challenge to reduce orbital uncertainties by developing whole atmosphere models to enable timely and accurate forecasts of thermospheric conditions. We recommend that researchers, forecasters, and policy makers coordinate to ensure that space weather research and forecasting is tightly integrated into upcoming changes to the operational Space Traffic Management system. Title: Radiation in Space: Relevance and Risk for Human Missions Authors: Hellweg, Christine E.; Berger, Thomas; Matthiä, Daniel; Baumstark-Khan, Christa Bibcode: 2020rsrr.book.....H Altcode: No abstract at ADS Title: University of Colorado Space Weather Technology, Research, and Education Center (SWx TREC): An academic center of excellence to accelerate research to operations and operations to research transitions Authors: Berger, T. E.; Thayer, J. P.; Baker, D. N.; Knipp, D. J.; Pankratz, C. K.; Cranmer, S. R.; Sutton, E. K.; Baltzer, T.; Lucas, G.; Craft, J.; Bosanac, N.; Smith, T. R. Bibcode: 2019AGUFMSA13A..06B Altcode: The University of Colorado at Boulder Space Weather Technology Research and Education Center (SWx TREC) is a University Chancellor's Grand Challenge Initiative forming a campus-wide center for research, mission and technology development, and educational initiatives in the space weather enterprise. SWx TREC offers a unique open academic environment with contributions not only from the departments of Astrophysics and Planetary Sciences, Aerospace Engineering Sciences, and Atmospheric and Oceanic Sciences, but from campus institutes such as the Laboratory for Atmospheric and Space Physics (LASP) and the Cooperative Institute for Research in Environmental Sciences (CIRES) as well. In addition, SWx TREC serves as a "Front Range" space weather collaboration engine, reaching out to local government (NOAA/SWPC, USAF/SpaceCommand) and industry (Ball Aerospace, Lockheed Martin, Raytheon, Google) elements, commercial space weather providers such as Astra LLC and Space Environment Technologies (SET), and local FFRDCs such as the National Solar Observatory (NSO), NCAR's High Altitude Observatory (HAO), the Southwest Research Institute (SWRI), and Northwest Research Associates (NWRA) to pursue opportunities to advance space weather forecasting through innovative research. We discuss how SWx TREC is working with these partners to develop new satellite drag models for Civil Space Traffic Management (STM) applications, a Space Weather Data Portal to ease multi-instrument data display and analysis, and a Space Weather Testbed that will allow academic and commercial developers to test new models and forecasting tools in a cloud-based prototyping facility with student and professional forecaster engagement. SWx TREC is also developing two innovative mission concepts to fill major gaps in the current space weather observing system: the Solar Polar Observing Constellation (SPOC) with Ball Aerospace, and the Operational Radiation Belts (ORB) mission for the Air Force. Title: SWx TREC: An Emerging Community Resource for Integrative Space Weather Data Access and Model/Algorithm R2O Promotion Authors: Pankratz, C. K.; Baltzer, T.; Lucas, G.; Craft, J.; Knuth, J.; Berger, T. E.; Sutton, E. K.; Baker, D. N.; Jaynes, A. N. Bibcode: 2019AGUFMSH33C3373P Altcode: The Space Weather Technology, Research and Education Center (SWx TREC) is an emerging national center of excellence in cross-disciplinary research, technology, innovation, and education, intended to facilitate evolving space weather research and forecasting needs. SWx TREC is positioned to facilitate breakthrough research advances, innovative missions, and data and computing technologies that directly support the needs of the operational forecasting enterprise to ensure closure of the Research to Operations (R2O) and Operations to Research (O2R) loop. Improving our understanding and prediction of space weather requires coupled Research and Operations. SWx-TREC is working to provide new research models, applications and data for use in operational environments, improving the Research-to-Operations (R2O) pipeline. Advancement in the fundamental scientific understanding of space weather processes is also vital, requiring that researchers have convenient and effective access to a wide variety of data sets and models from multiple sources. The space weather research community, as with many scientific communities, must access data from dispersed and often uncoordinated data repositories to acquire the data necessary for the analysis and modeling efforts that advance our understanding of solar influences and space physics in the Earth's environment. The University of Colorado (CU) is a leading institution in both producing data products and advancing the state of scientific understanding of space weather processes, and is serving many of these needs, including 1) implementation of an interoperable data portal intended to more effectively serve the needs of the Space Weather research community and 2) implementing a community-accessible testbed environment to support development, testing, transition, and use of new models and algorithms. In this presentation, we will outline the motivating factors for effective space weather data access and modeling support, describe a new testbed environment for supporting model, algorithm, and visualization testing/incubation needs, and demonstrate a new Space Weather Data Portal, designed to meet the data management and access needs of the disparate communities who require space weather data and information. Title: Adding Lunar Observations to Multi-point Observations around Earth to Determine the Structure Heliospheric Discontinuities Authors: Wimmer-Schweingruber, R. F.; Yu, J.; Xu, Z.; Zhang, S.; Hou, D.; Guo, J.; Freiherr von Forstner, J. L.; Lohf, H.; Boettcher, S. I.; Burmeister, S.; Matthiae, D.; Berger, T.; Hellweg, C. Bibcode: 2019AGUFMSH41A..01W Altcode: The Chinese Chang'E 4 spacecraft landed on the Moon on January 3, 2019. The Lunar Lander Neutrons and Dosimetry (LND) instrument aboard the Chang'E 4 lander provides measurements of the radiation environment on the Moon. Some of its data products are provided at a cadence of once per minute. Combining such data with high time resolution data from other spacecraft near Earth (i.e., ACE, DSCOVR, SOHO, and Wind at L1) allows to determine the three-dimensional structure of discontinuities in the solar wind when (instrumental) counting statistics are good enough.

We will present first attempts at reconstructing the inclination angles of large-scale heliospheric discontinuities using data from ACE, Chang'E 4, DSCOVR, SOHO, and Wind. We assume a radially flowing solar wind speed of constant speed in individual solar wind streams and investigate the timing of discontinuities in count rates of particle and solar-wind instruments on these spacecraft. Title: Energetic particles measurements on the lunar far side by Lunar Lander Neutron and Dosimetry(LND) experiment Authors: Xu, Z.; Wimmer-Schweingruber, R. F.; Guo, J.; Yu, J.; Zhang, S.; Berger, T.; Matthiae, D.; Burmeister, S.; Boettcher, S. I.; Heber, B. Bibcode: 2019AGUFMSH41D3340X Altcode: After Chang'E 4 successfully landed on the far side of the moon on Jan 3rd, 2019, the Lunar Lander Neutron and Dosimetry experiment has been working for 7 lunar days from January to July, sending back the measurements of dose, linear energy transfer (LET) spectrum, neutrons and charged particles. Here, we show observations of charged particles especially protons and Helium ions, including long term variation and solar energetic events, which are also the first such measurements on the surface of the moon. The long-term variation is mainly caused by solar modulation of galactic cosmic rays (GCR) and anomalous cosmic rays (ACR). Comparing the energy spectra of protons and He4 with those detected by EPHIN in 2019 and during the previous solar minimum in 1996, as well as the Crème and BO10 models, we find that the protons detected by LND were from GCR and solar source, while the He4 were mainly from the ACR. This is a consequence of LND's energy coverage. We also derive the upward proton fluxes due to the interaction of downward energetic particles with lunar regolith. We will also present a solar energetic particle event registered by LND in May, 2019. The temporal variations of particle fluxes on the far side of the moon detected by LND provide a new observation site in space and can be helpful to improve our understanding of particle propagation and transport in the heliosphere. Title: The Solar Polar Observing Constellation (SPOC) Mission: research and operational monitoring of space weather from polar heliocentric orbits Authors: Berger, T. E.; Bosanac, N.; Smith, T. R.; Duncan, N. A.; Wu, G.; Turner, E.; Hurlburt, N.; Korendyke, C. Bibcode: 2019AGUFMSH43F3352B Altcode: The Sun's polar regions remain largely unobserved and yet understanding and monitoring of the magnetic field, convective flows, and coronal outflow conditions in the solar polar regions are the keys to accurately modeling and forecasting the solar cycle, solar wind conditions, and CME arrival times at Earth. We describe the Solar Polar Observing Constellation (SPOC), a mission to establish continuous high-resolution imaging of solar magnetic field dynamics, high-latitude surface and sub-surface convective flows, and coronal mass ejection tracking from a low-eccentricity polar heliocentric orbit. SPOC will consist of two identical spacecraft, each equipped with a Lockheed Martin Compact Magnetic Imager (CMI, derived from the Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager), the Naval Research Laboratory (NRL) Compact Coronagraph (CCOR), and in-situ solar wind and energetic particle instruments. Falcon Heavy launch vehicles will place the SPOC spacecraft into a Jupiter gravitational assist (JGA) heliocentric orbit, achieving an 88-degree ecliptic inclination, with the spacecraft passing over the solar poles within 4 years after launch. Ion engines will subsequently reduce the eccentricity of the orbits to below 0.05 at approximately 0.9 AU within 6 years after launch. Orbital phasing will place the spacecraft over alternate poles to enable continuous monitoring of the polar regions with operational-level redundancy of systems. The inclusion of CCOR will enable visualization and tracking of coronal mass ejections from above (or below) the ecliptic for the first time, greatly enhancing our ability to forecast CME arrival times at Earth and other planets such as Mars. SPOC combines polar region exploration, high-latitude helioseismology and magnetic imaging, and operational space weather monitoring in a single mission. Along with planned missions to the L1 and L5 Lagrangian points in the ecliptic, SPOC will enable an approach to the long-sought goal of continuous full-sphere measurements of the solar magnetic field, solar wind and CME outflow, and energetic particle flux - a goal that cannot be achieved with observations from the ecliptic plane alone. Title: Search for Light Dark Matter Interactions Enhanced by the Migdal Effect or Bremsstrahlung in XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Depoian, A.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gaemers, P.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Greene, Z.; Hasterok, C.; Hils, C.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itay, R.; Joerg, F.; Kazama, S.; Kish, A.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Manenti, M.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Masbou, J.; Mastroianni, S.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Qin, J.; Qiu, H.; Ramírez García, D.; Reichard, S.; Riedel, B.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Volta, G.; Wack, O.; Wang, H.; Wei, Y.; Weinheimer, C.; Wenz, D.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Xenon Collaboration Bibcode: 2019PhRvL.123x1803A Altcode: 2019arXiv190712771A Direct dark matter detection experiments based on a liquid xenon target are leading the search for dark matter particles with masses above ∼5 GeV /c2, but have limited sensitivity to lighter masses because of the small momentum transfer in dark matter-nucleus elastic scattering. However, there is an irreducible contribution from inelastic processes accompanying the elastic scattering, which leads to the excitation and ionization of the recoiling atom (the Migdal effect) or the emission of a bremsstrahlung photon. In this Letter, we report on a probe of low-mass dark matter with masses down to about 85 MeV /c2 by looking for electronic recoils induced by the Migdal effect and bremsstrahlung using data from the XENON1T experiment. Besides the approach of detecting both scintillation and ionization signals, we exploit an approach that uses ionization signals only, which allows for a lower detection threshold. This analysis significantly enhances the sensitivity of XENON1T to light dark matter previously beyond its reach. Title: The University of Colorado Space Weather Technology, Research, and Education Center's Space Weather Portal: A Tool for Easing Access to and Understanding of Datasets to Characterize Space Weather Events Authors: Baltzer, T.; Berger, T. E.; Knuth, J.; Lindholm, D. M.; Wilson, A.; Pankratz, C. K. Bibcode: 2019AGUFMSH33C3371B Altcode: In our work with researchers, we consistently hear that a significant hurdle they encounter is obtaining datasets from disparate providers in varying formats, needing to repeat processes to obtain new timeframes for those datasets and that having an idea of what is available (e.g. is there an instrument outage during the time of interest?) before downloading it is often unavailable. This is particularly challenging for space weather researchers attempting to characterize an event from the moment of occurrence on the Sun to the impacts it has on the Earth.

As part of the University of Colorado's Space Weather Technology, Research and Education Center (SWx-TREC https://www.colorado.edu/spaceweather/), the Laboratory for Atmospheric and Space Physics (LASP) is developing a Space Weather Portal (http://lasp.colorado.edu/space-weather-portal) to provide unified access to disparate datasets to help close the Research to Operations (R2O) and Operations to Research (O2R) gap. This presentation will describe how this portal can be used to characterize an historical event (2015 St. Patrick's day storm) from available datasets, visualize them and download them for further use. It will also describe the underlying middleware (LaTiS) that enables the portal. Title: Light Dark Matter Search with Ionization Signals in XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Antochi, V. C.; Angelino, E.; Arneodo, F.; Barge, D.; Baudis, L.; Bauermeister, B.; Bellagamba, L.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Depoian, A.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gaemers, P.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Greene, Z.; Hasterok, C.; Hils, C.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itay, R.; Joerg, F.; Kazama, S.; Kish, A.; Kobayashi, M.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Masbou, J.; Mastroianni, S.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Palacio, J.; Pelssers, B.; Peres, R.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Qin, J.; Qiu, H.; Ramírez García, D.; Reichard, S.; Riedel, B.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Volta, G.; Wack, O.; Wang, H.; Wei, Y.; Weinheimer, C.; Wenz, D.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Xenon Collaboration Bibcode: 2019PhRvL.123y1801A Altcode: 2019arXiv190711485A We report constraints on light dark matter (DM) models using ionization signals in the XENON1T experiment. We mitigate backgrounds with strong event selections, rather than requiring a scintillation signal, leaving an effective exposure of (22 ±3 ) tonne day. Above ∼0.4 keVe e , we observe <1 event/(tonne day keVe e) , which is more than 1000 times lower than in similar searches with other detectors. Despite observing a higher rate at lower energies, no DM or CEvNS detection may be claimed because we cannot model all of our backgrounds. We thus exclude new regions in the parameter spaces for DM-nucleus scattering for DM masses mχ within 3 - 6 GeV /c2 , DM-electron scattering for mχ>30 MeV /c2 , and absorption of dark photons and axionlike particles for mχ within 0.186 - 1 keV /c2 . Title: Cooling Condensation at Coronal Null Points and Quasi-Separatrix Layers Involving Magnetic Reconnection Authors: Liu, W.; Sun, X.; Yu, S.; Luna Bennasar, M.; Antolin, P.; Titov, V. S.; Downs, C.; Berger, T. E. Bibcode: 2019AGUFMSH11C3394L Altcode: The solar corona, Sun's outer atmosphere, is million-degrees hot and tenuous. This hot plasma, under certain conditions, can enigmatically undergo a radiative cooling instability and condense into material of 100 times cooler in the form of prominences or coronal rain. Where, when, and how such cooling condensation takes place remain poorly understood. Answers to these questions are not only of scientific importance in their own right, but also bear implications for the fundamental question of coronal heating and the chromosphere-corona mass cycle. Magnetic fields in the magnetized corona undoubtedly play a crucial role (e.g., by trapping the plasma), but where and how? We report recent imaging and spectroscopic observations from SDO/AIA/HMI and IRIS that can shed light on these puzzles. Through a systematic survey, we found that a large fraction of quiet-Sun condensations preferentially occur at the dips of coronal loops or funnels. Such dips are located at/near magnetic topological features, such as null points and quasi-separatrix layers (QSLs), which are regions characterized by high values of the squashing factor. We also identified evidence of magnetic reconnection at such locations, which can produce favorable conditions, e.g., density enhancement by compression and/or mass trapping in plasmoids, that can trigger run-away radiative cooling. We present proof-of-concept MHD simulations that demonstrate the role of reconnection in transporting cooled mass from overlying, long loops to underlying, short loops where it slide down as coronal rain. We will discuss the significance and broader implications of these results beyond solar physics. Title: SWx TREC Testbed: Facilitating Model/Algorithm R2O and O2R Development within a Cloud Computing Environment Authors: Lucas, G.; Craft, J.; Pankratz, C. K.; Sutton, E. K.; Berger, T. E. Bibcode: 2019AGUFMSH33C3372L Altcode: The Space Weather Technology, Research and Education Center (SWx TREC) is an emerging national center of excellence in cross-disciplinary research, technology, innovation, and education, intended to facilitate evolving space weather research and forecasting needs. Within this center, we are developing a Space Weather Testbed environment to facilitate the research to operations (R2O) and operations to research (O2R) pipelines. The Testbed leverages cloud computing to provide a managed computational environment for independent science teams to deploy their processing software into an operational-like system. Using cloud computing for the environment enables traditional defined-cadence (daily, hourly) model runs to be scheduled while also providing the ability to submit on-demand runs during storm times with no additional bulk hardware purchases that would otherwise sit idle most of the time.

In this poster, we will discuss the technologies that are being used in producing the Space Weather Testbed and demonstrate two ways that the testbed is currently being utilized. First, in the R2O pipeline, we have implemented code from the USGS to produce electric field maps at a set cadence to demonstrate that the code can be run in an operational mode. Second, in the O2R pipeline, we are taking an operational code, the NOAA Whole Atmosphere Model (WAM), and enabling researchers to investigate new data assimilation techniques that can supplement and enhance current operational code capabilities. The Space Weather TREC Testbed is utilizing modern computer architectures and software practices to facilitate researchers and forecasters bridge the R2O and O2R gaps. Title: VizieR Online Data Catalog: Revised radii of KIC stars & planets using Gaia DR2 (Berger+, 2018) Authors: Berger, T. A.; Huber, D.; Gaidos, E.; van Saders, J. L. Bibcode: 2019yCat..18660099B Altcode: First, we crossmatched the positions of all stars from the Kepler Stellar Properties Catalog (KSPC DR25; Mathur+ 2017, J/ApJS/229/30) with the Gaia Data Release 2 (DR2, I/345) by utilizing the X-match service of the Centre de Donnees astronomiques de Strasbourg (CDS). This provided a table of Gaia DR2 source matches within 3" of each Keplers tar. Excluding stars through a variety of cuts reduced our final sample to 177911 Kepler stars. See section 2.1 for further details.

(2 data files). Title: Planetesimals around stars with TESS (PAST) - I. Transient dimming of a binary solar analogue at the end of the planet accretion era Authors: Gaidos, E.; Jacobs, T.; LaCourse, D.; Vanderburg, A.; Rappaport, S.; Berger, T.; Pearce, L.; Mann, A. W.; Weiss, L.; Fulton, B.; Behmard, A.; Howard, A. W.; Ansdell, M.; Ricker, G. R.; Vanderspek, R. K.; Latham, D. W.; Seager, S.; Winn, J. N.; Jenkins, J. M. Bibcode: 2019MNRAS.488.4465G Altcode: 2019arXiv190702476G; 2019MNRAS.tmp.1875G We report detection of quasi-periodic (1.5-d) dimming of HD 240779, the solar-mass primary in a 5 arcsec visual binary (also TIC 284730577), by the Transiting Exoplanet Survey Satellite. This dimming, as has been shown for other `dipper' stars, is likely due to occultation by circumstellar dust. The barycentric space motion, lithium abundance, rotation, and chromospheric emission of the stars in this system point to an age of ≈125 Myr, and possible membership in the AB Doradus moving group. As such it occupies an important but poorly explored intermediate regime of stars with transient dimming between young stellar objects in star-forming regions and main-sequence stars, and between UX Orionis-type Ae/Be stars and M-type `dippers'. HD 240779, but not its companion BD+10 714B, has Wide-field Infrared Survey Explorer (WISE)-detected excess infrared emission at 12 and 22 μm indicative of circumstellar dust. We propose that infrared emission is produced by collisions of planetesimals during clearing of a residual disc at the end of rocky planet formation, and that quasi-periodic dimming is produced by the rapid disintegration of a ≳100 km planetesimal near the silicate evaporation radius. Further studies of this and similar systems will illuminate a poorly understood final phase of rocky planet formation like that which produced the inner Solar system. Title: Phobos LIFE (Living Interplanetary Flight Experiment) Authors: Betts, Bruce H.; Warmflash, David; Fraze, Raymond E.; Friedman, Louis; Vorobyova, Elena; Lilburn, Timothy G.; Smith, Amy; Rettberg, Petra; Jönsson, K. Ingemar; Ciftcioglu, Neva; Fox, George E.; Svitek, Tomas; Kirschvinck, Joseph L.; Moeller, Ralf; Wassmann, Marko; Berger, Thomas Bibcode: 2019AsBio..19.1177B Altcode: The Planetary Society's Phobos Living Interplanetary Flight Experiment (Phobos LIFE) flew in the sample return capsule of the Russian Federal Space Agency's Phobos Grunt mission and was to have been a test of one aspect of the hypothesis that life can move between nearby planets within ejected rocks. Although the Phobos Grunt mission failed, we present here the scientific and engineering design and motivation of the Phobos LIFE experiment to assist with the scientific and engineering design of similar future experiments. Phobos LIFE flew selected organisms in a simulated meteoroid. The 34-month voyage would have been the first such test to occur in the high-radiation environment outside the protection of Earth's magnetosphere for more than a few days. The patented Phobos LIFE "biomodule" is an 88 g cylinder consisting of a titanium outer shell, several types of redundant seals, and 31 individual Delrin sample containers. Phobos LIFE contained 10 different organisms, representing all three domains of life, and one soil sample. The organisms are all very well characterized, most with sequenced genomes. Most are extremophiles, and most have flown in low Earth orbit. Upon return from space, the health and characteristics of organisms were to have been compared with controls that remained on Earth and have not yet been opened. Title: First Results from the Lunar Lander Neutron and Dosimetry Experiment (LND) on China's Chang'E 4 mission to the far side of the Moon Authors: Wimmer-Schweingruber, Robert F.; Zhang, Shenyi; Yu, Jia; Böttcher, Stephan I.; Burmeister, Sönke; Lohf, Henning; Guo, Jingnan; Xu, Zigong; Berger, Thomas; Hellweg, Christine; Matthiä, Daniel Bibcode: 2019EPSC...13.1289W Altcode: Chang'E 4 is the Chinese mission which landed on the far side of the Moon at 02:26 UTC on January 3, 2019. It consists of a lander, a rover, and an re- lay spacecraft. We will present first results from the Lunar Lander Neutron and Dosimetry (LND) Experi- ment aboard Chang'E 4. LND has obtained first active dosimetric measurements on the surface of the Moon, both of the charged as well as neutral radiation com- ponent. Title: Measurements of radiation quality factor on Mars with the Mars Science Laboratory Radiation Assessment Detector Authors: Zeitlin, C.; Hassler, D. M.; Ehresmann, B.; Rafkin, S. C. R.; Guo, J.; Wimmer-Schweingruber, R. F.; Berger, T.; Matthiä, D. Bibcode: 2019LSSR...22...89Z Altcode: We report the first long-term measurements of the radiation quality factor of energetic charged particles on the surface of Mars. The Radiation Assessment Detector (RAD) aboard the Mars Science Laboratory rover, also known as Curiosity, has been operating on Mars since 2012. RAD contains thin silicon detectors that record the ionization energy loss of energetic charged particles. The particles are dominantly galactic cosmic rays (GCRs) and the products of their interactions in the Martian atmosphere, with occasional contributions from solar energetic particles (SEPs). The quality factor on the surface of Mars is influenced by two factors: variations in the shielding provided by the atmosphere, and changes in the spectrum of the incident energetic particle flux due to the 11-year solar cycle. The two cannot be easily disentangled using the data alone, but insights can be gained from calculations and Monte Carlo simulations. Title: Photochemistry on the Space Station—Antibody Resistance to Space Conditions after Exposure Outside the International Space Station Authors: Coussot, Gaëlle; Le Postollec, Aurélie; Faye, Clément; Baqué, Mickaël; Vandenabeele-Trambouze, Odile; Incerti, Sébastien; Vigier, Flavie; Chaput, Didier; Cottin, Hervé; Przybyla, Bartos; Berger, Thomas; Dobrijevic, Michel Bibcode: 2019AsBio..19.1053C Altcode: Antibody-based analytical instruments are under development to detect signatures of life on planetary bodies. Antibodies are molecular recognition reagents able to detect their target at sub-nanomolar concentrations, with high affinity and specificity. Studying antibody binding performances under space conditions is mandatory to convince space agencies of the adequacy of this promising tool for planetary exploration. To complement previous ground-based experiments on antibody resistance to simulated irradiation, we evaluate in this paper the effects of antibody exposure to real space conditions during the EXPOSE-R2 mission outside the International Space Station. The absorbed dose of ionizing radiation recorded during the 588 days of this mission (220 mGy) corresponded to the absorbed dose expected during a mission to Mars. Moreover, samples faced, at the same time as irradiation, thermal cycles, launch constraints, and long-term storage. A model biochip was used in this study with antibodies in freeze-dried form and under two formats: free or covalently grafted to a solid surface. We found that antibody-binding performances were not significantly affected by cosmic radiation, and more than 40% of the exposed antibody, independent of its format, was still functional during all this experiment. We conclude that antibody-based instruments are well suited for in situ analysis on planetary bodies. Title: Photochemistry on the Space Station—Aptamer Resistance to Space Conditions: Particles Exposure from Irradiation Facilities and Real Exposure Outside the International Space Station Authors: Coussot, Gaëlle; Le Postollec, Aurélie; Incerti, Sébastien; Baqué, Mickaël; Faye, Clément; Vandenabeele-Trambouze, Odile; Cottin, Hervé; Ravelet, Corinne; Peyrin, Eric; Fiore, Emmanuelle; Vigier, Flavie; Caron, Jérôme; Chaput, Didier; Przybyla, Bartos; Berger, Thomas; Dobrijevic, Michel Bibcode: 2019AsBio..19.1063C Altcode: Some microarray-based instruments that use bioaffinity receptors such as antibodies or aptamers are under development to detect signatures of past or present life on planetary bodies. Studying the resistance of such instruments against space constraints and cosmic rays in particular is a prerequisite. We used several ground-based facilities to study the resistance of aptamers to various types of particles (protons, electrons, neutrons, and carbon ions) at different energies and fluences. We also tested the resistance of aptamers during the EXPOSE-R2 mission outside the International Space Station (ISS). The accumulated dose measured after the 588 days of this mission (220 mGy) corresponds to the accumulated dose that can be expected during a mission to Mars. We found that the recognition ability of fluorescently labeled aptamers was not significantly affected during short-term exposure experiments taking into account only one type of radiation at a time. However, we demonstrated that the same fluorescent dye was significantly affected by temperature variations (-21°C to +58°C) and storage throughout the entirety of the ISS experiment (60% of signal loss). This induced a large variability of aptamer signal in our analysis. However, we found that >50% of aptamers were still functional after the whole EXPOSE-R2 mission. We conclude that aptamer-based instruments are well suited for in situ analysis on planetary bodies, but the detection step requires additional investigations. Title: VizieR Online Data Catalog: Radial velocities and transit times for KOI 4 (Chontos+, 2019) Authors: Chontos, A.; Huber, D.; Latham, D. W.; Bieryla, A.; van Eylen, V.; Bedding, T. R.; Berger, T.; Buchhave, L. A.; Campante, T. L.; Chaplin, W. J.; Colman, I. L.; Coughlin, J. L.; Davies, G.; Hirano, T.; Howard, A. W.; Isaacson, H. Bibcode: 2019yCat..51570192C Altcode: Following the asteroseismic reclassification of the host star, we initiated an intensive radial velocity (RV) follow-up program using the Tillinghast Reflector Echelle Spectrograph (TRES), a fiber-fed echelle spectrograph spanning the spectral range of 3900-9100 Å with a resolving power of R~44000. We obtained 23 spectra with TRES between UT 2009 November 8 and 2017 September 13 using the medium 2.3" fiber. The spectra were reduced and extracted as outlined in Buchhave et al. (2010, J/ApJ/720/1118). The average exposure time of ~1800 s, corresponding to a mean signal-to-noise ratio (S/N) per resolution element of ~53 at the peak of the continuum near the Mg b triplet at 519 nm. We used the strongest S/N spectrum as a template to derive relative RVs by cross-correlating the remaining spectra order-by-order against the template, which is given a relative velocity of 0 km/s, by definition.

(2 data files). Title: Coronal Condensation at Preferential Topological Locations: The Birth of Solar Prominences and Coronal Rain Authors: Liu, Wei; Sun, Xudong; Yu, Sijie; Antolin, Patrick; Titov, Viacheslav; Downs, Cooper; Berger, Thomas Bibcode: 2019AAS...23412502L Altcode: The million-degree hot and tenuous solar coronal plasma, under certain conditions, can enigmatically undergo a radiative cooling instability and condense into material of 100 times cooler in the form of prominences or coronal rain. Where, when, and how such cooling condensation takes place remain poorly understood. Answers to these questions are not only of scientific importance in their own right, but also bear implications for the fundamental question of coronal heating and the chromosphere-corona mass cycle. Magnetic fields in the magnetized corona undoubtedly play a crucial role (e.g., by trapping the plasma), but where and how? We report recent imaging and spectroscopic observations from SDO/AIA/HMI and IRIS that can shed light on these puzzles. Through a systematic survey, we found that a large fraction of quiet-Sun condensations preferentially occur at the dips of coronal loops or funnels. Such dips are located at/near magnetic topological features, such as null points and quasi-separatrix layers (QSLs), which are regions characterized by high values of the squashing factor. We also identified evidence of magnetic reconnection at such locations, which can produce favorable conditions, e.g., density enhancement by compression and/or mass trapping in plasmoids, that can trigger run-away radiative cooling. We will discuss the significance and broader implications of these novel observations. Title: Solar Polar Observing Constellation (SPOC): A New Age for Solar Observations Authors: Upton, Lisa; Berger, Thomas; Duncan, Nicole; Bosanac, Natasha Bibcode: 2019AAS...23410614U Altcode: Current observing platforms can only measure the solar magnetic field over a portion of the Earth-facing hemisphere, forcing us to rely on solar rotation to build up fictional "synoptic maps" of the full-Sun field over 27-days. The lack of magnetic field "boundary conditions" over the full Sun represents a fundamental gap in our ability to accurately model the solar coronal magnetic field and solar wind acceleration. Views restricted to the ecliptic plane cannot capture the Sun's polar regions. Observation of the poles from a high latitude vantage point are needed to advance helioseismology and constrain the Sun's polar fields and high latitude flows, which are crucial to understanding the solar activity cycle. Furthermore, sustained observation of the Sun's polar regions will enable helioseismology investigations of the polar subsurface flows, allowing us to probe deeper into the mechanisms of the solar cycle.

We propose a novel constellation of small satellites called the Solar Polar Observing Constellation (SPOC) that will obtain magnetic field and doppler velocity measurements from a solar polar orbit, including nearly direct overhead measurements of the poles. The SPOC constellation consists of two identical satellites placed into 90-degree inclination heliocentric orbits using Jupiter gravitational assist (JGA) trajectories and ion electric propulsion to circularize the orbit at about 0.9 AU. Instrumentation includes a compact helioseismic magnetic imager, compact coronagraph, and in-situ solar wind plasma measuring instruments. The SPOC mission follows the model of "hybrid operational-research" missions developed by the CU Space Weather Technology, Research, and Education (SWx-TREC) to enhance utility and collaboration by developing critical operational data sources for space weather forecasting that can also produce exploratory science data. Title: Deep Learning and Feature Engineering for Solar Flare Prediction Authors: Carande, Wendy Hawley; Berger, Tom; Cai, Justin; Craft, James; Hartnett, Maxine; Jones, Andrew; Newman, William; Pankratz, Chris; Woods, Tom Bibcode: 2019shin.confE.156C Altcode: Space weather events can inflict chaos on our modern, technologically-dependent world, such as degradation, and sometimes even disruption, for our telecommunications, power grids, navigation systems, and satellite operations. Therefore, improving the accuracy in predicting such events is of the upmost importance. With this in mind, we built a deep learning system capable of predicting M and X class solar flares in a 24 hour time window, and we achieved a True Skill Score of 0.9. The inputs to our deep learning algorithm are magnetograms from the Solar Dynamics Observatory Helioseismic and Magnetic Imager (SDO/HMI), and the output is a binary classification indicating whether or not a solar flare will occur in the time window. The highest True Skill Scores were attained with the convolutional neural networks AlexNet and VGGNet. We are currently working to incorporate SDO Extreme ultraviolet Variability (EVE) time series data into our existing deep learning framework. As we add more data, we anticipate a richer model with increased predictive power. Using examples and results from our convolutional neural network and multilayer perceptron models, we’ll present how we approached challenges and sought to fix them and what methods we propose as we further develop our models. We’ll also present the importance of feature engineering as it relates to solar flare prediction, and the obstacles and rewards of creating our own in-house features, including polarity inversion lines. Title: Calibrating GONG Magnetograms Using MURaM as Ground Truth Authors: Plowman, Joseph; Petrie, Gordon; Berger, Tom Bibcode: 2019shin.confE.223P Altcode: Results of a GONG calibration based on an end-to-end simulation of its measurement process are presented. The calibration begins with a MuRAM 3D MHD simulation, models solar radiative transfer of the GONG nickel line, emulates the GONG measurement process, and inverts the resulting synthetic GONG observations to produce magnetograms. The theory of producing calibration curves from comparison of synthetic magnetograms with the corresponding ground truth is then considered, and the resulting calibration curves are shown. The implications of these results for space weather applications are discussed, and they also shed new light on the old question of the relative calibration of magnetographs. Title: SWx TREC: An Open Space Weather (SWx) R2O Development and Testbed Environment Authors: Craft, James; Pankratz, Chris; Berger, Thomas; Thayer, Jeffrey; Baltzer, Thomas; Baker, Daniel Bibcode: 2019EGUGA..2112073C Altcode: The Chancellor of the University of Colorado recently awarded a Grand Challenge grant to a group of departments and labs for the development of the Space Weather Technology, Research and Education Center (https://www.colorado.edu/spaceweather/). As part of this effort, the Laboratory for Atmospheric and Space Physics (LASP) is developing a Space Weather Testbed to provide a platform to explore research and development models side-by-side with operational standards. The Space Weather Testbed is being built using technologies employed by LASP Data Systems for the Magnetospheric Multiscale Mission Science Data Center and the Emirates Mars Mission Science Data Center. These data centers provide a managed computational environment for independent science teams to deploy their processing software into the operational system. This poster will discuss the technologies that will be used in producing the Space Weather Testbed and how the exploration between Operations to Research (O2R) and Research to Operations (R2O) will be supported. Title: Constraining the Spin-Dependent WIMP-Nucleon Cross Sections with XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Anthony, M.; Antochi, V. C.; Arneodo, F.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Greene, Z.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itay, R.; Joerg, F.; Kazama, S.; Kish, A.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Mosbacher, Y.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Pelssers, B.; Piastra, F.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Priel, N.; Qiu, H.; Ramírez García, D.; Reichard, S.; Riedel, B.; Rizzo, A.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Wack, O.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wenz, D.; Wittweg, C.; Wulf, J.; Xu, Z.; Ye, J.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Xenon Collaboration Bibcode: 2019PhRvL.122n1301A Altcode: 2019arXiv190203234A We report the first experimental results on spin-dependent elastic weakly interacting massive particle (WIMP) nucleon scattering from the XENON1T dark matter search experiment. The analysis uses the full ton year exposure of XENON1T to constrain the spin-dependent proton-only and neutron-only cases. No significant signal excess is observed, and a profile likelihood ratio analysis is used to set exclusion limits on the WIMP-nucleon interactions. This includes the most stringent constraint to date on the WIMP-neutron cross section, with a minimum of 6.3 ×10-42 cm2 at 30 GeV /c2 and 90% confidence level. The results are compared with those from collider searches and used to exclude new parameter space in an isoscalar theory with an axial-vector mediator. Title: The Lunar Lander Neutron and Dosimetry (LND) Experiment on Chang'E4 Authors: Wimmer-Schweingruber, R. F.; Zhang, S.; Yu, J.; Hellweg, C. E.; Guo, J.; Lohf, H.; Berger, T.; Böttcher, S. I.; Burmeister, S.; Knappmann, A.; Knierim, V.; Schuster, B.; Seimetz, L.; Xu, Z.; Shen, G.; Yuan, B. Bibcode: 2019LPI....50.2348W Altcode: Chang'E4 was launched on December 8, 2018 and landed on January 3, 2019. We present first data from the Lunar Lander Neutron and Dosimetry (LND) Experiment. Title: Limits of Life and the Habitability of Mars: The ESA Space Experiment BIOMEX on the ISS Authors: de Vera, Jean-Pierre; Alawi, Mashal; Backhaus, Theresa; Baqué, Mickael; Billi, Daniela; Böttger, Ute; Berger, Thomas; Bohmeier, Maria; Cockell, Charles; Demets, René; de la Torre Noetzel, Rosa; Edwards, Howell; Elsaesser, Andreas; Fagliarone, Claudia; Fiedler, Annelie; Foing, Bernard; Foucher, Frédéric; Fritz, Jörg; Hanke, Franziska; Herzog, Thomas; Horneck, Gerda; Hübers, Heinz-Wilhelm; Huwe, Björn; Joshi, Jasmin; Kozyrovska, Natalia; Kruchten, Martha; Lasch, Peter; Lee, Natuschka; Leuko, Stefan; Leya, Thomas; Lorek, Andreas; Martínez-Frías, Jesús; Meessen, Joachim; Moritz, Sophie; Moeller, Ralf; Olsson-Francis, Karen; Onofri, Silvano; Ott, Sieglinde; Pacelli, Claudia; Podolich, Olga; Rabbow, Elke; Reitz, Günther; Rettberg, Petra; Reva, Oleg; Rothschild, Lynn; Garcia Sancho, Leo; Schulze-Makuch, Dirk; Selbmann, Laura; Serrano, Paloma; Szewzyk, Ulrich; Verseux, Cyprien; Wadsworth, Jennifer; Wagner, Dirk; Westall, Frances; Wolter, David; Zucconi, Laura Bibcode: 2019AsBio..19..145D Altcode: BIOMEX (BIOlogy and Mars EXperiment) is an ESA/Roscosmos space exposure experiment housed within the exposure facility EXPOSE-R2 outside the Zvezda module on the International Space Station (ISS). The design of the multiuser facility supports—among others—the BIOMEX investigations into the stability and level of degradation of space-exposed biosignatures such as pigments, secondary metabolites, and cell surfaces in contact with a terrestrial and Mars analog mineral environment. In parallel, analysis on the viability of the investigated organisms has provided relevant data for evaluation of the habitability of Mars, for the limits of life, and for the likelihood of an interplanetary transfer of life (theory of lithopanspermia). In this project, lichens, archaea, bacteria, cyanobacteria, snow/permafrost algae, meristematic black fungi, and bryophytes from alpine and polar habitats were embedded, grown, and cultured on a mixture of martian and lunar regolith analogs or other terrestrial minerals. The organisms and regolith analogs and terrestrial mineral mixtures were then exposed to space and to simulated Mars-like conditions by way of the EXPOSE-R2 facility. In this special issue, we present the first set of data obtained in reference to our investigation into the habitability of Mars and limits of life. This project was initiated and implemented by the BIOMEX group, an international and interdisciplinary consortium of 30 institutes in 12 countries on 3 continents. Preflight tests for sample selection, results from ground-based simulation experiments, and the space experiments themselves are presented and include a complete overview of the scientific processes required for this space experiment and postflight analysis. The presented BIOMEX concept could be scaled up to future exposure experiments on the Moon and will serve as a pretest in low Earth orbit. Title: First Results on the Scalar WIMP-Pion Coupling, Using the XENON1T Experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Anthony, M.; Antochi, V. C.; Arneodo, F.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Grandi, L.; Greene, Z.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Iacovacci, M.; Itay, R.; Joerg, F.; Kaminsky, B.; Kazama, S.; Kish, A.; Koltman, G.; Kopec, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; López Fune, E.; Macolino, C.; Mahlstedt, J.; Manfredini, A.; Marignetti, F.; Marrodán Undagoitia, T.; Masbou, J.; Masson, D.; Mastroianni, S.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Odgers, K.; Pelssers, B.; Piastra, F.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Priel, N.; Qiu, H.; Ramírez García, D.; Reichard, S.; Riedel, B.; Rizzo, A.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Šarčević, N.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Therreau, C.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Wack, O.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wenz, D.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Zopounidis, J. P.; Hoferichter, M.; Klos, P.; Menéndez, J.; Schwenk, A.; Xenon Collaboration Bibcode: 2019PhRvL.122g1301A Altcode: 2018arXiv181112482A We present first results on the scalar coupling of weakly interacting massive particles (WIMPs) to pions from 1 t yr of exposure with the XENON1T experiment. This interaction is generated when the WIMP couples to a virtual pion exchanged between the nucleons in a nucleus. In contrast to most nonrelativistic operators, these pion-exchange currents can be coherently enhanced by the total number of nucleons and therefore may dominate in scenarios where spin-independent WIMP-nucleon interactions are suppressed. Moreover, for natural values of the couplings, they dominate over the spin-dependent channel due to their coherence in the nucleus. Using the signal model of this new WIMP-pion channel, no significant excess is found, leading to an upper limit cross section of 6.4 ×10-46 cm2 (90% confidence level) at 30 GeV /c2 WIMP mass. Title: VizieR Online Data Catalog: Lithium abundances of KOIs from CKS spectra (Berger+, 2018) Authors: Berger, T. A.; Howard, A. W.; Boesgaard, A. M. Bibcode: 2019yCat..18550115B Altcode: One key follow-up survey of Kepler-discovered exoplanets is the California Kepler Survey (CKS) (Petigura+ 2017, J/AJ/154/107), which was proposed to measure precise stellar parameters (Teff, logg, [Fe/H], vsini) by using local thermodynamic equilibrium (LTE) modeling of Keck-HIRES spectra of ~1000 Kepler FGK stars. Most spectra have signal-to-noise ratios (S/Ns) of ~45 per pixel, or ~90 per resolution element at 6700Å, with a resolution R=55000 and wavelength coverage from 3642-7990Å. S/N ranges from ~5 to ~200.

(3 data files). Title: Skynet Algorithm for Single-dish Radio Mapping. I. Contaminant-cleaning, Mapping, and Photometering Small-scale Structures Authors: Martin, J. R.; Reichart, D. E.; Dutton, D. A.; Maples, M. P.; Berger, T. A.; Ghigo, F. D.; Haislip, J. B.; Shaban, O. H.; Trotter, A. S.; Barnes, L. M.; Paggen, M. L.; Gao, R. L.; Salemi, C. P.; Langston, G. I.; Bussa, S.; Duncan, J. A.; White, S.; Heatherly, S. A.; Karlik, J. B.; Johnson, E. M.; Reichart, J. E.; Foster, A. C.; Kouprianov, V. V.; Mazlin, S.; Harvey, J. Bibcode: 2019ApJS..240...12M Altcode: 2018arXiv180806128M We present a single-dish mapping algorithm with a number of advantages over traditional techniques. (1) Our algorithm makes use of weighted modeling, instead of weighted averaging, to interpolate between signal measurements. This smooths the data, but without blurring the data beyond instrumental resolution. Techniques that rely on weighted averaging blur point sources sometimes by as much as 40%. (2) Our algorithm makes use of local, instead of global, modeling to separate astronomical signal from instrumental and/or environmental signal drift along the telescope’s scans. Other techniques, such as basket weaving, model this drift with simple functional forms (linear, quadratic, etc.) across the entirety of scans, limiting their ability to remove such contaminants. (3) Our algorithm makes use of a similar, local modeling technique to separate astronomical signal from radio-frequency interference (RFI), even if only continuum data are available. (4) Unlike other techniques, our algorithm does not require data to be collected on a rectangular grid or regridded before processing. (5) Data from any number of observations, overlapping or not, may be appended and processed together. (6) Any pixel density may be selected for the final image. We present our algorithm and evaluate it using both simulated and real data. We are integrating it into the image-processing library of the Skynet Robotic Telescope Network, which includes optical telescopes spanning four continents, and now also Green Bank Observatory’s 20 m diameter radio telescope in West Virginia. Skynet serves hundreds of professional users, and additionally tens of thousands of students, of all ages. Default data products are generated on the fly, but will soon be customizable after the fact. Title: Roadmap for Reliable Ensemble Forecasting of the Sun-Earth System Authors: Nita, Gelu; Angryk, Rafal; Aydin, Berkay; Banda, Juan; Bastian, Tim; Berger, Tom; Bindi, Veronica; Boucheron, Laura; Cao, Wenda; Christian, Eric; de Nolfo, Georgia; DeLuca, Edward; DeRosa, Marc; Downs, Cooper; Fleishman, Gregory; Fuentes, Olac; Gary, Dale; Hill, Frank; Hoeksema, Todd; Hu, Qiang; Ilie, Raluca; Ireland, Jack; Kamalabadi, Farzad; Korreck, Kelly; Kosovichev, Alexander; Lin, Jessica; Lugaz, Noe; Mannucci, Anthony; Mansour, Nagi; Martens, Petrus; Mays, Leila; McAteer, James; McIntosh, Scott W.; Oria, Vincent; Pan, David; Panesi, Marco; Pesnell, W. Dean; Pevtsov, Alexei; Pillet, Valentin; Rachmeler, Laurel; Ridley, Aaron; Scherliess, Ludger; Toth, Gabor; Velli, Marco; White, Stephen; Zhang, Jie; Zou, Shasha Bibcode: 2018arXiv181008728N Altcode: The authors of this report met on 28-30 March 2018 at the New Jersey Institute of Technology, Newark, New Jersey, for a 3-day workshop that brought together a group of data providers, expert modelers, and computer and data scientists, in the solar discipline. Their objective was to identify challenges in the path towards building an effective framework to achieve transformative advances in the understanding and forecasting of the Sun-Earth system from the upper convection zone of the Sun to the Earth's magnetosphere. The workshop aimed to develop a research roadmap that targets the scientific challenge of coupling observations and modeling with emerging data-science research to extract knowledge from the large volumes of data (observed and simulated) while stimulating computer science with new research applications. The desire among the attendees was to promote future trans-disciplinary collaborations and identify areas of convergence across disciplines. The workshop combined a set of plenary sessions featuring invited introductory talks and workshop progress reports, interleaved with a set of breakout sessions focused on specific topics of interest. Each breakout group generated short documents, listing the challenges identified during their discussions in addition to possible ways of attacking them collectively. These documents were combined into this report-wherein a list of prioritized activities have been collated, shared and endorsed. Title: Robust Chauvenet Outlier Rejection Authors: Maples, M. P.; Reichart, D. E.; Konz, N. C.; Berger, T. A.; Trotter, A. S.; Martin, J. R.; Dutton, D. A.; Paggen, M. L.; Joyner, R. E.; Salemi, C. P. Bibcode: 2018ApJS..238....2M Altcode: 2018arXiv180705276M Sigma clipping is commonly used in astronomy for outlier rejection, but the number of standard deviations beyond which one should clip data from a sample ultimately depends on the size of the sample. Chauvenet rejection is one of the oldest, and simplest, ways to account for this, but, like sigma clipping, it depends on the sample’s mean and standard deviation, neither of which are robust quantities: both are easily contaminated by the very outliers they are being used to reject. Many, more robust measures of central tendency, and of sample deviation, exist, but each has a trade-off with precision. Here we demonstrate that outlier rejection can be both very robust and very precise if decreasingly robust but increasingly precise techniques are applied in sequence. To this end, we present a variation on Chauvenet rejection that we call “robust” Chauvenet rejection (RCR), which uses three decreasingly robust/increasingly precise measures of central tendency and four decreasingly robust/increasingly precise measures of sample deviation. We show this sequential approach to be very effective for a wide variety of contaminant types, even when a significant—even dominant—fraction of the sample is contaminated, and especially when the contaminants are strong. Furthermore, we have developed a bulk-rejection variant, to significantly decrease computing times, and RCR can be applied both to weighted data and when fitting parameterized models to data. We present aperture photometry in a contaminated, crowded field as an example. RCR may be used by anyone at https://skynet.unc.edu/rcr, and source code is available there as well. Title: Dark Matter Search Results from a One Ton-Year Exposure of XENON1T Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Elykov, A.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Grandi, L.; Greene, Z.; Qiu, H.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Itay, R.; Joerg, F.; Kaminsky, B.; Kazama, S.; Kish, A.; Koltman, G.; Landsman, H.; Lang, R. F.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Mahlstedt, J.; Manfredini, A.; Marrodán Undagoitia, T.; Masbou, J.; Masson, D.; Messina, M.; Micheneau, K.; Miller, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pelssers, B.; Piastra, F.; Pienaar, J.; Pizzella, V.; Plante, G.; Podviianiuk, R.; Priel, N.; Ramírez García, D.; Rauch, L.; Reichard, S.; Reuter, C.; Riedel, B.; Rizzo, A.; Rocchetti, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schulte, D.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Thers, D.; Toschi, F.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Wack, O.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Xenon Collaboration Bibcode: 2018PhRvL.121k1302A Altcode: 2018arXiv180512562A We report on a search for weakly interacting massive particles (WIMPs) using 278.8 days of data collected with the XENON1T experiment at LNGS. XENON1T utilizes a liquid xenon time projection chamber with a fiducial mass of (1.30 ±0.01 ) t o n , resulting in a 1.0 ton yr exposure. The energy region of interest, [1.4 ,10.6 ] keVee ([4.9 ,40.9 ] keVnr ), exhibits an ultralow electron recoil background rate of [82-3+5(syst ) ±3 (stat ) ] events /(t o n yr keVee) . No significant excess over background is found, and a profile likelihood analysis parametrized in spatial and energy dimensions excludes new parameter space for the WIMP-nucleon spin-independent elastic scatter cross section for WIMP masses above 6 GeV /c2, with a minimum of 4.1 ×10-47 cm2 at 30 GeV /c2 and a 90% confidence level. Title: ESA Active Dosimeter a Technolgy Demonstration for ISS and beyond Authors: Straube, Ulrich; Berger, Thomas Bibcode: 2018cosp...42E3270S Altcode: Human presence in space has increased significantly over the last decade. Extended space flights supported by various international crews that lasted half a year and longer became a reality. Challenges to human health and well-being proofed to remain significant and increasing with mission-length and workload. Ongoing strong efforts did enable for such mission scenarios and shall do so for the future, the human journey to deep space that is intended. Several of the risks arising seem to have the potential to be mitigated and finally covered sufficiently. Despite health risks from ionizing radiation during extended exploratory deep space missions remain to be of significance and may strongly limit human presence and mission goals beyond Low Earth Orbit. The ESA Active Dosimeter [EAD] hardware enables for advanced personal dosimetry capabilities in real time. The system consists of several small portable Personal Active Dosimeters (MU = Mobile Unit's) as well as a surface attached docking station, called "Personal Storage Device (PSD)". The PSD provides data read-out data and advanced display capabilities as well as data storage and telemetry. The PSD contains a Tissue Equivalent Proportional Counter (TEPC) and an internal MU (iMU) for advanced analysis of the complex radiation environment in the space station and to ensure means of cross calibrations. The MU is applied for personal dosimetry as well as used for area monitoring purposes throughout the station. Verification of the system capabilities have been successfully executed in flight on ISS. Further utilization has been recommend by the ISS partner agencies. System developments and testing, including operations during a future flight of NASA's Orion program, is en-route. This presentation will give an overview of the relevant data from the first year of operations on ISS. Title: Round Table Discussion - Part 1: The Future of Space Radiation Research Authors: Hellweg, Christine; Ottolenghi, Andrea; Sun, Yeqing; Berger, Thomas Bibcode: 2018cosp...42E1428H Altcode: Space radiation is the "Number One Health Risk" (Chancellor et al., 2014) for long-term space missions beyond Low Earth Orbit (LEO). During space missions, astronauts are chronically exposed to galactic cosmic radiation (GCR) consisting of energetic protons, helium and heavier nuclei up to iron. This chronic exposure increases the risk for developing cancer and degenerative diseases (cataract of the eye lens, and possibly also decrements of the central nervous system (CNS) and other organ systems). The extents of these risks and the underlying mechanisms have to be further elucidated. In addition to the baseline exposure to GCR, Solar particle events (SPEs) bear the risk of acute high dose exposure, and might even provoke the acute radiation syndrome. Mitigation of the space radiation risks necessitates a multidisciplinary approach, from understanding the nature of the space radiation environment, the development of relevant radiation dosimeter systems, having the relevant tools to model the radiation environment, understanding the influence of shielding to the biological effects of space radiation, and being able to develop relevant countermeasures. The invited speakers of the cross discipline talks of the session F2.5 will discuss the upcoming challenges in the fields of space radiation physics, dosimetry, and modeling, biology and countermeasure development.References:Chancellor JC, Scott GBI,1, Sutton JP (2014) Space Radiation: The Number One Risk to Astronaut Health beyond Low Earth Orbit. Life (Basel). 2014 Sep; 4(3): 491-510. Title: The september 2017 solar energetic particle event observed by MSL/RAD on the surface of mars Authors: Ehresmann, Bent; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Rafkin, Scot; Guo, Jingnan; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Matthiä, Daniel; Lohf, Henning; Kristoffer Appel, Jan; Hassler, Donald M. Bibcode: 2018cosp...42E.966E Altcode: The Radiation Assessment Detector (RAD) has been continuously monitoring the Martian surface radiation environment in Gale crater as part of NASA's Mars Science Laboratory (MSL) mission since August 2012. On September 11 2017, RAD detected the strongest SEP event on the Martian surface to date. This event lead to the highest radiation levels since the beginning of the RAD operations in Gale crater. The SEPs associated with this solar storm increased the surface radiation dose by a factor of 3 over the course of a few hours, and the peak radiation dose was more than 50% higher than the previous maximum measured in October 2013.Here, we give an overview of the heliospheric conditions during the September 2017 solar storm, and present measurements of charged particle spectra during and before the event. RAD saw significant increases in the surface proton and helium fluxes, as well as in the neutral particles (neutrons and gamma-rays) created by interactions of the SEPs with the atmosphere and soil. Title: Scene-Setting talk: Solar Activity Forecasting in Practice Authors: Berger, Thomas Bibcode: 2018shin.confE.159B Altcode: We review the state-of-the-art in solar activity and resultant space weather event forecasting as well as some of the challenges, both Grand and mundane, as a scene-setting talk for Session 22 Title: Three-dimensional Velocity Measurements in Solar Prominence Bubbles and Combined Kelvin-Helmholtz/Rayleigh-Taylor Instability Authors: Berger, Thomas; Hillier, Andrew; Liu, Wei Bibcode: 2018cosp...42E.293B Altcode: We present measurements of flow velocities in solar prominences that display so-called "prominence bubble" events. Prominence bubbles are large-scale buoyant intrusions into prominences that rise from below and penetrate into the overlying plasma. They are believed to be due to magnetic flux emergence below prominences and can trigger Rayleigh-Taylor and Kelvin-Helmholtz instability flows as they interact with the overlying prominence. Prominence bubbles frequently result in the formation of plumes that rise into, or entirely through, the overlying prominence. This presents a mechanism for increasing magnetic flux and helicity in the associated coronal magnetic flux tubes, which are key for their eventual loss of equilibrium and eruptions as coronal mass ejections (CMEs). In this presentation, Hinode/Solar Optical Telescope (SOT) and Interface Region Imaging Spectrograph (IRIS) observations are analyzed to infer three-dimensional flow vectors in the "boundary layer" above several prominence bubble events. IRIS Doppler velocity measurements indicate flow speeds of 50-100 km/sec perpendicular to the sky plane, consistent with flow speeds inferred from combined Kelvin-Helmholtz/Rayleigh-Taylor instability analysis using typical quiescent prominence density and magnetic flux density values. With these typical values, flow speeds and magnetic flux densities within the bubbles can be inferred to be on the order of 100 km/sec and 10 Gauss, respectively. We discuss the implications of these novel results, and in particular, the potential for strong shear flows at the bubble boundary to trigger Kelvin-Helmholtz instability waves that develop into large-scale Rayleigh-Taylor instability plumes. Title: Radiation measurements and dosimetry for deep-space exploration Authors: Ehresmann, Bent; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Rafkin, Scot; Guo, Jingnan; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Matthiä, Daniel; Lohf, Henning; Kristoffer Appel, Jan; Hassler, Donald M. Bibcode: 2018cosp...42E.965E Altcode: Dosimetry and radiation monitoring are key factors for the planning of future human exploration on deep-space missions outside of Low-Earth Orbit (LEO), as radiation exposure poses one of the major health risks for astronauts in deep space. The amount of radiation dose astronauts would accumulate during typical mission scenarios and durations can potentially exceed currently allowable exposure limits within months.In space radiation monitoring the three main areas of concern are: 1) high-energy and deeply-penetrating Galactic Cosmic Rays (GCRs); 2) impulsive Solar Energetic Particle (SEP) events with high flux intensities up to a few hundred MeVs; and 3) secondary neutrons created by interactions of primary radiation with spacecraft material or planetary atmospheres and soils. Furthermore, in-situ radiation measurements provide invaluable input for radiation transport models that are used to calculate expected radiation exposures and shielding effectiveness, and subsequently potential health risks for future deep-space mission scenarios.Here, we present an overview of dosimetry in LEO, lunar orbit, and in deep space, and place the findings from years of measurements in context of what our current state of knowledge of space radiation implies for future exploration missions. Because the planet Mars is a prime goal for future exploration, we will focus in more detail on measurements conducted on the Martian surface with the Radiation Assessment Detector (RAD) as part of the Mars Science Laboratory (MSL) mission. Since Mars lacks a global magnetic field and its atmosphere is very thin, the surface is only weakly protected from impacts of GCRs and SEPs. This makes understanding and assessing the Martian surface radiation environment a key goal for future exploration. MSL/RAD has been characterizing in detail the charged and neutral particle environment induced by GCRs, as well as during short-term radiation enhancements from SEP events arriving at Mars.We will discuss the capabilities of the existing space dosimetry instrumentation, as well as highlight areas outside the current scope where we need to improve our understanding of the space radiation environment. Title: The Lunar Lander Neutron & Dosimetry (LND) Experiment on Chang'E4 Authors: Wimmer-Schweingruber, Robert; Hellweg, Christine; Berger, Thomas; Boettcher, Stephan; Burmeister, Soenke; Seimetz, Lars; Schuster, Bjoern; Guo, Jingnan; Zhang, Shenyi; Lohf, Henning; Yu, Jia; Knierim, Violetta; Shen, G.; Yuan, B. Bibcode: 2018cosp...42E3672W Altcode: Chang'E4, the next Chinese mission to the Moon, is planned to launch in December 2018 and to land on the far side of the Moon in the South Pole Aitken Basin. The mission consists of a lander, a rover, and a communication relay around the Earth-Moon L2 libration point. Here we describe the Lunar Lander Neutron & Dosimetry experiment (LND) on the lander. It consists of a stack of 10 segmented Si solid-state detectors (SSDs) which forms a particle telescope to measure charged particles (electrons 150-500 keV, protons 12-30 MeV, and heavier nuclei 15-30 MeV/nuc). A special geometrical arrangement allows observations of fast neutrons (and g-rays) which are also important for dosimetry and cosmic-ray exposure of lunar soils. Thermal neutrons are measured using a very thin Gd conversion foil which is sandwiched between two SSDs. Thermal neutrons are sensitive to subsurface water and important to understand lunar surface mixing processes. Despite the aim of landing humans on the Moon in the not too distant future, radiation measurements in the vicinity of the Moon are remarkably scarce. Fairly recent measurements in lunar orbit were provided by the Radiation Dose Monitor (RADOM) on board Chandrayaan-1. The spacecraft reached its operational 100 km circular orbit on November 12, 2008. Measurements showed a dose rate of 0.23 mGy per day averaged over 3545 hours of measurement time (20/11/2008 to 18/5/2009). Newer measurements have been provided by the Cosmic Ray Telescope for the Effects of Radiation (CRaTER) instrument on board the Lunar Reconnaissance Orbiter (LRO). CRaTER measured a radiation exposure of about 0.22 _ 0.27 mGy per day in its 50 km orbit. In comparison with these meager orbital data, there is a real dearth of data on the lunar surface. The current knowledge about the radiation environment on the surface of the Moon is based exclusively on calculations using radiation transport models with input parameters from models for the galactic cosmic ray spectra and for solar particle events. This is highly questionable, especially since we know that these models are fraught with uncertainties. Thus LND will provide the first active dosimetry measurements on the surface of the Moon.In this presentation we will discuss the science, implementation, and status of LND on China's Chang'E4 mission. Title: Are "Solar Tornadoes" Really Rotating? Authors: Liu, Wei; Chye Low, Boon; Okamoto, Joten; Berger, Thomas Bibcode: 2018cosp...42E2053L Altcode: Solar "tornadoes" have been proposed to explain certain vertical structures in prominences that exhibit apparent rotations. Yet, it remains highly controversial whether such motions are real rotations or transverse oscillations. We present a statistical study of IRIS observations that reveal no clear evidence of systematic or coherent rotations, which would otherwise result in opposite Doppler shifts, i.e., blueshifts on the one side of the vertical structure and redshifts on the other, which were not found in our sample of "tornadoes". In addition, we find in one particular case observed by SDO/AIA that the "tornado" disappeared upon the impact of an eruption that pushed its mass away along a primarily horizontal trajectory (presumably along magnetic field lines). This "tornado" shortly reformed with the replenishment of material from the return flow of some of the displaced mass back to its original location, at the dips of local magnetic field lines, followed by back and forth transverse oscillations around the dips. Such observations from both IRIS and AIA suggest that, at least for the cases being analyzed here, the apparent oscillatory motions of "tornadoes" are a result of longitudinal oscillations (like a pendulum) of dense and heavy prominence material about the local minimum of gravitational potential at the magnetic dips, an interpretation proposed and supported by a number of authors. Title: Cool Material in the Hot Solar Corona and the Chromosphere-Corona Mass Cycle Authors: Liu, Wei; Vial, Jean-Claude; Antolin, Patrick; Sun, Xudong; Berger, Thomas Bibcode: 2018cosp...42E2052L Altcode: In the million-degree hot and tenuous solar corona, under favorable conditions, some mass can undergo a radiative cooling instability and condense into material of 100 times cooler in two distinct forms - prominences and coronal rain. Being at similar temperatures, they exhibit contrasting morphologies and behaviors: a quiescent prominence usually consists of numerous long-lasting, filamentary downflow threads, while coronal rain consists of transient mass blobs falling at comparably higher speeds along well-defined, curved paths (e.g., guided by coronal loops). We report recent imaging and spectroscopic observations from SDO/AIA and IRIS of a hybrid prominence-coronal rain complex structure that suggest different magnetic environments being responsible for such distinctions. We also present an ensemble of observations of the so-called funnel prominences that reside near the dips of magnetic funnels. Regardless of their morphological and behavioral differences, a large fraction of prominence and coronal rain material eventually falls back to the chromosphere and serves as the return flow of the so-called chromosphere-corona mass cycle (the other half of this cycle is the upward transport of heated mass from the chromosphere to the corona). We estimate the downflow mass fluxes in prominences and coronal rain, and compare them with the coronal mass budget in this cycle and with the mass loss to the solar wind and coronal mass ejections (CMEs). We will discuss the broad physical implications of these observations for fundamental questions, such as coronal heating and beyond. Title: Predicting Solar Eruptive Events Using Artificial Neural Networks Authors: Poduval, Bala; Berger, Tom Bibcode: 2018shin.confE.157P Altcode: Solar eruptive events, such as coronal mass ejections (CMEs), are the major sources of space weather events, causing disruptions and damages to our technological infrastructure, and endangering humans in space. Prediction of such eruptive events is highly challenging mainly because of lack of a single physics-based model adequately representing the complex solar dynamo and the magnetized, turbulent plasma. Methods of artificial intelligence (AI) can develop algorithms to identify patterns in long-stretches of data and make effective predictions with reasonable accuracy. Making use of deep neural networks (DNNs), we make an attempt to predict a few events in the SHARP catalog. Presented here are the results and accuracies of our prediction. Title: Facilitating Advancements in Space Weather Data Availability Through a Space Weather Testbed and Data Portal Authors: Pankratz, Christopher; Baker, Daniel N.; Elkington, Scot; Berger, Thomas; Jaynes, Allison; Craft, James; Baltzer, Thomas; Sanchez, Fernando Bibcode: 2018cosp...42E2572P Altcode: Society has grown reliant on complex and highly interconnected technological systems, which makes us increasingly vulnerable to the effects of space weather events. An extreme space weather event today could conceivably impact many of the crucial systems we rely on, including disrupting operating earth-orbiting satellites, potential collapse of electrical grids, and impairing navigation, communication, and remote sensing capabilities. Thus, it is imperative that the scientific community address the question of just how severe events might become and to ensure stakeholders have access to the essential data needed for research and decision making. Stakeholders include policy makers and public safety officials who need to be informed by the facts on what might happen during extreme conditions. This requires essentially extremely timely up-to-the-minute alerts, warnings, and also forecasts of severe space weather events, which in turn demands measurements, models, and associated data products to be available via the most effective data discovery and access methods possible. Similarly, advancement in the fundamental scientific understanding of space weather processes is also vital, requiring that researchers have convenient and effective access to a wide variety of data sets and models from multiple sources. The space weather research community, as with many scientific communities, must access data from dispersed and often uncoordinated data repositories to acquire the data necessary for the analysis and modeling efforts that advance our understanding of solar influences and space physics on the Earth's environment. The University of Colorado (CU) is a leading institution in both producing data products and advancing the state of scientific understanding of space weather processes, is well positioned to address many of these issues. CU is inaugurating a dedicated Space Weather Technology, Research, and Education Center (SWx TREC) that will serve many of these needs, including implementation of an interoperable data portal intended to more effectively serve the needs of the Space Weather research community, as well as facilitating the advancement of models into production/operational use. In this presentation, we will outline the motivating factors for effective space weather data access and present plans and methods for meeting model testing/incubation needs, as well as the data management and access needs of the disparate communities who require space weather data and information. Title: Towards Space Exploration of Moon, Mars & Neos: Radiation Biological Basis Authors: Hellweg, Christine; Baumstark-Khan, Christa; Berger, Thomas Bibcode: 2018cosp...42E1427H Altcode: Radiation has emerged as the most critical issue to be resolved for long-term missions both orbital and interplanetary. Astronauts are constantly exposed to galactic cosmic radiation (GCR) of various energies at a low dose rate. Primarily late tissue sequels like genetic alterations, cancer and non-cancer effects, i.e. cataracts and degenerative diseases of e.g. the central nervous system or the cardiovascular system, are the potential risks. Cataracts were observed to occur earlier and more often in astronauts exposed to higher proportions of galactic ions (Cucinotta et al., 2001). Predictions of cancer risk and acceptable radiation exposure in space are subject to many uncertainties including the relative biological effectiveness (RBE) of space radiation especially heavy ions, dose-rate effects and possible interaction with microgravity and other spaceflight environmental factors. The initial cellular response to radiation exposure paves the way to late sequelae and starts with damage to the DNA which complexity depends on the linear energy transfer (LET) of the radiation. Repair of such complex DNA damage is more challenging and requires more time than the repair of simple DNA double strand breaks (DSB) which can be visualized by immunofluorescence staining of the phosphorylated histone 2AX (γH2AX) and might explain the observed prolonged cell cycle arrests induced by high-LET in comparison to low-LET irradiation. Unrepaired or mis-repaired DNA DSB are proposed to be responsible for cell death, mutations, chromosomal aberrations and oncogenic cell transformation. Cell killing and mutation induction are most efficient in an LET range of 90-200 keV/μm. Also the activation of transcription factors such as Nuclear Factor κB (NF-κB) and gene expression shaping the cellular radiation response depend on the LET with a peak RBE between 90 and 300 keV/μm. Such LET-RBE relationships were observed for cataract and cancer induction by heavy ions in laboratory animals, with varying maximal efficiencies. Furthermore, there is always the added risk of acute exposure to high proton fluxes during a solar particle event (SPE), which can threaten immediate survival of the astronauts in case of insufficient shielding by eliciting the acute radiation syndrome. Its symptoms depend on absorbed total radiation dose, type of radiation, the dose distribution in the body and the individual radiation sensitivity. After the prodromal stage with nausea and vomiting and a subsequent symptom-free phase, depending on dose, the hematopoietic syndrome with suppression of the acquired immune system and thrombocytopenia (0.7-4 Sv), the gastrointestinal tract syndrome (5-12 Sv) or the central nervous system syndrome (> 20 Sv) develop and they are accompanied by exacerbated innate immune responses. Exposure to large SPE has to be avoided by warning systems and stay inside a radiation shelter during the event. Treatment options encompass e.g. the administration of colony-stimulating factors (CSF), growth factors and blood transfusions to overcome the hematopoietic syndrome and the administration of antibiotics against secondary infections. A concerted action of ground-based studies and space experiments is required to improve the radiobiological basis of space radiation risk assessment and countermeasure development.Reference:Cucinotta FA, Manuel FK, Jones J, Iszard G, Murrey J, Djojonegro B and Wear M (2001) Space Radiation and Cataracts in Astronauts. Rad Res 156, 460-466 Title: The DOSIS 3D Project Onboard the International Space Station - Analysis of the Solar Particle Event in September 2017 Authors: Burmeister, Soenke; Berger, Thomas; Matthiä, Daniel; Bruedern, Maximilian Bibcode: 2018cosp...42E.473B Altcode: Besides the effects of the microgravity environment, and the psychological and psychosocial problems encountered in confined spaces, radiation is the main health detriment for long duration human space missions. The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones encountered on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station ISS is therefore needed. As a follow up to the DOSIS experiment (2009 - 2011) DOSIS 3D measures since May 2012 the spatial and temporal variations of the radiation field in Columbus. The active part the DOSIS MAIN BOX thereby consist of two active radiation detectors (Dosimetry Telescopes = DOSTELs) with a DDPU (DOSTEL Data and Power Unit) is mounted in a Nomex pouch at a fixed location in the bottom area of the European Physiology Module rack (EPM).The temporal variation in dependence of ISS altitude and solar cycle has been measured with the DOSTEL instruments since May 2012 covering thereby already 6 years of continuous measurements in the frame of DOSIS 3D. Of special interest was the first Solar Particle Event (SPE) (GLE 72) measured inside the Space Station within the DOSIS 3D project in September 2017. This was the first event measured since 2012 inside the ISS and in terms of exploration missions extremely important, since it was also measured in Moon orbit and at the surface of Mars. The presentation will focus on the timeline of the event observed inside Columbus and provide data for dose and relevant energy deposition spectra and also show first comparisons with GEANT4 simulations. It will also provide comparison with events observed with DOSTEL like instruments on space station MIR (1997) and on ISS (2001).The CAU contributions to DOSIS and DOSIS 3D are financially supported by BMWi under Grants 50WB0826, 50WB1026, 50WB1232 and 50WB1533. Title: The 2015 - Present Rise of the GCR as observed by RAD on Mars Authors: Wimmer-Schweingruber, Robert; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Guo, Jingnan; Ehresmann, Bent; Zeitlin, Cary; Matthiä, Daniel; Lohf, Henning; Hassler, Donald M.; von Forstner, Johan Lauritz Freiherr; Khaksari, Salman; Thorben Lundt, Niklas Bibcode: 2018cosp...42E3670W Altcode: The radiation exposure due to galactic cosmic rays has been rising since early 2015 and is reaching some of the highest levels observed in the space age. This observation is not limited to the near-Earth space environment, but is also seen at Mars in measurements performed by the highly capable Radiation Assessment Detector (RAD) on NASA's Curiosity rover. We will discuss the increased radiation exposure at Mars and elsewhere, put into the larger heliospheric context and discuss implications for human exploration. Title: Space Radiation and Human Exploration on the Moon, Mars and Neos - Dosimetry, Models and Challenges Authors: Berger, Thomas; Hellweg, Christine; Uchihori, Yukio; Matthiä, Daniel Bibcode: 2018cosp...42E.294B Altcode: Space programs are shifting towards planetary exploration and, in particular, towards missions by human beings to the Moon and to Mars. Radiation is considered to be one of the major hazards for human long-term missions beyond Low Earth Orbit (LEO). During transit to these far away destinations and during relevant extravehicular activities (EVA) on their surface, complete shielding of the highly energetic particles is impracticable. The two sources of radiation that can impact a mission outside the Earth's magnetic field are Solar Energetic Particles (SEP) and Galactic Cosmic Rays (GCR). The main goal for exploration missions is therefore the quantification and reduction of space radiation health hazards, with the goal of maximizing the number of days that may be spent in space. The research to be carried out has to support all phases of exploration including mission planning, component design, operation and post-flight studies. Having this in mind this calls for novel and improved radiation detector assemblies as well as extended calibrations, detector intercomparisons and analysis algorithms. New measurements are a prerequisite for reliable risk assessment, a crucial input for radiation source modelling, and are also needed for real-time calibration of the detectors thereby allowing for a detailed understanding of the radiation environment the astronauts are going to live in. For exploration missions, radiation risk assessment will predominately rely on simulation models. The reliability of these models needs to be optimized through a series of tests against a wide set of measurements at sites/conditions where instruments are available or can be made available. More and more radiation details are needed to correctly assess radiation risks, and this requires detailed model outputs to be tested against proper measurements. In the last years various radiation detector systems have been send either to the Moon (circulating in Moon orbit) or are already on the surface of Mars, providing thereby a tremendously needed data set for model validation and benchmarking and input data to face the challenges ahead of us. Title: Space Weather - Technology, Research, and Education Center (SWx-TREC) Authors: Baker, Daniel N.; Thayer, Jeffrey; Berger, Thomas Bibcode: 2018cosp...42E.164B Altcode: SWx-TREC is a new Center at the University of Colorado - Boulder initiated under a grant intended to create a center of gravity for the many units at CU working on space weather topics. TREC will be in the College of Engineering and Applied Science and the Laboratory for Atmospheric and Space Physics (LASP). It will be able to work across the usual academic boundaries to better develop and integrate space weather models, missions, and data that will have a direct benefit to the operational forecasting offices. TREC will also be the focal point for creating undergraduate, graduate, and professional courses in space weather. TREC is currently making strategic investments in research-to-operations (R2O) projects such as an improved full-physics model of Low-Earth-Orbit satellite and debris drag, as well as operations-to-research (O2R) projects including improvements to solar magnetic field measurements and models that form the basis of operational solar wind forecasting models. In addition, TREC will host a "space weather data portal" and a forecast center "test bed", enabling close interaction between operational forecasters and researchers from around the nation and the world. In short, TREC is a new academic research and technology center dedicated to helping bridge the gap between space weather research and operations, and to educating the space science workforce, from undergraduates to industry professionals. TREC will work with national and international operational forecast centers, industry, other academic groups, and NSF and NASA centers such as the NASA/NSF CCMC, to develop and transition new models and tools that improve space weather forecasting and nowcasting. TREC will also be focusing significant effort on its educational mission in alignment with CU's mission as a leading space science university. Title: Implications of the September 2017 Solar Particle Event for Human Exploration of Mars Authors: Hassler, Donald M.; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Guo, Jingnan; Ehresmann, Bent; Zeitlin, Cary; Wimmer-Schweingruber, Robert; Matthiä, Daniel Bibcode: 2018cosp...42E1393H Altcode: Although the Sun is approaching solar minimum, a series of large solar particle events (SPEs) occurred in September 2017 that impacted both Earth and Mars. In particular, the event of 10 September 2017 was the largest event that RAD has seen on the surface of Mars since it landed in 2012. Due to the modulating effect of the Martian atmosphere, the shape and intensity of these SEP spectra will differ significantly between interplanetary space and the Martian surface. Understanding how these SEP events influence the surface radiation field is crucial to assessing associated health risks for potential human missions to Mars. We will discuss in this talk the dosimetric quantities measured by MSL RAD before, during and after the Sept. 10 event, and their implications for potential human missions to Mars.MSL RAD is supported by NASA (HEOMD) under JPL subcontract #1273039 to SwRI, and by DLR in Germany under contract with Christian-Albrechts-Universitat (CAU). Title: Round Table Discussion - Part 2: The Future of Space Radiation Research Authors: Hellweg, Christine; Ottolenghi, Andrea; Sun, Yeqing; Berger, Thomas Bibcode: 2018cosp...42E1429H Altcode: Space radiation is the "Number One Health Risk" (Chancellor et al., 2014) for long-term space missions beyond Low Earth Orbit (LEO). During space missions, astronauts are chronically exposed to galactic cosmic radiation (GCR) consisting of energetic protons, helium and heavier nuclei up to iron. This chronic exposure increases the risk for developing cancer and degenerative diseases (cataract of the eye lens, and possibly also decrements of the central nervous system (CNS) and other organ systems). The extents of these risks and the underlying mechanisms have to be further elucidated. In addition to the baseline exposure to GCR, Solar particle events (SPEs) bear the risk of acute high dose exposure, and might even provoke the acute radiation syndrome. Mitigation of the space radiation risks necessitates a multidisciplinary approach, from understanding the nature of the space radiation environment, the development of relevant radiation dosimeter systems, having the relevant tools to model the radiation environment, understanding the influence of shielding to the biological effects of space radiation, and being able to develop relevant countermeasures. The invited speakers of the cross discipline talks of the session F2.5 will discuss the upcoming challenges in the fields of space radiation physics, dosimetry, and modeling, biology and countermeasure development.References:Chancellor JC, Scott GBI,1, Sutton JP (2014) Space Radiation: The Number One Risk to Astronaut Health beyond Low Earth Orbit. Life (Basel). 2014 Sep; 4(3): 491-510. Title: The DOSIS 3D Project Onboard the International Space Station - Status and Science Overview of 6 years of measurements (2012 - 2018) Authors: Berger, Thomas Bibcode: 2018cosp...42E.295B Altcode: The radiation environment encountered in space differs in nature from that on Earth, consisting mostly of highly energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on Earth for occupational radiation workers. Since the beginning of the space era the radiation exposure during space missions has been monitored with various passive and active radiation instruments. Also on-board the International Space Station (ISS) a number of area monitoring devices provide data related to the spatial and temporal variation of the radiation field in - and outside the ISS. The aim of the DOSIS 3D (2012 - ongoing) experiment is the measurement of the radiation environment within the European Columbus Laboratory of the ISS. These measurements are, on the one hand, performed with passive radiation detectors mounted at eleven locations within Columbus for the determination of the spatial distribution of the radiation field parameters and, on the other hand, with two active radiation detectors (DOSTEL) mounted at a fixed position inside Columbus for the determination of the temporal variation of the radiation field parameters. The talk will give an overview of the current results of the data evaluation performed for the passive and active radiation detectors for DOSIS 3D in the years 2012 to 2018 and further focus on the work in progress for data comparison with other passive and active radiation detector systems measuring on-board the ISS. Acknowledgments: The participation of the Technische Universität Wien, Atominstitut (ATI), Vienna, Austria in the DOSIS-1 and -2 experiments was supported by the Austrian Space Applications Programme (ASAP) under contract no. 819643. The Polish contribution for the Institute of Nuclear Physics (IFJ), Krakow, Poland was supported by the National Science Center (project No DEC-2012/06/M/ST9/00423). MTA EK greatly acknowledges the possibility to participate in the project to DLR and to the ESA PECS for the financial grant No. PECS4000108464. The participation of the Nuclear Physics Institute of the Czech Academy of Sciences has been supported by the grant of Czech Science Foundation (GACR) No. 15-16622Y. The CAU, University of Kiel was supported by DLR under grants 50WB0826, 50WB1026, 50WB1232 and 50WB1533. Title: On the Nature of Funnel Prominences Authors: Liu, Wei; Chye Low, Boon; Berger, Thomas Bibcode: 2018cosp...42E2054L Altcode: It has been proposed that prominences are manifestations of a magneto-thermal convection process that involves ever-present dynamic descents of cool material threads and upflows of hot bubbles and plumes (Berger et al. 2011 Nature). On global scales, prominences may play an important role as the return flows of the chromosphere-corona mass cycle. A critical step in this cycle is the condensation of million-degree coronal plasma into T<10,000 K prominence material by radiative cooling instability. Direct observational evidence has been lacking for decades, a situation that has recently changed, especially with the advent of the SDO mission. We present here SDO/AIA observations of runaway cooling in coronal loops leading to condensation at magnetic dips and formation of funnel-shaped prominences (e.g., Liu et al. 2012, 2014; Berger et al. 2012 ApJL). We find that a macroscopically quiescent prominence is microscopically dynamic, involving the passage (through condensation and drainage) of a significant mass of typically 10^{15} gram/day (comparable to the mass of a typical CME). This picture is further supported by the theoretical development on spontaneous formation of current sheets and condensations (Low et al. 2012a, b, ApJ). Such funnel prominences, usually small in size, can constitute a new type of prominences. We suggest that similar processes could produce elementary building blocks of large-scale quiescent prominences in filament channels. Title: Energetic Particle Radiation Environment Observed by RAD on the Surface of Mars During the September 2017 Event Authors: Ehresmann, B.; Hassler, D. M.; Zeitlin, C.; Guo, J.; Wimmer-Schweingruber, R. F.; Matthiä, D.; Lohf, H.; Burmeister, S.; Rafkin, S. C. R.; Berger, T.; Reitz, G. Bibcode: 2018GeoRL..45.5305E Altcode: The 10-12 September Solar Energetic Particle event produced the strongest increase of the radiation environment measured by the Radiation Assessment Detector on the surface of Mars since landing in August 2012. We report the details of the measurements of the energetic particle environment from Radiation Assessment Detector in Gale crater during this event. The Solar Energetic Particle event increased the low-energy proton flux (below 100 MeV) by a factor of 30, and the higher-energy proton flux by a factor of 4, above preevent levels. The 4He flux (below 100 MeV/nuc) rose by factors up to 10, and neutral particles by a factor of 2 above background. The increase started on 10 September around 19:50 UTC, peak-level fluxes were reached on the morning of 11 September and prevailed for about 10 hr before decreasing toward background levels. The onset of a Forbush decrease on 13 September decreased the proton flux below preevent intensities. Title: Analysis of the Radiation Hazard Observed by RAD on the Surface of Mars During the September 2017 Solar Particle Event Authors: Zeitlin, C.; Hassler, D. M.; Guo, J.; Ehresmann, B.; Wimmer-Schweingruber, R. F.; Rafkin, S. C. R.; Freiherr von Forstner, J. L.; Lohf, H.; Berger, T.; Matthiae, D.; Reitz, G. Bibcode: 2018GeoRL..45.5845Z Altcode: We report dosimetric quantities measured by the Mars Science Laboratory Radiation Assessment Detector (RAD) on the surface of Mars during the 10-12 September 2017 solar particle event. Despite 23 g/cm2 of CO2 shielding provided by the atmosphere above RAD, dose rates rose above background galactic cosmic ray levels by factors of 2 to 3 over the course of several hours and leveled off at sustained peak rates for about 12 hr before declining over the following 36 hr. As the solar particle event flux was gradually declining, a shock front reached Mars and caused a sudden drop of about 15% in instantaneous dose rates. No solar particles followed the shock arrival, and the magnetic shielding of galactic cosmic rays by the shock reduced their intensity to levels below those seen before the start of the event. This event is the largest seen to date by RAD on Mars. Title: Signal yields of keV electronic recoils and their discrimination from nuclear recoils in liquid xenon Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Grandi, L.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Mahlstedt, J.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Ramírez García, D.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rupp, N.; Saldanha, R.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Xenon Collaboration Bibcode: 2018PhRvD..97i2007A Altcode: 2017arXiv170910149A We report on the response of liquid xenon to low energy electronic recoils below 15 keV from beta decays of tritium at drift fields of 92 V /cm , 154 V /cm and 366 V /cm using the XENON100 detector. A data-to-simulation fitting method based on Markov Chain Monte Carlo is used to extract the photon yields and recombination fluctuations from the experimental data. The photon yields measured at the two lower fields are in agreement with those from literature; additional measurements at a higher field of 366 V /cm are presented. The electronic and nuclear recoil discrimination as well as its dependence on the drift field and photon detection efficiency are investigated at these low energies. The results provide new measurements in the energy region of interest for dark matter searches using liquid xenon. Title: The Lunar Lander Neutron and Dosimetry (LND) Experiment on Chang'e4 Authors: Wimmer-Schweingruber, R. F.; Zhang, S.; Hellweg, C. E.; Yu, J.; Guo, J.; Lohf, H.; Berger, T.; Böttcher, S. I.; Burmeister, S.; Knappmann, A. C.; Knierim, V.; Schuster, B.; Seimetz, L.; Shen, G.; Yuan, B. Bibcode: 2018LPI....49.1413W Altcode: Chang'e4 is scheduled to launch to the far side of the Moon in December 2018. LND will measure the radiation environment in preparation of human exploration. Title: Low-Energy Cosmic Rays: Radiation Environment Studies and Astrophysics on the Deep Space Gateway Authors: Losekamm, M. J.; Berger, T. Bibcode: 2018LPICo2063.3108L Altcode: The Deep Space Gateway will be ideally located to investigate the cosmic radiation that astronauts are subjected to in deep space and to help shed light on one of the most intriguing astrophysical mysteries of today: What is the universe made of? Title: Matroshka AstroRad Radiation Experiment (MARE) on the Deep Space Gateway Authors: Gaza, R.; Hussein, H.; Murrow, D.; Hopkins, J.; Waterman, G.; Milstein, O.; Berger, T.; Przybyla, B.; Aeckerlein, J.; Marsalek, K.; Matthiae, D.; Rutczynska, A. Bibcode: 2018LPICo2063.3042G Altcode: The Matroshka AstroRad Radiation Experiment is a science payload on Orion EM-1 flight. A research platform derived from MARE is proposed for the Deep Space Gateway. Feedback is invited on desired Deep Space Gateway design features to maximize its science potential. Title: Space Weather Research and Operational Observing from a Cis-Lunar Deep Space Gateway Authors: Berger, T. E.; Baker, D. N.; Woods, T. N. Bibcode: 2018LPICo2063.3147B Altcode: We review the status of observational architectures for space weather research and operational forecasting and suggest ways in which the Deep Space Gateway may act as an ideal supplement to current and future space weather observing platforms. Title: Alamos: An International Collaboration to Provide a Space Based Environmental Monitoring Solution for the Deep Space Network Authors: Kennedy, S. O.; Dunn, A.; Lecomte, J.; Buchheim, K.; Johansson, E.; Berger, T. Bibcode: 2018LPICo2063.3069K Altcode: This abstract proposes the advantages of an externally mounted instrument in support of the human physiology, space biology, and human health and performance key science area. Alamos provides Space-Based Environmental Monitoring capabilities. Title: Results from Field Testing the RIMFAX GPR on Svalbard. Authors: Hamran, S. E.; Amundsen, H. E. F.; Berger, T.; Carter, L. M.; Dypvik, H.; Ghent, R. R.; Kohler, J.; Mellon, M. T.; Nunes, D. C.; Paige, D. A.; Plettemeier, D.; Russell, P. Bibcode: 2017AGUFM.P23G..07H Altcode: The Radar Imager for Mars' Subsurface Experiment - RIMFAX is a Ground Penetrating Radar being developed for NASÁs MARS 2020 rover mission. The principal goals of the RIMFAX investigation are to image subsurface structures, provide context for sample sites, derive information regarding subsurface composition, and search for ice or brines. In meeting these goals, RIMFAX will provide a view of the stratigraphic section and a window into the geological and environmental history of Mars. To verify the design an Engineering Model (EM) of the radar was tested in the field in the spring 2017. Different sounding modes on the EM were tested in different types of subsurface geology on Svalbard. Deep soundings were performed on polythermal glaciers down to a couple of hundred meters. Shallow soundings were used to map a ground water table in the firn area of a glacier. A combination of deep and shallow soundings was used to image buried ice under a sedimentary layer of a couple of meters. Subsurface sedimentary layers were imaged down to more than 20 meters in sand stone permafrost. This presentation will give an overview of the RIMFAX investigation, describe the development of the radar system, and show results from field tests of the radar. Title: Search for bosonic super-WIMP interactions with the XENON100 experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Althueser, L.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Capelli, C.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Ramírez García, D.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Xenon Collaboration Bibcode: 2017PhRvD..96l2002A Altcode: 2017arXiv170902222X We present results of searches for vector and pseudoscalar bosonic super-weakly interacting massive particles (WIMPs), which are dark matter candidates with masses at the keV-scale, with the XENON100 experiment. XENON100 is a dual-phase xenon time projection chamber operated at the Laboratori Nazionali del Gran Sasso. A profile likelihood analysis of data with an exposure of 224.6 live days ×34 kg showed no evidence for a signal above the expected background. We thus obtain new and stringent upper limits in the (8 - 125 ) keV /c2 mass range, excluding couplings to electrons with coupling constants of ga e>3 ×10-13 for pseudo-scalar and α'/α >2 ×10-28 for vector super-WIMPs, respectively. These limits are derived under the assumption that super-WIMPs constitute all of the dark matter in our galaxy. Title: The XENON1T dark matter experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Antunes, B.; Arneodo, F.; Balata, M.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breskin, A.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Chiarini, A.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Corrieri, R.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Gangi, P. Di; Giovanni, A. Di; Diglio, S.; Disdier, J. -M.; Doets, M.; Duchovni, E.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Franco, D.; Front, D.; Fulgione, W.; Rosso, A. Gallo; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Giboni, K. -L.; Goetzke, L. W.; Grandi, L.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Huhmann, C.; Itay, R.; James, A.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Maier, R.; Manfredini, A.; Maris, I.; Undagoitia, T. Marrodán; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morå, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Orlandi, D.; Othegraven, R.; Pakarha, P.; Parlati, S.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; García, D. Ramírez; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Santos, J. M. F. dos; Saldanha, R.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Lavina, L. Scotto; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Sivers, M. v.; Stern, M.; Stein, A.; Tatananni, D.; Tatananni, L.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Upole, N.; Vargas, M.; Wack, O.; Walet, R.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wittweg, C.; Wulf, J.; Ye, J.; Zhang, Y. Bibcode: 2017EPJC...77..881A Altcode: 2017arXiv170807051X The XENON1T experiment at the Laboratori Nazionali del Gran Sasso (LNGS) is the first WIMP dark matter detector operating with a liquid xenon target mass above the ton-scale. Out of its 3.2 t liquid xenon inventory, 2.0 t constitute the active target of the dual-phase time projection chamber. The scintillation and ionization signals from particle interactions are detected with low-background photomultipliers. This article describes the XENON1T instrument and its subsystems as well as strategies to achieve an unprecedented low background level. First results on the detector response and the performance of the subsystems are also presented. Title: First Dark Matter Search Results from the XENON1T Experiment Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Gardner, R.; Geis, C.; Goetzke, L. W.; Grandi, L.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Howlett, J.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Mariş, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Riedel, B.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Saldanha, R.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Shockley, E.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thapa, S.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Upole, N.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y.; Zhu, T.; Xenon Collaboration Bibcode: 2017PhRvL.119r1301A Altcode: 2017arXiv170506655A We report the first dark matter search results from XENON1T, a ∼2000 -kg -target-mass dual-phase (liquid-gas) xenon time projection chamber in operation at the Laboratori Nazionali del Gran Sasso in Italy and the first ton-scale detector of this kind. The blinded search used 34.2 live days of data acquired between November 2016 and January 2017. Inside the (1042 ±12 )-kg fiducial mass and in the [5 ,40 ] keVnr energy range of interest for weakly interacting massive particle (WIMP) dark matter searches, the electronic recoil background was (1.93 ±0.25 )×10-4 events /(kg ×day ×keVee) , the lowest ever achieved in such a dark matter detector. A profile likelihood analysis shows that the data are consistent with the background-only hypothesis. We derive the most stringent exclusion limits on the spin-independent WIMP-nucleon interaction cross section for WIMP masses above 10 GeV /c2 , with a minimum of 7.7 ×10-47 cm2 for 35 -GeV /c2 WIMPs at 90% C.L. Title: Quiescent Prominence Dynamics Observed with the Hinode Solar Optical Telescope. II. Prominence Bubble Boundary Layer Characteristics and the Onset of a Coupled Kelvin-Helmholtz Rayleigh-Taylor Instability Authors: Berger, Thomas; Hillier, Andrew; Liu, Wei Bibcode: 2017ApJ...850...60B Altcode: 2017arXiv170705265B We analyze solar quiescent prominence bubble characteristics and instability dynamics using Hinode/Solar Optical Telescope data. We measure the bubble expansion rate, prominence downflows, and the profile of the boundary layer brightness and thickness as a function of time. The largest bubble analyzed rises into the prominence with a speed of about 1.3 {km} {{{s}}}-1 until it is destabilized by a localized shear flow on the boundary. Boundary layer thickness grows gradually as prominence downflows deposit plasma onto the bubble with characteristic speeds of 20{--}35 {km} {{{s}}}-1. Lateral downflows initiate from the thickened boundary layer with characteristic speeds of 25{--}50 {km} {{{s}}}-1, “draining” the layer of plasma. Strong shear flow across one bubble boundary leads to an apparent coupled Kelvin-Helmholtz Rayleigh-Taylor (KH-RT) instability. We measure shear flow speeds above the bubble of 10 {km} {{{s}}}-1 and infer interior bubble flow speeds on the order of 100 {km} {{{s}}}-1. Comparing the measured growth rate of the instability to analytic expressions, we infer a magnetic flux density across the bubble boundary of ∼10-3 T (10 Gauss) at an angle of ∼ 70^\circ to the prominence plane. The results are consistent with the hypothesis that prominence bubbles are caused by magnetic flux that emerges below a prominence, setting up the conditions for RT, or combined KH-RT, instability flows that transport flux, helicity, and hot plasma upward into the overlying coronal magnetic flux rope. Title: Search for magnetic inelastic dark matter with XENON100 Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Di Gangi, P.; Di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. v.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y. Bibcode: 2017JCAP...10..039A Altcode: 2017arXiv170405804X We present the first search for dark matter-induced delayed coincidence signals in a dual-phase xenon time projection chamber, using the 224.6 live days of the XENON100 science run II. This very distinct signature is predicted in the framework of magnetic inelastic dark matter which has been proposed to reconcile the modulation signal reported by the DAMA/LIBRA collaboration with the null results from other direct detection experiments. No candidate event has been found in the region of interest and upper limits on the WIMP's magnetic dipole moment are derived. The scenarios proposed to explain the DAMA/LIBRA modulation signal by magnetic inelastic dark matter interactions of WIMPs with masses of 58.0 GeV/c2 and 122.7 GeV/c2 are excluded at 3.3 σ and 9.3 σ, respectively. Title: Modelling the radiation on the Martian surface Authors: Matthiä, D.; Berger, T. Bibcode: 2017EPSC...11..655M Altcode: Radiation caused by galactic cosmic radiation can be harmful to electronics and is of interest for future manned missions. A model of the radiation exposure caused by galactic cosmic radiation on the Martian surface is presented and the results are compared to measurements by the Radiation Assessment (RAD) detector of the Mars Science Laboratory (MSL). Title: Exploiting different active silicon detectors in the International Space Station: ALTEA and DOSTEL galactic cosmic radiation (GCR) measurements Authors: Narici, Livo; Berger, Thomas; Burmeister, Sönke; Di Fino, Luca; Rizzo, Alessandro; Matthiä, Daniel; Reitz, Günther Bibcode: 2017JSWSC...7A..18N Altcode: The solar system exploration by humans requires to successfully deal with the radiation exposition issue. The scientific aspect of this issue is twofold: knowing the radiation environment the astronauts are going to face and linking radiation exposure to health risks. Here we focus on the first issue. It is generally agreed that the final tool to describe the radiation environment in a space habitat will be a model featuring the needed amount of details to perform a meaningful risk assessment. The model should also take into account the shield changes due to the movement of materials inside the habitat, which in turn produce changes in the radiation environment. This model will have to undergo a final validation with a radiation field of similar complexity. The International Space Station (ISS) is a space habitat that features a radiation environment inside which is similar to what will be found in habitats in deep space, if we use measurements acquired only during high latitude passages (where the effects of the Earth magnetic field are reduced). Active detectors, providing time information, that can easily select data from different orbital sections, are the ones best fulfilling the requirements for these kinds of measurements. The exploitation of the radiation measurements performed in the ISS by all the available instruments is therefore mandatory to provide the largest possible database to the scientific community, to be merged with detailed Computer Aided Design (CAD) models, in the quest for a full model validation. While some efforts in comparing results from multiple active detectors have been attempted, a thorough study of a procedure to merge data in a single data matrix in order to provide the best validation set for radiation environment models has never been attempted. The aim of this paper is to provide such a procedure, to apply it to two of the most performing active detector systems in the ISS: the Anomalous Long Term Effects in Astronauts (ALTEA) instrument and the DOSimetry TELescope (DOSTEL) detectors, applied in the frame of the DOSIS and DOSIS 3D project onboard the ISS and to present combined results exploiting the features of each of the two apparatuses. Title: The Fate of Cool Material in the Hot Corona: Solar Prominences and Coronal Rain Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Vial, Jean-Claude; Berger, Thomas Bibcode: 2017SPD....4810501L Altcode: As an important chain of the chromosphere-corona mass cycle, some of the million-degree hot coronal mass undergoes a radiative cooling instability and condenses into material at chromospheric or transition-region temperatures in two distinct forms - prominences and coronal rain (some of which eventually falls back to the chromosphere). A quiescent prominence usually consists of numerous long-lasting, filamentary downflow threads, while coronal rain consists of transient mass blobs falling at comparably higher speeds along well-defined paths. It remains puzzling why such material of similar temperatures exhibit contrasting morphologies and behaviors. We report recent SDO/AIA and IRIS observations that suggest different magnetic environments being responsible for such distinctions. Specifically, in a hybrid prominence-coronal rain complex structure, we found that the prominence material is formed and resides near magnetic null points that favor the radiative cooling process and provide possibly a high plasma-beta environment suitable for the existence of meandering prominence threads. As the cool material descends, it turns into coronal rain tied onto low-lying coronal loops in a likely low-beta environment. Such structures resemble to certain extent the so-called coronal spiders or cloud prominences, but the observations reported here provide critical new insights. We will discuss the broad physical implications of these observations for fundamental questions, such as coronal heating and beyond (e.g., in astrophysical and/or laboratory plasma environments). Title: Intrinsic backgrounds from Rn and Kr in the XENON100 experiment Authors: XENON Collaboration; Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Di Gangi, P.; Di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morå, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Piro, M. -C.; Pizzella, V.; Plante, G.; Priel, N.; Ramírez García, D.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. v.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Weber, M.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y. Bibcode: 2017arXiv170803617X Altcode: In this paper, we describe the XENON100 data analyses used to assess the target-intrinsic background sources radon ($^{222}$Rn), thoron ($^{220}$Rn) and krypton ($^{85}$Kr). We detail the event selections of high-energy alpha particles and decay-specific delayed coincidences. We derive distributions of the individual radionuclides inside the detector and quantify their abundances during the main three science runs of the experiment over a period of $\sim$ 4 years, from January 2010 to January 2014. We compare our results to external measurements of radon emanation and krypton concentrations where we find good agreement. We report an observed reduction in concentrations of radon daughters that we attribute to the plating-out of charged ions on the negatively biased cathode. Title: The fading of Cassiopeia A, and improved models for the absolute spectrum of primary radio calibration sources Authors: Trotter, A. S.; Reichart, D. E.; Egger, R. E.; Stýblová, J.; Paggen, M. L.; Martin, J. R.; Dutton, D. A.; Reichart, J. E.; Kumar, N. D.; Maples, M. P.; Barlow, B. N.; Berger, T. A.; Foster, A. C.; Frank, N. R.; Ghigo, F. D.; Haislip, J. B.; Heatherly, S. A.; Kouprianov, V. V.; LaCluyzé, A. P.; Moffett, D. A.; Moore, J. P.; Stanley, J. L.; White, S. Bibcode: 2017MNRAS.469.1299T Altcode: 2017arXiv170400002T Based on 5 yr of observations with the 40-foot telescope at Green Bank Observatory (GBO), Reichart & Stephens found that the radio source Cassiopeia A had either faded more slowly between the mid-1970s and late 1990s than Baars et al. had found it to be fading between the late 1940s and mid-1970s, or that it had rebrightened and then resumed fading sometime between the mid-1970s and mid-1990s, in the L band (1.4 GHz). Here, we present 15 additional years of observations of Cas A and Cyg A with the 40-foot in the L band, and three and a half additional years of observations of Cas A, Cyg A, Tau A and Vir A with GBO's recently refurbished 20-m telescope in the L and X (9 GHz) bands. We also present a more sophisticated analysis of the 40-foot data, and a reanalysis of the Baars et al. data, which reveals small, but non-negligible differences. We find that overall, between the late 1950s and late 2010s, Cas A faded at an average rate of 0.670 ± 0.019 per cent yr-1 in the L band, consistent with Reichart & Stephens. However, we also find, at the 6.3σ credible level, that it did not fade at a constant rate. Rather, Cas A faded at a faster rate through at least the late 1960s, rebrightened (or at least faded at a much slower rate), and then resumed fading at a similarly fast rate by, at most, the late 1990s. Given these differences from the original Baars et al. analysis, and given the importance of their fitted spectral and temporal models for flux-density calibration in radio astronomy, we update and improve on these models for all four of these radio sources. In doing so, we additionally find that Tau A is fading at a rate of 0.102^{+0.042}_{-0.043} per cent yr-1 in the L band. Title: The radiation environment on the surface of Mars - Numerical calculations of the galactic component with GEANT4/PLANETOCOSMICS Authors: Matthiä, Daniel; Berger, Thomas Bibcode: 2017LSSR...14...57M Altcode: Galactic cosmic radiation and secondary particles produced in the interaction with the atmosphere lead to a complex radiation field on the Martian surface. A workshop (;1st Mars Space Radiation Modeling Workshop;) organized by the MSL-RAD science team was held in June 2016 in Boulder with the goal to compare models capable to predict this radiation field with each other and measurements from the RAD instrument onboard the curiosity rover taken between November 15, 2015 and January 15, 2016.

In this work the results of PLANETOCOSMICS/GEANT4 contributed to the workshop are presented. Calculated secondary particle spectra on the Martian surface are investigated and the radiation field's directionality of the different particles in dependence on the energy is discussed. Omnidirectional particle fluxes are used in combination with fluence to dose conversion factors to calculate absorbed dose rates and dose equivalent rates in a slab of tissue. Title: Effective field theory search for high-energy nuclear recoils using the XENON100 dark matter detector Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morâ, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang., Y.; Farmer, B.; Xenon Collaboration Bibcode: 2017PhRvD..96d2004A Altcode: 2017arXiv170502614A We report on weakly interacting massive particles (WIMPs) search results in the XENON100 detector using a nonrelativistic effective field theory approach. The data from science run II (34 kg ×224.6 live days) were reanalyzed, with an increased recoil energy interval compared to previous analyses, ranging from (6.6 -240 ) keVnr . The data are found to be compatible with the background-only hypothesis. We present 90% confidence level exclusion limits on the coupling constants of WIMP-nucleon effective operators using a binned profile likelihood method. We also consider the case of inelastic WIMP scattering, where incident WIMPs may up-scatter to a higher mass state, and set exclusion limits on this model as well. Title: Prominence Bubble Shear Flows and the Coupled Kelvin-Helmholtz — Rayleigh-Taylor Instability Authors: Berger, Thomas; Hillier, Andrew Bibcode: 2017SPD....4820103B Altcode: Prominence bubbles are large arched structures that rise from below into quiescent prominences, often growing to heights on the order of 10 Mm before going unstable and generating plume upflows. While there is general agreement that emerging flux below pre-existing prominences causes the structures, there is lack of agreement on the nature of the bubbles and the cause of the instability flows. One hypothesis is that the bubbles contain coronal temperature plasma and rise into the prominence above due to both magnetic and thermal buoyancy, eventually breaking down via a magnetic Rayleigh-Taylor (RT) instability to release hot plasma and magnetic flux and helicity into the overlying coronal flux rope. Another posits that the bubbles are actually just “arcades” in the prominence indicating a magnetic separator line between the bipole and the prominence fields with the observed upflows and downflows caused by reconnection along the separator. We analyze Hinode/SOT, SDO/AIA, and IRIS observations of prominence bubbles, focusing on characteristics of the bubble boundary layers that may discriminate between the two hypotheses. We find speeds on the order of 10 km/s in prominence plasma downflows and lateral shear flows along the bubble boundary. Inflows to the boundary gradually increase the thickness and brightness of the layer until plasma drains from there, apparently around the dome-like bubble domain. In one case, shear flow across the bubble boundary develops Kelvin-Helmholtz (KH) vortices that we use to infer flow speeds in the low-density bubble on the order of 100 km/sec. IRIS spectra indicate that plasma flows on the bubble boundary at transition region temperatures achieve Doppler speeds on the order of 50 km/s, consistent with this inference. Combined magnetic KH-RT instability analysis leads to flux density estimates of 10 G with a field angle of 30° to the prominence, consistent with vector magnetic field measurements. In contrast, we find no evidence of the impulsive brightening or bi-directional jets that are expected from reconnection driven flows at bubble boundaries. We conclude that observations to date are consistent with the hot bubble/Rayleigh-Taylor instability hypothesis. Title: The radiation environment on the surface of Mars - Summary of model calculations and comparison to RAD data Authors: Matthiä, Daniel; Hassler, Donald M.; de Wet, Wouter; Ehresmann, Bent; Firan, Ana; Flores-McLaughlin, John; Guo, Jingnan; Heilbronn, Lawrence H.; Lee, Kerry; Ratliff, Hunter; Rios, Ryan R.; Slaba, Tony C.; Smith, Michael; Stoffle, Nicholas N.; Townsend, Lawrence W.; Berger, Thomas; Reitz, Günther; Wimmer-Schweingruber, Robert F.; Zeitlin, Cary Bibcode: 2017LSSR...14...18M Altcode: The radiation environment at the Martian surface is, apart from occasional solar energetic particle events, dominated by galactic cosmic radiation, secondary particles produced in their interaction with the Martian atmosphere and albedo particles from the Martian regolith. The highly energetic primary cosmic radiation consists mainly of fully ionized nuclei creating a complex radiation field at the Martian surface. This complex field, its formation and its potential health risk posed to astronauts on future manned missions to Mars can only be fully understood using a combination of measurements and model calculations. In this work the outcome of a workshop held in June 2016 in Boulder, CO, USA is presented: experimental results from the Radiation Assessment Detector of the Mars Science Laboratory are compared to model results from GEANT4, HETC-HEDS, HZETRN, MCNP6, and PHITS. Charged and neutral particle spectra and dose rates measured between 15 November 2015 and 15 January 2016 and model results calculated for this time period are investigated. Title: Search for WIMP inelastic scattering off xenon nuclei with XENON100 Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kazama, S.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lombardi, F.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Mora, K.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Vargas, M.; Wang, H.; Wang, Z.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y.; Xenon Collaboration Bibcode: 2017PhRvD..96b2008A Altcode: 2017arXiv170505830A We present the first constraints on the spin-dependent, inelastic scattering cross section of weakly interacting massive particles (WIMPs) on nucleons from XENON100 data with an exposure of 7.64 ×103 kg .days . XENON100 is a dual-phase xenon time projection chamber with 62 kg of active mass, operated at the Laboratori Nazionali del Gran Sasso (LNGS) in Italy and designed to search for nuclear recoils from WIMP-nucleus interactions. Here we explore inelastic scattering, where a transition to a low-lying excited nuclear state of <mml:mmultiscripts>Xe 129 </mml:mmultiscripts> is induced. The experimental signature is a nuclear recoil observed together with the prompt deexcitation photon. We see no evidence for such inelastic WIMP-<mml:mmultiscripts>Xe 129 </mml:mmultiscripts> interactions. A profile likelihood analysis allows us to set a 90% C.L. upper limit on the inelastic, spin-dependent WIMP-nucleon cross section of 3.3 ×10-38 cm2 at 100 GeV /c2 . This is the most constraining result to date, and sets the pathway for an analysis of this interaction channel in upcoming, larger dual-phase xenon detectors. Title: DOSIS & DOSIS 3D: radiation measurements with the DOSTEL instruments onboard the Columbus Laboratory of the ISS in the years 2009-2016 Authors: Berger, Thomas; Burmeister, Sönke; Matthiä, Daniel; Przybyla, Bartos; Reitz, Günther; Bilski, Pawel; Hajek, Michael; Sihver, Lembit; Szabo, Julianna; Ambrozova, Iva; Vanhavere, Filip; Gaza, Ramona; Semones, Edward; Yukihara, Eduardo G.; Benton, Eric R.; Uchihori, Yukio; Kodaira, Satoshi; Kitamura, Hisashi; Boehme, Matthias Bibcode: 2017JSWSC...7A...8B Altcode: The natural radiation environment in Low Earth Orbit (LEO) differs significantly in composition and energy from that found on Earth. The space radiation field consists of high energetic protons and heavier ions from Galactic Cosmic Radiation (GCR), as well as of protons and electrons trapped in the Earth's radiation belts (Van Allen belts). Protons and some heavier particles ejected in occasional Solar Particle Events (SPEs) might in addition contribute to the radiation exposure in LEO. All sources of radiation are modulated by the solar cycle. During solar maximum conditions SPEs occur more frequently with higher particle intensities. Since the radiation exposure in LEO exceeds exposure limits for radiation workers on Earth, the radiation exposure in space has been recognized as a main health concern for humans in space missions from the beginning of the space age on. Monitoring of the radiation environment is therefore an inevitable task in human spaceflight. Since mission profiles are always different and each spacecraft provides different shielding distributions, modifying the radiation environment measurements needs to be done for each mission. The experiments "Dose Distribution within the ISS (DOSIS)" (2009-2011) and "Dose Distribution within the ISS 3D (DOSIS 3D)" (2012-onwards) onboard the Columbus Laboratory of the International Space Station (ISS) use a detector suite consisting of two silicon detector telescopes (DOSimetry TELescope = DOSTEL) and passive radiation detector packages (PDP) and are designed for the determination of the temporal and spatial variation of the radiation environment. With the DOSTEL instruments' changes of the radiation composition and the related exposure levels in dependence of the solar cycle, the altitude of the ISS and the influence of attitude changes of the ISS during Space Shuttle dockings inside the Columbus Laboratory have been monitored. The absorbed doses measured at the end of May 2016 reached up to 286 μGy/day with dose equivalent values of 647 μSv/day. Title: The Lunar Lander Neutron and Dosimetry (LND) Experiment on Chang'e4 Authors: Wimmer-Schweingruber, R. F.; Zhang, S.; Hellweg, C. E.; Yu, J.; Guo, J.; Lohf, H.; Berger, T.; Böttcher, S. I.; Burmeister, S.; Jüngling, M.; Knappmann, A.; Knierim, V.; Schuster, B.; Seimetz, L.; Shen, G.; Steinhagen, J.; Yuan, B. Bibcode: 2017LPI....48.1320W Altcode: The Lunar Lander Neutron and Dosimetry (LND) experiment on China's lunar mission Chang'e4 will measure the neutral and charged radiation on the lunar surface. Title: STARLIFE - An International Campaign to Study the Role of Galactic Cosmic Radiation in Astrobiological Model Systems Authors: Moeller, Ralf; Raguse, Marina; Leuko, Stefan; Berger, Thomas; Hellweg, Christine Elisabeth; Fujimori, Akira; Okayasu, Ryuichi; Horneck, Gerda Bibcode: 2017AsBio..17..101M Altcode: In-depth knowledge regarding the biological effects of the radiation field in space is required for assessing the radiation risks in space. To obtain this knowledge, a set of different astrobiological model systems has been studied within the STARLIFE radiation campaign during six irradiation campaigns (2013-2015). The STARLIFE group is an international consortium with the aim to investigate the responses of different astrobiological model systems to the different types of ionizing radiation (X-rays, γ rays, heavy ions) representing major parts of the galactic cosmic radiation spectrum. Low- and high-energy charged particle radiation experiments have been conducted at the Heavy Ion Medical Accelerator in Chiba (HIMAC) facility at the National Institute of Radiological Sciences (NIRS) in Chiba, Japan. X-rays or γ rays were used as reference radiation at the German Aerospace Center (DLR, Cologne, Germany) or Beta-Gamma-Service GmbH (BGS, Wiehl, Germany) to derive the biological efficiency of different radiation qualities. All samples were exposed under identical conditions to the same dose and qualities of ionizing radiation (i) allowing a direct comparison between the tested specimens and (ii) providing information on the impact of the space radiation environment on currently used astrobiological model organisms. Title: Search for Electronic Recoil Event Rate Modulation with 4 Years of XENON100 Data Authors: The XENON collaboration; Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Butikofer, L.; Calven, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Di Gangi, P.; Di Giovanni, A.; Diglio, S.; Eurin, G.; Fei, J.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Lin, Q.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Manfredini, A.; Maris, I.; Marrodan Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Messina, M.; Micheneau, K.; Miguez, B.; Molinario, A.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Pizzella, V.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. v.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; Wang, H.; Wei, Y.; Weinheimer, C.; Wulf, J.; Ye, J.; Zhang, Y. Bibcode: 2017arXiv170100769T Altcode: We report on a search for electronic recoil event rate modulation signatures in the XENON100 data accumulated over a period of 4 years, from January 2010 to January 2014. A profile likelihood method, which incorporates the stability of the XENON100 detector and the known electronic recoil background model, is used to quantify the significance of periodicity in the time distribution of events. There is a weak modulation signature at a period of $431^{+16}_{-14}$ days in the low energy region of $(2.0-5.8)$ keV in the single scatter event sample, with a global significance of $1.9\,\sigma$, however no other more significant modulation is observed. The expected annual modulation of a dark matter signal is not compatible with this result. Single scatter events in the low energy region are thus used to exclude the DAMA/LIBRA annual modulation as being due to dark matter electron interactions via axial vector coupling at $5.7\,\sigma$. Title: XENON100 dark matter results from a combination of 477 live days Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Diglio, S.; Duchovni, E.; Fei, J.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Gallo Rosso, A.; Galloway, M.; Gao, F.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Le Calloch, M.; Levy, C.; Lin, Q.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Manfredini, A.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Meng, Y.; Messina, M.; Micheneau, K.; Miguez, B.; Molinario, A.; Murra, M.; Naganoma, J.; Ni, K.; Oberlack, U.; Orrigo, S. E. A.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Piro, M. -C.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M.; Simgen, H.; Sivers, M. V.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C. D.; Wall, R.; Wang, H.; Weber, M.; Wei, Y.; Weinheimer, C.; Wulf, J.; Zhang, Y.; Xenon Collaboration Bibcode: 2016PhRvD..94l2001A Altcode: 2016arXiv160906154X We report on WIMP search results of the XENON100 experiment, combining three runs summing up to 477 live days from January 2010 to January 2014. Data from the first two runs were already published. A blind analysis was applied to the last run recorded between April 2013 and January 2014 prior to combining the results. The ultralow electromagnetic background of the experiment, ∼5 ×10-3 events /(keVee×kg ×day ) ) before electronic recoil rejection, together with the increased exposure of 48 kg ×yr , improves the sensitivity. A profile likelihood analysis using an energy range of (6.6 - 43.3 ) keVnr sets a limit on the elastic, spin-independent WIMP-nucleon scattering cross section for WIMP masses above 8 GeV /c2 , with a minimum of 1.1 ×10-45 cm2 at 50 GeV /c2 and 90% confidence level. We also report updated constraints on the elastic, spin-dependent WIMP-nucleon cross sections obtained with the same data. We set upper limits on the WIMP-neutron (proton) cross section with a minimum of 2.0 ×10-40 cm2 (52 ×10-40 cm2 ) at a WIMP mass of 50 GeV /c2 , at 90% confidence level. Title: Probing the Physical Connection between Solar Prominences and Coronal Rain Authors: Liu, W.; Antolin, P.; Sun, X.; Vial, J. C.; Guo, L.; Gibson, S. E.; Berger, T. E.; Okamoto, J.; De Pontieu, B. Bibcode: 2016AGUFMSH43C2587L Altcode: Solar prominences and coronal rain are intimately related phenomena, both involving cool material at chromospheric temperatures within the hot corona and both playing important roles as part of the return flow of the chromosphere-corona mass cycle. At the same time, they exhibit distinct morphologies and dynamics not yet well understood. Quiescent prominences consist of numerous long-lasting, filamentary downflow threads, while coronal rain is more transient and falls comparably faster along well-defined curved paths. We report here a novel, hybrid prominence-coronal rain complex in an arcade-fan geometry observed by SDO/AIA and IRIS, which provides new insights to the underlying physics of such contrasting behaviors. We found that the supra-arcade fan region hosts a prominence sheet consisting of meandering threads with broad line widths. As the prominence material descends to the arcade, it turns into coronal rain sliding down coronal loops with line widths 2-3 times narrower. This contrast suggests that distinct local plasma and magnetic conditions determine the fate of the cool material, a scenario supported by our magnetic field extrapolations from SDO/HMI. Specifically, the supra-arcade fan (similar to those in solar flares) is likely situated in a current sheet, where the magnetic field is weak and the plasma-beta could be close to unity, thus favoring turbulent flows like those prominence threads. In contrast, the underlying arcade has a stronger magnetic field and most likely a low-beta environment, such that the material is guided along magnetic field lines to appear as coronal rain. We will discuss the physical implications of these observations beyond the phenomena of prominences and coronal rain. Title: LND for Chang'E 4 Mission Authors: Wimmer-Schweingruber, R. F.; Yu, J.; Hellweg, C.; Berger, T.; Zhang, S.; Burmeister, S.; Seimetz, L.; Schuster, B.; Boettcher, S. I.; Woyciechowski, H.; Guo, J.; Lohf, H.; Knierim, V. Bibcode: 2016AGUFMSM51A2465W Altcode: The Lunar Lander Neutrons & Dosimetry experiment (LND) is part of the payload of the next Chinese lunar mission, Chang'E 4, which is planned to land on the far side of the Moon. The University of Kiel in Germany is responsible for the design, development, and build of LND. This instrument will be accommodated on the Chang'E 4 Lander and has two major science objectives: dosimetry for human exploration of the Moon and contribution to heliospheric science. To achieve the first objective, LND is designed to determine the time series of dose rate and of linear energy transfer (LET) spectra in the complex radiation field of the lunar surface. For the second objective, LND is capable to measure the particle fluxes and their temporal variations, which can contribute to the understanding of particle propagation and transport in the heliosphere. With a stack of 10 silicon solid-state detectors, LND can measure fast neutrons in the energy rang from 2 - 20 MeV, protons from 10 - 30 MeV, electrons from 60 - 500 keV, alpha particles from 10 - 20 MeV/n and heavy ions from 15 - 40 MeV/n. Using two Gd-sandwich detectors, LND can in addition measure fluxes of thermal neutrons, which are sensitive to subsurface water and important to understand lunar surface mixing processes. Here we present the current development status of LND including the test results of the engineering model, together with plans for future activities. Title: Blending of Ground- and Space-Based Magnetograms: Application to L1-L5 Solar Wind and Coronal Hole Predictions Authors: Berger, T. E.; Pevtsov, A. A.; Martinez-Pillet, V.; Bertello, L.; Petrie, G. J. D.; Arge, C. N.; Henney, C. J.; Biesecker, D. A. Bibcode: 2016AGUFMSH11C2241B Altcode: We examine the effect of blending ground-based Global Oscillations Network Group (GONG) line-of-sight solar magnetic flux maps ("magnetograms") with space-based magnetograms from the Solar Dynamics Observatory (SDO) Helioseismic and Magnetic Imager (HMI) instrument on solar wind and coronal hole model-based forecasts. The longitudinally blended maps are used to "reforecast" solar wind conditions using the Wang-Sheeley-Arge (WSA) solar wind model during historical periods of coronal hole High Speed Streams (HSS) and Corotating Interaction Regions (CIRs) and compared to Advanced Composition Explorer (ACE) data at the L1 Lagrangian point. The same WSA runs are repeated using GONG and HMI data alone to determine the effect of data blending. The blended maps are also used to create Potential Field Source Surface (PFSS) maps of open coronal field lines and compared with historical coronal hole data from SDO Atmospheric Imaging Assembly (AIA) images. The study addresses the feasibility of combining ground- and space-based data from instruments with widely disparate and varying spatiotemporal resolution and flux sensitivity levels for use as inputs to solar wind and coronal hole forecasting models. The results are relevant to mission studies considering blended data inputs from, e.g., L5 Lagrangian point satellite instruments with ground-based measurements on the Sun-Earth line, as well as to expected magnetogram data from the Solar Orbiter Polarimetric and Helioseismic Imager (PHI) instrument. This study complements others that examine the utility of having multiple viewpoint (e.g. L1 and L5) magnetogram inputs to solar wind models by exploring data blending from disparate instruments. Title: DARWIN: towards the ultimate dark matter detector Authors: Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Amsler, C.; Aprile, E.; Arazi, L.; Arneodo, F.; Barrow, P.; Baudis, L.; Benabderrahmane, M. L.; Berger, T.; Beskers, B.; Breskin, A.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Calvén, J.; Cardoso, J. M. R.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; Diglio, S.; Drexlin, G.; Duchovni, E.; Erdal, E.; Eurin, G.; Ferella, A.; Fieguth, A.; Fulgione, W.; Gallo Rosso, A.; Di Gangi, P.; Di Giovanni, A.; Galloway, M.; Garbini, M.; Geis, C.; Glueck, F.; Grandi, L.; Greene, Z.; Grignon, C.; Hasterok, C.; Hannen, V.; Hogenbirk, E.; Howlett, J.; Hilk, D.; Hils, C.; James, A.; Kaminsky, B.; Kazama, S.; Kilminster, B.; Kish, A.; Krauss, L. M.; Landsman, H.; Lang, R. F.; Lin, Q.; Linde, F. L.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Mayani, D.; Messina, M.; Micheneau, K.; Molinario, A.; Morå, K. D.; Morteau, E.; Murra, M.; Naganoma, J.; Newstead, J. L.; Ni, K.; Oberlack, U.; Pakarha, P.; Pelssers, B.; de Perio, P.; Persiani, R.; Piastra, F.; Piro, M. C.; Plante, G.; Rauch, L.; Reichard, S.; Rizzo, A.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schumann, M.; Schreiner, J.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Silva, M. C.; Simgen, H.; Sissol, P.; von Sivers, M.; Thers, D.; Thurn, J.; Tiseni, A.; Trotta, R.; Tunnell, C. D.; Valerius, K.; Vargas, M. A.; Wang, H.; Wei, Y.; Weinheimer, C.; Wester, T.; Wulf, J.; Zhang, Y.; Zhu, T.; Zuber, K. Bibcode: 2016JCAP...11..017A Altcode: 2016arXiv160607001A DARk matter WImp search with liquid xenoN (DARWIN) will be an experiment for the direct detection of dark matter using a multi-ton liquid xenon time projection chamber at its core. Its primary goal will be to explore the experimentally accessible parameter space for Weakly Interacting Massive Particles (WIMPs) in a wide mass-range, until neutrino interactions with the target become an irreducible background. The prompt scintillation light and the charge signals induced by particle interactions in the xenon will be observed by VUV sensitive, ultra-low background photosensors. Besides its excellent sensitivity to WIMPs above a mass of 5 GeV/c2, such a detector with its large mass, low-energy threshold and ultra-low background level will also be sensitive to other rare interactions. It will search for solar axions, galactic axion-like particles and the neutrinoless double-beta decay of 136Xe, as well as measure the low-energy solar neutrino flux with < 1% precision, observe coherent neutrino-nucleus interactions, and detect galactic supernovae. We present the concept of the DARWIN detector and discuss its physics reach, the main sources of backgrounds and the ongoing detector design and R&D efforts. Title: Low-mass dark matter search using ionization signals in XENON100 Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arneodo, F.; Barrow, P.; Baudis, L.; Bauermeister, B.; Benabderrahmane, M. L.; Berger, T.; Breur, P. A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Buss, A.; Bütikofer, L.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; di Gangi, P.; di Giovanni, A.; Duchovni, E.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Galloway, M.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Gross, E.; Hasterok, C.; Hogenbirk, E.; Itay, R.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Levinson, L.; Le Calloch, M.; Levy, C.; Linde, F.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Lyashenko, A.; Manfredini, A.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Masson, D.; Mayani, D.; Melgarejo Fernandez, A. J.; Meng, Y.; Messina, M.; Micheneau, K.; Miguez, B.; Molinario, A.; Murra, M.; Naganoma, J.; Oberlack, U.; Orrigo, S. E. A.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; Dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Simgen, H.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C. D.; von Sivers, M.; Wall, R.; Wang, H.; Weber, M.; Wei, Y.; Weinheimer, C.; Wulf, J.; Zhang, Y.; Xenon Collaboration Bibcode: 2016PhRvD..94i2001A Altcode: 2016arXiv160506262X We perform a low-mass dark matter search using an exposure of 30 kg ×yr with the XENON100 detector. By dropping the requirement of a scintillation signal and using only the ionization signal to determine the interaction energy, we lowered the energy threshold for detection to 0.7 keV for nuclear recoils. No dark matter detection can be claimed because a complete background model cannot be constructed without a primary scintillation signal. Instead, we compute an upper limit on the WIMP-nucleon scattering cross section under the assumption that every event passing our selection criteria could be a signal event. Using an energy interval from 0.7 keV to 9.1 keV, we derive a limit on the spin-independent WIMP-nucleon cross section that excludes WIMPs with a mass of 6 GeV /c2 above 1.4 ×10-41 cm2 at 90% confidence level. Title: DOSIS & DOSIS 3D: long-term dose monitoring onboard the Columbus Laboratory of the International Space Station (ISS) Authors: Berger, Thomas; Przybyla, Bartos; Matthiä, Daniel; Reitz, Günther; Burmeister, Sönke; Labrenz, Johannes; Bilski, Pawel; Horwacik, Tomasz; Twardak, Anna; Hajek, Michael; Fugger, Manfred; Hofstätter, Christina; Sihver, Lembit; Palfalvi, Jozsef K.; Szabo, Julianna; Stradi, Andrea; Ambrozova, Iva; Kubancak, Jan; Brabcova, Katerina Pachnerova; Vanhavere, Filip; Cauwels, Vanessa; Van Hoey, Olivier; Schoonjans, Werner; Parisi, Alessio; Gaza, Ramona; Semones, Edward; Yukihara, Eduardo G.; Benton, Eric R.; Doull, Brandon A.; Uchihori, Yukio; Kodaira, Satoshi; Kitamura, Hisashi; Boehme, Matthias Bibcode: 2016JSWSC...6A..39B Altcode: The radiation environment encountered in space differs in nature from that on Earth, consisting mostly of highly energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on Earth for occupational radiation workers. Since the beginning of the space era, the radiation exposure during space missions has been monitored with various active and passive radiation instruments. Also onboard the International Space Station (ISS), a number of area monitoring devices provide data related to the spatial and temporal variation of the radiation field in and outside the ISS. The aim of the DOSIS (2009-2011) and the DOSIS 3D (2012-ongoing) experiments was and is to measure the radiation environment within the European Columbus Laboratory of the ISS. These measurements are, on the one hand, performed with passive radiation detectors mounted at 11 locations within Columbus for the determination of the spatial distribution of the radiation field parameters and, on the other, with two active radiation detectors mounted at a fixed position inside Columbus for the determination of the temporal variation of the radiation field parameters. Data measured with passive radiation detectors showed that the absorbed dose values inside the Columbus Laboratory follow a pattern, based on the local shielding configuration of the radiation detectors, with minimum dose values observed in the year 2010 of 195-270 μGy/day and maximum values observed in the year 2012 with values ranging from 260 to 360 μGy/day. The absorbed dose is modulated by (a) the variation in solar activity and (b) the changes in ISS altitude. Title: The RIMFAX GPR Instrument Development for the Mars 2020 Rover Mission Authors: Hamran, S. -E.; Amundsen, H. E. F.; Asak, L.; Berger, T.; Brovoll, S.; Buskenes, J. I.; Carter, L.; Damsgård, L.; Diaz, C.; Ghent, R.; Helleren, Ø.; Kohler, J.; Mellon, M.; Nunez, D.; Paige, D.; Plettemeier, D.; Rowe, K.; Russell, P.; Sagsveen, B.; Ødegaard, N.; Øyan, M. J. Bibcode: 2016LPICo1980.4031H Altcode: The Radar Imager for Mars' subsurface eXperiment (RIMFAX) ground penetrating radar (GPR) experiment for the Mars 2020 Rover will add a new dimension to the rover's toolset by providing the capability to image the shallow subsurface beneath the rover. Title: Joint SDO and IRIS Observations of a Novel, Hybrid Prominence-Coronal Rain Complex Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Gao, Lijia; Vial, Jean-Claude; Gibson, Sarah; Okamoto, Takenori; Berger, Thomas; Uitenbroek, Han; De Pontieu, Bart Bibcode: 2016usc..confE..99L Altcode: Solar prominences and coronal rain are intimately related phenomena, both involving cool material at chromospheric temperatures within the hot corona and both playing important roles as part of the return flow of the chromosphere-corona mass cycle. At the same time, they exhibit distinct morphologies and dynamics not yet well understood. Quiescent prominences consist of numerous long-lasting, filamentary downflow threads, while coronal rain is more transient and falls comparably faster along well-defined curved paths. We report here a novel, hybrid prominence-coronal rain complex in an arcade-fan geometry observed by SDO/AIA and IRIS, which provides new insights to the underlying physics of such contrasting behaviors. We found that the supra-arcade fan region hosts a prominence sheet consisting of meandering threads with broad line widths. As the prominence material descends to the arcade, it turns into coronal rain sliding down coronal loops with line widths 2-3 times narrower. This contrast suggests that distinct local plasma and magnetic conditions determine the fate of the cool material, a scenario supported by our magnetic field extrapolations from SDO/HMI. Specifically, the supra-arcade fan (similar to those in solar flares; e.g., McKenzie 2013) is likely situated in a current sheet, where the magnetic field is weak and the plasma-beta could be close to unity, thus favoring turbulent flows like those prominence threads. In contrast, the underlying arcade has a stronger magnetic field and most likely a low-beta environment, such that the material is guided along magnetic field lines to appear as coronal rain. We will discuss the physical implications of these observations beyond prominence and coronal rain. Title: Transitioning GONG data processing to NOAA SWPC operations Authors: Reinard, Alysha; Berger, Thomas; Marble, Andrew; Hill, Frank Bibcode: 2016shin.confE..26R Altcode: The NOAA Space Weather Prediction Center (SWPC) is the nation's official source of space weather watches, warnings, and alerts, providing 24x7 forecasting and support to critical infrastructure operators around the world. Observations of the conditions on the Sun are crucial for determining when and if a warning is needed. The Global Oscillation Network Group (GONG) operated by the National Solar Observatory (NSO) consists of six ground stations, allowing continuous observations of the Sun. Of particular interest for space weather purposes are the H-alpha images and magnetograms. H-alpha data is used to identify filaments and their eruptions, to assess active region evolution and plage extent, and to help localize flare locations. Magnetograms are used to identify neutral lines, examine potential shearing areas and characterize the magnetic structure of active regions. GONG magnetograms also provide the initial condition for models of solar wind expansion such as the WSA-Enlil model. GONG helioseismology products, in particular far-side imaging, are being examined for operational use in the near future.

NSO has operated GONG as a science facility since 1995 and has provided processed space weather data products to NOAA via public internet connections for the past several years. In 2014 the White House Office of Management and Budget (OMB) requested that NOAA transition the GONG network to an operational space weather asset in order to ensure the continued flow of critical magnetogram data for solar wind models. NSO will continue to operate and manage the instruments and sites, but the H-alpha images and 10 minute averaged magnetogram data will be sent directly to SWPC for processing and use in space weather modeling. SWPC will make these data available to NSO and the public via the new NOAA Integrated Dissemination Program (IDP) network. We discuss the progress and details of this change. Title: Towards Space Exploration of Moon, Mars Neos: Radiation Biological Basis Authors: Hellweg, Christine; Baumstark-Khan, Christa; Berger, Thomas; Reitz, Guenther Bibcode: 2016cosp...41E.825H Altcode: Radiation has emerged as the most critical issue to be resolved for long-term missions both orbital and interplanetary. Astronauts are constantly exposed to galactic cosmic radiation (GCR) of various energies with a low dose rate. Primarily late tissue sequels like genetic alterations, cancer and non-cancer effects, i.e. cataracts and degenerative diseases of e.g. the central nervous system or the cardiovascular system, are the potential risks. Cataracts were observed to occur earlier and more often in astronauts exposed to higher proportions of galactic ions (Cucinotta et al., 2001). Predictions of cancer risk and acceptable radiation exposure in space are subject to many uncertainties including the relative biological effectiveness (RBE) of space radiation especially heavy ions, dose-rate effects and possible interaction with microgravity and other spaceflight environmental factors. The initial cellular response to radiation exposure paves the way to late sequelae and starts with damage to the DNA which complexity depends on the linear energy transfer (LET) of the radiation. Repair of such complex DNA damage is more challenging and requires more time than the repair of simple DNA double strand breaks (DSB) which can be visualized by immunofluorescence staining of the phosphorylated histone 2AX (γH2AX) and might explain the observed prolonged cell cycle arrests induced by high-LET in comparison to low-LET irradiation. Unrepaired or mis-repaired DNA DSB are proposed to be responsible for cell death, mutations, chromosomal aberrations and oncogenic cell transformation. Cell killing and mutation induction are most efficient in an LET range of 90-200 keV/µm. Also the activation of transcription factors such as Nuclear Factor κB (NF-κB) and gene expression shaping the cellular radiation response depend on the LET with a peak RBE between 90 and 300 keV/µm. Such LET-RBE relationships were observed for cataract and cancer induction by heavy ions in laboratory animals, with varying maximal efficiencies. Furthermore, there is always the added risk of acute exposure to high proton fluxes during a solar particle event (SPE), which can threaten immediate survival of the astronauts in case of insufficient shielding by eliciting the acute radiation syndrome. Its symptoms depend on absorbed total radiation dose, type of radiation, the dose distribution in the body and the individual radiation sensitivity. After the prodromal stage with nausea and vomiting and a subsequent symptom-free phase, depending on dose, the hematopoietic syndrome with suppression of the acquired immune system and thrombocytopenia (0.7-4 Sv), the gastrointestinal tract syndrome (5-12 Sv) or the central nervous system syndrome (> 20 Sv) develop and they are accompanied by exacerbated innate immune responses. Exposure to large SPE has to be avoided by warning systems and stay inside a radiation shelter during the event. Treatment options encompass e.g. the administration of colony-stimulating factors (CSF), growth factors and blood transfusions to overcome the hematopoietic syndrome and the administration of antibiotics against secondary infections. A concerted action of ground-based studies and space experiments is required to improve the radiobiological basis of space radiation risk assessment and countermeasure development. References: Cucinotta FA, Manuel FK, Jones J, Iszard G, Murrey J, Djojonegro B and Wear M (2001) Space Radiation and Cataracts in Astronauts. Rad Res 156, 460-466 Title: Operational Space Weather Activities in the US Authors: Berger, Thomas; Singer, Howard; Onsager, Terrance; Viereck, Rodney; Murtagh, William; Rutledge, Robert Bibcode: 2016cosp...41E.180B Altcode: We review the current activities in the civil operational space weather forecasting enterprise of the United States. The NOAA/Space Weather Prediction Center is the nation's official source of space weather watches, warnings, and alerts, working with partners in the Air Force as well as international operational forecast services to provide predictions, data, and products on a large variety of space weather phenomena and impacts. In October 2015, the White House Office of Science and Technology Policy released the National Space Weather Strategy (NSWS) and associated Space Weather Action Plan (SWAP) that define how the nation will better forecast, mitigate, and respond to an extreme space weather event. The SWAP defines actions involving multiple federal agencies and mandates coordination and collaboration with academia, the private sector, and international bodies to, among other things, develop and sustain an operational space weather observing system; develop and deploy new models of space weather impacts to critical infrastructure systems; define new mechanisms for the transition of research models to operations and to ensure that the research community is supported for, and has access to, operational model upgrade paths; and to enhance fundamental understanding of space weather through support of research models and observations. The SWAP will guide significant aspects of space weather operational and research activities for the next decade, with opportunities to revisit the strategy in the coming years through the auspices of the National Science and Technology Council. Title: Data and Models Needed to Support Civil Aviation Authors: Onsager, Terrance; Biesecker, D. A.; Berger, Thomas; Rutledge, Robert Bibcode: 2016cosp...41E1469O Altcode: The effective utilization of existing data and models is an important element in advancing the goals of the COSPAR/ILWS space weather roadmap. This is recommended to be done through innovative approaches to data utilization, including data driving, data assimilation, and ensemble modeling. This presentation will focus on observations and models needed to support space weather services for civil aviation and commercial space transportation. The service needs for aviation will be discussed, and an overview will be given of some of the existing data and models that can provide these services. Efforts underway to define the requirements for real-time data and to assess current modeling capabilities will be described. Recommendations will be offered for internationally coordinated activities that could identify priorities and further the roadmap goals. Title: Experience Transitioning Models and Data at the NOAA Space Weather Prediction Center Authors: Berger, Thomas Bibcode: 2016cosp...41E.181B Altcode: The NOAA Space Weather Prediction Center has a long history of transitioning research data and models into operations and with the validation activities required. The first stage in this process involves demonstrating that the capability has sufficient value to customers to justify the cost needed to transition it and to run it continuously and reliably in operations. Once the overall value is demonstrated, a substantial effort is then required to develop the operational software from the research codes. The next stage is to implement and test the software and product generation on the operational computers. Finally, effort must be devoted to establishing long-term measures of performance, maintaining the software, and working with forecasters, customers, and researchers to improve over time the operational capabilities. This multi-stage process of identifying, transitioning, and improving operational space weather capabilities will be discussed using recent examples. Plans for future activities will also be described. Title: Transitioning GONG data processing to NOAA SWPC operations Authors: Reinard, Alysha; Marble, Andrew R.; Berger, Thomas Bibcode: 2016SPD....47.0205R Altcode: The NOAA Space Weather Prediction Center (SWPC) is the nation's official source of space weather watches, warnings, and alerts, providing 24x7 forecasting and support to critical infrastructure operators around the world. Observations of the conditions on the Sun are crucial for determining when and if a warning is needed. The Global Oscillation Network Group (GONG) operated by the National Solar Observatory (NSO) consists of six ground stations, allowing continuous observations of the Sun. Of particular interest for space weather purposes are the H-alpha images and magnetograms. The H-alpha data are used to identify filaments and their eruptions, to assess active region evolution and plage extent, and to help localize flare locations. The magnetograms are used to identify neutral lines, to examine potential shearing areas and to characterize the magnetic structure of active regions. GONG magnetograms also provide the initial condition for models of solar wind expansion through the heliosphere such as the WSA-Enlil model. Although beyond the scope of current space weather applications, GONG helioseismology products can be used to assess active region emergence on the far side of the Sun and to indicate the flaring potential of a front-side active region. These products are being examined as future tools in flare prediction.NSO has operated GONG as a science facility since 1995 and has provided processed space weather data products to NOAA via for the past several years. In 2014 the White House Office of Management and Budget (OMB) requested that NOAA transition the GONG network to an operational space weather asset in order to ensure the continued flow of critical data for solar wind models. NSO will continue to operate and manage the instruments and sites, but the H-alpha images and 10 minute averaged magnetogram data will be sent directly to SWPC for processing and use in space weather modeling. SWPC will make these data available to NSO and the public via the new NOAA Integrated Dissemination Program (IDP) network. We discuss the progress and details of this change. Title: Physics reach of the XENON1T dark matter experiment. Authors: Aprile, E.; Aalbers, J.; Agostini, F.; Alfonsi, M.; Amaro, F. D.; Anthony, M.; Arazi, L.; Arneodo, F.; Balan, C.; Barrow, P.; Baudis, L.; Bauermeister, B.; Berger, T.; Breur, P.; Breskin, A.; Brown, A.; Brown, E.; Bruenner, S.; Bruno, G.; Budnik, R.; Bütikofer, L.; Cardoso, J. M. R.; Cervantes, M.; Cichon, D.; Coderre, D.; Colijn, A. P.; Conrad, J.; Contreras, H.; Cussonneau, J. P.; Decowski, M. P.; de Perio, P.; Di Gangi, P.; Di Giovanni, A.; Duchovni, E.; Fattori, S.; Ferella, A. D.; Fieguth, A.; Franco, D.; Fulgione, W.; Galloway, M.; Garbini, M.; Geis, C.; Goetzke, L. W.; Greene, Z.; Grignon, C.; Gross, E.; Hampel, W.; Hasterok, C.; Itay, R.; Kaether, F.; Kaminsky, B.; Kessler, G.; Kish, A.; Landsman, H.; Lang, R. F.; Lellouch, D.; Levinson, L.; Le Calloch, M.; Levy, C.; Lindemann, S.; Lindner, M.; Lopes, J. A. M.; Lyashenko, A.; Macmullin, S.; Manfredini, A.; Marrodán Undagoitia, T.; Masbou, J.; Massoli, F. V.; Mayani, D.; Melgarejo Fernandez, A. J.; Meng, Y.; Messina, M.; Micheneau, K.; Miguez, B.; Molinario, A.; Murra, M.; Naganoma, J.; Oberlack, U.; Orrigo, S. E. A.; Pakarha, P.; Pelssers, B.; Persiani, R.; Piastra, F.; Pienaar, J.; Plante, G.; Priel, N.; Rauch, L.; Reichard, S.; Reuter, C.; Rizzo, A.; Rosendahl, S.; Rupp, N.; dos Santos, J. M. F.; Sartorelli, G.; Scheibelhut, M.; Schindler, S.; Schreiner, J.; Schumann, M.; Scotto Lavina, L.; Selvi, M.; Shagin, P.; Simgen, H.; Stein, A.; Thers, D.; Tiseni, A.; Trinchero, G.; Tunnell, C.; von Sivers, M.; Wall, R.; Wang, H.; Weber, M.; Wei, Y.; Weinheimer, C.; Wulf, J.; Zhang, Y. Bibcode: 2016JCAP...04..027A Altcode: 2015arXiv151207501T The XENON1T experiment is currently in the commissioning phase at the Laboratori Nazionali del Gran Sasso, Italy. In this article we study the experiment's expected sensitivity to the spin-independent WIMP-nucleon interaction cross section, based on Monte Carlo predictions of the electronic and nuclear recoil backgrounds.

The total electronic recoil background in 1 tonne fiducial volume and (1, 12) keV electronic recoil equivalent energy region, before applying any selection to discriminate between electronic and nuclear recoils, is (1.80 ± 0.15) · 10-4 (kg·day·keV)-1, mainly due to the decay of 222Rn daughters inside the xenon target. The nuclear recoil background in the corresponding nuclear recoil equivalent energy region (4, 50) keV, is composed of (0.6 ± 0.1) (t·y)-1 from radiogenic neutrons, (1.8 ± 0.3) · 10-2 (t·y)-1 from coherent scattering of neutrinos, and less than 0.01 (t·y)-1 from muon-induced neutrons. The sensitivity of XENON1T is calculated with the Profile Likelihood Ratio method, after converting the deposited energy of electronic and nuclear recoils into the scintillation and ionization signals seen in the detector. We take into account the systematic uncertainties on the photon and electron emission model, and on the estimation of the backgrounds, treated as nuisance parameters. The main contribution comes from the relative scintillation efficiency Script Leff, which affects both the signal from WIMPs and the nuclear recoil backgrounds. After a 2 y measurement in 1 t fiducial volume, the sensitivity reaches a minimum cross section of 1.6 · 10-47 cm2 at mχ = 50 GeV/c2. Title: The Martian surface radiation environment - a comparison of models and MSL/RAD measurements Authors: Matthiä, Daniel; Ehresmann, Bent; Lohf, Henning; Köhler, Jan; Zeitlin, Cary; Appel, Jan; Sato, Tatsuhiko; Slaba, Tony; Martin, Cesar; Berger, Thomas; Boehm, Eckart; Boettcher, Stephan; Brinza, David E.; Burmeister, Soenke; Guo, Jingnan; Hassler, Donald M.; Posner, Arik; Rafkin, Scot C. R.; Reitz, Günther; Wilson, John W.; Wimmer-Schweingruber, Robert F. Bibcode: 2016JSWSC...6A..13M Altcode: Context: The Radiation Assessment Detector (RAD) on the Mars Science Laboratory (MSL) has been measuring the radiation environment on the surface of Mars since August 6th 2012. MSL-RAD is the first instrument to provide detailed information about charged and neutral particle spectra and dose rates on the Martian surface, and one of the primary objectives of the RAD investigation is to help improve and validate current radiation transport models. Aims: Applying different numerical transport models with boundary conditions derived from the MSL-RAD environment the goal of this work was to both provide predictions for the particle spectra and the radiation exposure on the Martian surface complementing the RAD sensitive range and, at the same time, validate the results with the experimental data, where applicable. Such validated models can be used to predict dose rates for future manned missions as well as for performing shield optimization studies. Methods: Several particle transport models (GEANT4, PHITS, HZETRN/OLTARIS) were used to predict the particle flux and the corresponding radiation environment caused by galactic cosmic radiation on Mars. From the calculated particle spectra the dose rates on the surface are estimated. Results: Calculations of particle spectra and dose rates induced by galactic cosmic radiation on the Martian surface are presented. Although good agreement is found in many cases for the different transport codes, GEANT4, PHITS, and HZETRN/OLTARIS, some models still show large, sometimes order of magnitude discrepancies in certain particle spectra. We have found that RAD data is helping to make better choices of input parameters and physical models. Elements of these validated models can be applied to more detailed studies on how the radiation environment is influenced by solar modulation, Martian atmosphere and soil, and changes due to the Martian seasonal pressure cycle. By extending the range of the calculated particle spectra with respect to the experimental data additional information about the radiation environment is gained, and the contribution of different particle species to the dose is estimated. Title: Matroshka DOSTEL measurements onboard the International Space Station (ISS) Authors: Labrenz, Johannes; Burmeister, Soenke; Berger, Thomas; Heber, Bernd; Reitz, Guenther Bibcode: 2015JSWSC...5A..38L Altcode: This paper presents the absorbed dose and dose equivalent rate measurements achieved with the DOSimetry TElescope (DOSTEL) during the two Matroshka (MTR) experiment campaigns in 2004/2005 (MTR-1) and 2007/2008 (MTR-2B). The comparison between the inside (MTR-2B) and outside (MTR-1) mission has shown that the shielding thickness provided by the International Space Station (ISS) spacecraft hull has a minor effect on the radiation exposure caused by Galactic Cosmic Rays (GCR). The exposure varies with the solar modulation of the GCR, too. Particles from Earth's radiation belts are effectively shielded by the spacecraft hull, and thus the contribution to the radiation exposure is lower for the inside measurement during MTR-2B. While the MTR-DOSTEL absorbed dose rate shows a good agreement with passive detectors of the MTR experiment for the MTR-2B mission phase, the MTR-1 absorbed dose rates from MTR-DOSTEL measurements are much lower than those obtained by a nearby passive detector. Observed discrepancies between the MTR-DOSTEL measurements and the passive detectors located nearby could be explained by the additional exposure to an enhanced flux of electrons trapped between L-parameter 2.5 and 3.5 caused by solar storms in July 2004. Title: Transitioning GONG data processing to NOAA SWPC operations Authors: Reinard, A.; Marble, A.; Hill, F.; Berger, T. E. Bibcode: 2015AGUFMSH21B2394R Altcode: The NOAA Space Weather Prediction Center (SWPC) is the nation's official source of space weather watches, warnings, and alerts, providing 24x7 forecasting and support to critical infrastructure operators around the world. Observations of the conditions on the Sun are crucial for determining when and if a warning is needed. The Global Oscillation Network Group (GONG) operated by the National Solar Observatory (NSO) consists of six ground stations, allowing continuous observations of the Sun. Of particular interest for space weather purposes are the H-alpha images and magnetograms. The H-alpha data are used to identify filaments and their eruptions, to assess active region evolution and plage extent, and to help localize flare locations. The magnetograms are used to identify neutral lines, to examine potential shearing areas and to characterize the magnetic structure of active regions. GONG magnetograms also provide the initial condition for models of solar wind expansion through the heliosphere such as the WSA-Enlil model. Although beyond the scope of current space weather applications, GONG helioseismology products can be used to assess active region emergence on the far side of the Sun and to indicate the flaring potential of a front-side active region. These products are being examined as future tools in flare prediction. NSO has operated GONG as a science facility since 1995 and has provided processed space weather data products to NOAA via public internet connections for the past several years. In 2014 the White House Office of Management and Budget (OMB) requested that NOAA transition the GONG network to an operational space weather asset in order to ensure the continued flow of critical magnetogram data for solar wind models. NSO will continue to operate and manage the instruments and sites, but the H-alpha images and 10 minute averaged magnetogram data will be sent directly to SWPC for processing and use in space weather modeling. SWPC will make these data available to NSO and the public via the new NOAA Integrated Dissemination Program (IDP) network. We discuss the progress and details of this change. Title: Fifty Years of Space Weather Forecasting from Boulder Authors: Berger, T. E. Bibcode: 2015AGUFMSM13F..01B Altcode: The first official space weather forecast was issued by the Space Disturbances Laboratory in Boulder, Colorado, in 1965, ushering in an era of operational prediction that continues to this day. Today, the National Oceanic and Atmospheric Administration (NOAA) charters the Space Weather Prediction Center (SWPC) as one of the nine National Centers for Environmental Prediction (NCEP) to provide the nation's official watches, warnings, and alerts of space weather phenomena. SWPC is now integral to national and international efforts to predict space weather events, from the common and mild, to the rare and extreme, that can impact critical technological infrastructure. In 2012, the Strategic National Risk Assessment included extreme space weather events as low-to-medium probability phenomena that could, unlike any other meteorogical phenomena, have an impact on the government's ability to function. Recognizing this, the White House chartered the Office of Science and Technology Policy (OSTP) to produce the first comprehensive national strategy for the prediction, mitigation, and response to an extreme space weather event. The implementation of the National Strategy is ongoing with NOAA, its partners, and stakeholders concentrating on the goal of improving our ability to observe, model, and predict the onset and severity of space weather events. In addition, work continues with the research community to improve our understanding of the physical mechanisms - on the Sun, in the heliosphere, and in the Earth's magnetic field and upper atmosphere - of space weather as well as the effects on critical infrastructure such as electrical power transmission systems. In fifty years, people will hopefully look back at the history of operational space weather prediction and credit our efforts today with solidifying the necessary developments in observational systems, full-physics models of the entire Sun-Earth system, and tools for predicting the impacts to infrastructure to protect against any and all forms of space weather. Title: The Future of Operational Space Weather Observations Authors: Berger, T. E. Bibcode: 2015AGUFMSH12A..03B Altcode: We review the current state of operational space weather observations, the requirements for new or evolved space weather forecasting capablities, and the relevant sections of the new National strategy for space weather developed by the Space Weather Operations, Research, and Mitigation (SWORM) Task Force chartered by the Office of Science and Technology Policy of the White House. Based on this foundation, we discuss future space missions such as the NOAA space weather mission to the L1 Lagrangian point planned for the 2021 time frame and its synergy with an L5 mission planned for the same period; the space weather capabilities of the upcoming GOES-R mission, as well as GOES-Next possiblities; and the upcoming COSMIC-2 mission for ionospheric observations. We also discuss the needs for ground-based operational networks to supply mission critical and/or backup space weather observations including the NSF GONG solar optical observing network, the USAF SEON solar radio observing network, the USGS real-time magnetometer network, the USCG CORS network of GPS receivers, and the possibility of operationalizing the world-wide network of neutron monitors for real-time alerts of ground-level radiation events. Title: Space experiment "Cellular Responses to Radiation in Space (CELLRAD)": Hardware and biological system tests Authors: Hellweg, Christine E.; Dilruba, Shahana; Adrian, Astrid; Feles, Sebastian; Schmitz, Claudia; Berger, Thomas; Przybyla, Bartos; Briganti, Luca; Franz, Markus; Segerer, Jürgen; Spitta, Luis F.; Henschenmacher, Bernd; Konda, Bikash; Diegeler, Sebastian; Baumstark-Khan, Christa; Panitz, Corinna; Reitz, Günther Bibcode: 2015LSSR....7...73H Altcode: One factor contributing to the high uncertainty in radiation risk assessment for long-term space missions is the insufficient knowledge about possible interactions of radiation with other spaceflight environmental factors. Such factors, e.g. microgravity, have to be considered as possibly additive or even synergistic factors in cancerogenesis. Regarding the effects of microgravity on signal transduction, it cannot be excluded that microgravity alters the cellular response to cosmic radiation, which comprises a complex network of signaling pathways.

The purpose of the experiment ;Cellular Responses to Radiation in Space; (CELLRAD, formerly CERASP) is to study the effects of combined exposure to microgravity, radiation and general space flight conditions on mammalian cells, in particular Human Embryonic Kidney (HEK) cells that are stably transfected with different plasmids allowing monitoring of proliferation and the Nuclear Factor κB (NF-κB) pathway by means of fluorescent proteins.

The cells will be seeded on ground in multiwell plate units (MPUs), transported to the ISS, and irradiated by an artificial radiation source after an adaptation period at 0 × g and 1 × g. After different incubation periods, the cells will be fixed by pumping a formaldehyde solution into the MPUs. Ground control samples will be treated in the same way. For implementation of CELLRAD in the Biolab on the International Space Station (ISS), tests of the hardware and the biological systems were performed. The sequence of different steps in MPU fabrication (cutting, drilling, cleaning, growth surface coating, and sterilization) was optimized in order to reach full biocompatibility. Different coatings of the foil used as growth surface revealed that coating with 0.1 mg/ml poly-D-lysine supports cell attachment better than collagen type I. The tests of prototype hardware (Science Model) proved its full functionality for automated medium change, irradiation and fixation of cells. Exposure of HEK cells to the β-rays emitted by the radiation source dose-dependently decreased cell growth and increased NF-κB activation. The signal of the fluorescent proteins after formaldehyde fixation was stable for at least six months after fixation, allowing storage of the MPUs after fixation for several months before the transport back to Earth and evaluation of the fluorescence intensity. In conclusion, these tests show the feasibility of CELLRAD on the ISS with the currently available transport mechanisms. Title: First High-resolution Spectroscopic Observations of an Erupting Prominence Within a Coronal Mass Ejection by the Interface Region Imaging Spectrograph (IRIS) Authors: Liu, Wei; De Pontieu, Bart; Vial, Jean-Claude; Title, Alan M.; Carlsson, Mats; Uitenbroek, Han; Okamoto, Takenori J.; Berger, Thomas E.; Antolin, Patrick Bibcode: 2015ApJ...803...85L Altcode: 2015arXiv150204738L Spectroscopic observations of prominence eruptions associated with coronal mass ejections (CMEs), although relatively rare, can provide valuable plasma and three-dimensional geometry diagnostics. We report the first observations by the Interface Region Imaging Spectrograph mission of a spectacular fast CME/prominence eruption associated with an equivalent X1.6 flare on 2014 May 9. The maximum plane-of-sky and Doppler velocities of the eruption are 1200 and 460 km s-1, respectively. There are two eruption components separated by ∼200 km s-1 in Doppler velocity: a primary, bright component and a secondary, faint component, suggesting a hollow, rather than solid, cone-shaped distribution of material. The eruption involves a left-handed helical structure undergoing counterclockwise (viewed top-down) unwinding motion. There is a temporal evolution from upward eruption to downward fallback with less-than-free-fall speeds and decreasing nonthermal line widths. We find a wide range of Mg ii k/h line intensity ratios (less than ∼2 expected for optically-thin thermal emission): the lowest ever reported median value of 1.17 found in the fallback material, a comparably high value of 1.63 in nearby coronal rain, and intermediate values of 1.53 and 1.41 in the two eruption components. The fallback material exhibits a strong (\gt 5σ ) linear correlation between the k/h ratio and the Doppler velocity as well as the line intensity. We demonstrate that Doppler dimming of scattered chromospheric emission by the erupted material can potentially explain such characteristics. Title: Characteristics of Operational Space Weather Forecasting: Observations and Models Authors: Berger, Thomas; Viereck, Rodney; Singer, Howard; Onsager, Terry; Biesecker, Doug; Rutledge, Robert; Hill, Steven; Akmaev, Rashid; Milward, George; Fuller-Rowell, Tim Bibcode: 2015TESS....111204B Altcode: In contrast to research observations, models and ground support systems, operational systems are characterized by real-time data streams and run schedules, with redundant backup systems for most elements of the system. We review the characteristics of operational space weather forecasting, concentrating on the key aspects of ground- and space-based observations that feed models of the coupled Sun-Earth system at the NOAA/Space Weather Prediction Center (SWPC). Building on the infrastructure of the National Weather Service, SWPC is working toward a fully operational system based on the GOES weather satellite system (constant real-time operation with back-up satellites), the newly launched DSCOVR satellite at L1 (constant real-time data network with AFSCN backup), and operational models of the heliosphere, magnetosphere, and ionosphere/thermosphere/mesophere systems run on the Weather and Climate Operational Super-computing System (WCOSS), one of the worlds largest and fastest operational computer systems that will be upgraded to a dual 2.5 Pflop system in 2016. We review plans for further operational space weather observing platforms being developed in the context of the Space Weather Operations Research and Mitigation (SWORM) task force in the Office of Science and Technology Policy (OSTP) at the White House. We also review the current operational model developments at SWPC, concentrating on the differences between the research codes and the modified real-time versions that must run with zero fault tolerance on the WCOSS systems. Understanding the characteristics and needs of the operational forecasting community is key to producing research into the coupled Sun-Earth system with maximal societal benefit. Title: Constitutive expression of tdTomato protein as a cytotoxicity and proliferation marker for space radiation biology Authors: Chishti, Arif A.; Hellweg, Christine E.; Berger, Thomas; Baumstark-Khan, Christa; Feles, Sebastian; Kätzel, Thorben; Reitz, Günther Bibcode: 2015LSSR....4...35C Altcode: The radiation risk assessment for long-term space missions requires knowledge on the biological effectiveness of different space radiation components, e.g. heavy ions, on the interaction of radiation and other space environmental factors such as microgravity, and on the physical and biological dose distribution in the human body. Space experiments and ground-based experiments at heavy ion accelerators require fast and reliable test systems with an easy readout for different endpoints. In order to determine the effect of different radiation qualities on cellular proliferation and the biological depth dose distribution after heavy ion exposure, a stable human cell line expressing a novel fluorescent protein was established and characterized. tdTomato, a red fluorescent protein of the new generation with fast maturation and high fluorescence intensity, was selected as reporter of cell proliferation. Human embryonic kidney (HEK/293) cells were stably transfected with a plasmid encoding tdTomato under the control of the constitutively active cytomegalovirus (CMV) promoter (ptdTomato-N1). The stably transfected cell line was named HEK-ptdTomato-N1 8. This cytotoxicity biosensor was tested by ionizing radiation (X-rays and accelerated heavy ions) exposure. As biological endpoints, the proliferation kinetics and the cell density reached 100 h after irradiation reflected by constitutive expression of the tdTomato were investigated. Both were reduced dose-dependently after radiation exposure. Finally, the cell line was used for biological weighting of heavy ions of different linear energy transfer (LET) as space-relevant radiation quality. The relative biological effectiveness of accelerated heavy ions in reducing cellular proliferation peaked at an LET of 91 keV/μm. The results of this study demonstrate that the HEK-ptdTomato-N1 reporter cell line can be used as a fast and reliable biosensor system for detection of cytotoxic damage caused by ionizing radiation. Title: Photochemical studies in low Earth orbit for organic compounds related to small bodies, Titan and Mars. Current and future facilities. Authors: Cottin, H.; Saiagh, K.; Nguyen, D.; Grand, N.; Bénilan, Y.; Cloix, M.; Coll, P.; Gazaux, M. -C.; Fray, N.; Khalaf, D.; Raulin, F.; Stalort, F.; Carrasco, N.; Szopa, C.; Chaput, D.; Bertrand, M.; Westall, F.; Mattioda, A.; Quinn, R.; Ricco, A.; Santos, O.; Baratta, G. A.; Strazzulla, G.; Palumbo, M. E.; Le Postollec, A.; Dobrijevic, M.; Coussot, G.; Vigier, F.; Vandenabeele-Trambouze, O.; Incerti, S.; Berger, T. Bibcode: 2015BSRSL..84...60C Altcode: The study of the evolution of organic matter subjected to space conditions, and more specifically to solar photons in the vacuum ultraviolet range (120-200 nm) has been undertaken in low Earth Orbit since the 90's, and implemented on various space platforms. The most recent exposure facilities are BIOPAN outside the Russian automatic capsules FOTON, and EXPOSE-E & -R (1&2) outside the International Space Station. They allow the photolysis of many different samples simultaneously, and provide us with valuable data about the formation and evolution of organic matter in the Solar System (meteorites, comets, Titan's atmosphere, the Martian surface...) and in the Interstellar Medium. They have been used by European teams in the recent past(ORGANIC on BIOPAN V-FOTON M2 and UVolution on BIOPAN VI-FOTON M3, PROCESS on EXPOSE-E, AMINO and ORGANICS on EXPOSE-R), and a new EXPOSE set is currently exposed outside the ISS (PSS on EXPOSE-R2). These existing tools are very valuable; however, they have significant limitations that limit their capabilities and scientific return. One of the most critical issues for current studies is the lack of any in-situ analysis of the evolution of the samples as a function of time. Only two measurements are available for the experiment: one before and one after the exposure. A significant step forward has been achieved with the O/OREOS NASA nanosatellite and the OREOcube ESA project with onboard UV-visible measurements. However, for organic samples, following the evolution of the samples would be more informative and provide greater insight with infrared measurements, which display specific patterns characteristic of major organic functionalities in the mid-infrared range (4000-1000 cm-1). Title: GRB 150212A: Skynet DSO14/GORT observations. Authors: Trotter, A.; Reichart, D.; Lacluyze, A.; Haislip, J.; Smith, A.; Caton, D.; Hawkins, L.; McLin, K.; Cominsky, L.; Aji, A.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Crain, J. A. Bibcode: 2015GCN.17458....1T Altcode: 2015GCN..17458...1T No abstract at ADS Title: GRB 150314A: Skynet Yerkes-41 Observations of the Optical Afterglow. Authors: Trotter, A.; Reichart, D.; Lacluyze, A.; Haislip, J.; Hoette, V.; Cudworth, K.; Harper, D.; Kron, R.; Linder, T.; Russell, R.; Struble, E.; Aji, A.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Crain, J. A. Bibcode: 2015GCN.17577....1T Altcode: 2015GCN..17577...1T No abstract at ADS Title: Mars methane detection and variability at Gale crater Authors: Webster, Christopher R.; Mahaffy, Paul R.; Atreya, Sushil K.; Flesch, Gregory J.; Mischna, Michael A.; Meslin, Pierre-Yves; Farley, Kenneth A.; Conrad, Pamela G.; Christensen, Lance E.; Pavlov, Alexander A.; Martín-Torres, Javier; Zorzano, María-Paz; McConnochie, Timothy H.; Owen, Tobias; Eigenbrode, Jennifer L.; Glavin, Daniel P.; Steele, Andrew; Malespin, Charles A.; Archer, P. Douglas; Sutter, Brad; Coll, Patrice; Freissinet, Caroline; McKay, Christopher P.; Moores, John E.; Schwenzer, Susanne P.; Bridges, John C.; Navarro-Gonzalez, Rafael; Gellert, Ralf; Lemmon, Mark T.; MSL Science Team; Abbey, William; Achilles, Cherie; Agard, Christophe; Alexandre Alves Verdasca, José; Anderson, Dana; Anderson, Robert C.; Anderson, Ryan B.; Appel, Jan Kristoffer; Archer, Paul Douglas; Arevalo, Ricardo; Armiens-Aparicio, Carlos; Arvidson, Raymond; Atlaskin, Evgeny; Atreya, Andrew Sushil; Azeez, Aubrey Sherif; Baker, Burt; Baker, Michael; Balic-Zunic, Tonci; Baratoux, David; Baroukh, Julien; Barraclough, Bruce; Battalio, Michael; Beach, Michael; Bean, Keri; Beck, Pierre; Becker, Richard; Beegle, Luther; Behar, Alberto; Belgacem, Inès; Bell, James F., III; Bender, Steven; Benna, Mehdi; Bentz, Jennifer; Berger, Jeffrey; Berger, Thomas; Berlanga, Genesis; Berman, Daniel; Bish, David; Blacksberg, Jordana; Blake, David F.; José Blanco, Juan; Blaney, Ávalos Diana; Blank, Jennifer; Blau, Hannah; Bleacher, Lora; Boehm, Eckart; Bonnet, Jean-Yves; Botta, Oliver; Böttcher, Stephan; Boucher, Thomas; Bower, Hannah; Boyd, Nick; Boynton, William; Braswell, Shaneen; Breves, Elly; Bridges, John C.; Bridges, Nathan; Brinckerhoff, William; Brinza, David; Bristow, Thomas; Brunet, Claude; Brunner, Anna; Brunner, Will; Buch, Arnaud; Bullock, Mark; Burmeister, Sönke; Burton, John; Buz, Jennifer; Cabane, Michel; Calef, Fred; Cameron, James; Campbell, John L.; Cantor, Bruce; Caplinger, Michael; Clifton, Carey, Jr.; Caride Rodríguez, Javier; Carmosino, Marco; Carrasco Blázquez, Isaías; Cavanagh, Patrick; Charpentier, Antoine; Chipera, Steve; Choi, David; Christensen, Lance; Clark, Benton; Clegg, Sam; Cleghorn, Timothy; Cloutis, Ed; Cody, George; Coll, Patrice; Coman, Ecaterina I.; Conrad, Pamela; Coscia, David; Cousin, Agnès; Cremers, David; Crisp, Joy A.; Cropper, Kevin; Cros, Alain; Cucinotta, Francis; d'Uston, Claude; Davis, Scott; Day, Mackenzie; Daydou, Yves; DeFlores, Lauren; Dehouck, Erwin; Delapp, Dorothea; DeMarines, Julia; Dequaire, Tristan; Des Marais, David; Desrousseaux, Roch; Dietrich, William; Dingler, Robert; Domagal-Goldman, Shawn; Donny, Christophe; Downs, Robert; Drake, Darrell; Dromart, Gilles; Dupont, Audrey; Duston, Brian; Dworkin, Jason P.; Dyar, M. Darby; Edgar, Lauren; Edgett, Kenneth; Edwards, Christopher S.; Edwards, Laurence; Edwards, Peter; Ehlmann, Bethany; Ehresmann, Bent; Eigenbrode, Jennifer; Elliott, Beverley; Elliott, Harvey; Ewing, Ryan; Fabre, Cécile; Fairén, Alberto; Fairén, Alberto; Farley, Kenneth; Farmer, Jack; Fassett, Caleb; Favot, Laurent; Fay, Donald; Fedosov, Fedor; Feldman, Jason; Fendrich, Kim; Fischer, Erik; Fisk, Martin; Fitzgibbon, Mike; Flesch, Gregory; Floyd, Melissa; Flückiger, Lorenzo; Forni, Olivier; Fox, Valerie; Fraeman, Abigail; Francis, Raymond; François, Pascaline; Franz, Heather; Freissinet, Caroline; French, Katherine Louise; Frydenvang, Jens; Garvin, James; Gasnault, Olivier; Geffroy, Claude; Gellert, Ralf; Genzer, Maria; Getty, Stephanie; Glavin, Daniel; Godber, Austin; Goesmann, Fred; Goetz, Walter; Golovin, Dmitry; Gómez Gómez, Felipe; Gómez-Elvira, Javier; Gondet, Brigitte; Gordon, Suzanne; Gorevan, Stephen; Graham, Heather; Grant, John; Grinspoon, David; Grotzinger, John; Guillemot, Philippe; Guo, Jingnan; Gupta, Sanjeev; Guzewich, Scott; Haberle, Robert; Halleaux, Douglas; Hallet, Bernard; Hamilton, Victoria; Hand, Kevin; Hardgrove, Craig; Hardy, Keian; Harker, David; Harpold, Daniel; Harri, Ari-Matti; Harshman, Karl; Hassler, Donald; Haukka, Harri; Hayes, Alexander; Herkenhoff, Kenneth; Herrera, Paul; Hettrich, Sebastian; Heydari, Ezat; Hipkin, Victoria; Hoehler, Tori; Hollingsworth, Jeff; Hudgins, Judy; Huntress, Wesley; Hurowitz, Joel; Hviid, Stubbe; Iagnemma, Karl; Indyk, Stephen; Israël, Guy; Jackson, Ryan Steele; Jacob, Samantha; Jakosky, Bruce; Jean-Rigaud, Laurent; Jensen, Elsa; Kløvgaard Jensen, Jaqueline; Johnson, Jeffrey R.; Johnson, Micah; Johnstone, Stephen; Jones, Andrea; Jones, John H.; Joseph, Jonathan; Joulin, Mélissa; Jun, Insoo; Kah, Linda C.; Kahanpää, Henrik; Kahre, Melinda; Kaplan, Hannah; Karpushkina, Natalya; Kashyap, Srishti; Kauhanen, Janne; Keely, Leslie; Kelley, Simon; Kempe, Fabian; Kemppinen, Osku; Kennedy, Megan R.; Keymeulen, Didier; Kharytonov, Alexander; Kim, Myung-Hee; Kinch, Kjartan; King, Penelope; Kirk, Randolph; Kirkland, Laurel; Kloos, Jacob; Kocurek, Gary; Koefoed, Asmus; Köhler, Jan; Kortmann, Onno; Kotrc, Benjamin; Kozyrev, Alexander; Krau, Johannes; Krezoski, ß. Gillian; Kronyak, Rachel; Krysak, Daniel; Kuzmin, Ruslan; Lacour, Jean-Luc; Lafaille, Vivian; Langevin, Yves; Lanza, Nina; Lapôtre, Mathieu; Larif, Marie-France; Lasue, Jérémie; Le Deit, Laetitia; Le Mouélic, Stéphane; Lee, Ella Mae; Lee, Qiu-Mei; Lee, Rebekka; Lees, David; Lefavor, Matthew; Lemmon, Mark; Lepinette, Alain; Lepore, Malvitte Kate; Leshin, Laurie; Léveillé, Richard; Lewin, Éric; Lewis, Kevin; Li, Shuai; Lichtenberg, Kimberly; Lipkaman, Leslie; Lisov, Denis; Little, Cynthia; Litvak, Maxim; Liu, Lu; Lohf, Henning; Lorigny, Eric; Lugmair, Günter; Lundberg, Angela; Lyness, Eric; Madsen, Morten Bo; Magee, Angela; Mahaffy, Paul; Maki, Justin; Mäkinen, Teemu; Malakhov, Alexey; Malespin, Charles; Malin, Michael; Mangold, Nicolas; Manhes, Gerard; Manning, Heidi; Marchand, Geneviève; Marín Jiménez, Mercedes; Martín García, César; Martin, David K.; Martin, Mildred; Martin, Peter; Martínez Martínez, Germán; Martínez-Frías, Jesús; Martín-Sauceda, Jaime; Martín-Soler, Martín Javier; Martín-Torres, F. Javier; Mason, Emily; Matthews, Tristan; Matthiä, Daniel; Mauchien, Patrick; Maurice, Sylvestre; McAdam, Amy; McBride, Marie; McCartney, Elaina; McConnochie, Timothy; McCullough, Emily; McEwan, Ian; McKay, Christopher; McLain, Hannah; McLennan, Scott; McNair, Sean; Melikechi, Noureddine; Mendaza de Cal, Teresa; Merikallio, Sini; Merritt, Sean; Meslin, Pierre-Yves; Meyer, Michael; Mezzacappa, Alissa; Milkovich, Sarah; Millan, Maëva; Miller, Hayden; Miller, Kristen; Milliken, Ralph; Ming, Douglas; Minitti, Michelle; Mischna, Michael; Mitchell, Julie; Mitrofanov, Igor; Moersch, Jeffrey; Mokrousov, Maxim; Molina, Antonio; Moore, Jurado Casey; Moores, John E.; Mora-Sotomayor, Luis; Moreno, Gines; Morookian, John Michael; Morris, Richard V.; Morrison, Shaunna; Mousset, Valérie; Mrigakshi, Alankrita; Mueller-Mellin, Reinhold; Muller, Jan-Peter; Muñoz Caro, Guillermo; Nachon, Marion; Nastan, Abbey; Navarro López, Sara; Navarro González, Rafael; Nealson, Kenneth; Nefian, Ara; Nelson, Tony; Newcombe, Megan; Newman, Claire; Newsom, Horton; Nikiforov, Sergey; Nikitczuk, Matthew; Niles, Paul; Nixon, Brian; Noblet, Audrey; Noe, Eldar; Nolan, Dobrea Thomas; Oehler, Dorothy; Ollila, Ann; Olson, Timothy; Orthen, Tobias; Owen, Tobias; Ozanne, Marie; de Pablo Hernández, Miguel Ángel; Pagel, Hannah; Paillet, Alexis; Pallier, Etienne; Palucis, Marisa; Parker, Timothy; Parot, Yann; Parra, Alex; Patel, Kiran; Paton, Mark; Paulsen, Gale; Pavlov, Alexander; Pavri, Betina; Peinado-González, Verónica; Pepin, Robert; Peret, Laurent; Pérez, René; Perrett, Glynis; Peterson, Joseph; Pilorget, Cedric; Pinet, Patrick; Pinnick, Veronica; Pla-García, Jorge; Plante, Ianik; Poitrasson, Franck; Polkko, Jouni; Popa, Radu; Posiolova, Liliya; Posner, Arik; Pradler, Irina; Prats, Benito; Prokhorov, Vasily; Raaen, Eric; Radziemski, Leon; Rafkin, Scot; Ramos, Miguel; Rampe, Elizabeth; Rapin, William; Raulin, François; Ravine, Michael; Reitz, Günther; Ren, Jun; Rennó, Nilton; Rice, Melissa; Richardson, Mark; Ritter, Birgit; Rivera-Hernández, Frances; Robert, François; Robertson, Kevin; Rodriguez Manfredi, José Antonio; José Romeral-Planelló, Julio; Rowland, Scott; Rubin, David; Saccoccio, Muriel; Said, David; Salamon, Andrew; Sanin, Anton; Sans Fuentes, Sara Alejandra; Saper, Lee; Sarrazin, Philippe; Sautter, Violaine; Savijärvi, Hannu; Schieber, Juergen; Schmidt, Mariek; Schmidt, Walter; Scholes, Daniel; Schoppers, Marcel; Schröder, Susanne; Schwenzer, Susanne P.; Sciascia Borlina, Cauê; Scodary, Anthony; Sebastián Martínez, Eduardo; Sengstacken, Aaron; Shechet, Jennifer Griffes; Shterts, Ruslan; Siebach, Kirsten; Siili, Tero; Simmonds, John J.; Sirven, Jean-Baptiste; Slavney, Susan; Sletten, Ronald; Smith, Michael D.; Sobron Sanchez, Pablo; Spanovich, Nicole; Spray, John; Spring, Justin; Squyres, Steven; Stack, Katie; Stalport, Fabien; Starr, Richard; Stein, Andrew Steele Thomas; Stern, Jennifer; Stewart, Noel; Stewart, Wayne; Stipp, Svane Susan Louise; Stoiber, Kevin; Stolper, Edward; Sucharski, Robert; Sullivan, Robert; Summons, Roger; Sumner, Dawn Y.; Sun, Vivian; Supulver, Kimberley; Sutter, Brad; Szopa, Cyril; Tan, Florence; Tate, Christopher; Teinturier, Samuel; ten Kate, Inge Loes; Thomas, Alicia; Thomas, Peter; Thompson, Lucy; Thuillier, Franck; Thulliez, Emmanual; Tokar, Robert; Toplis, Michael; de la Torre Juárez, Manuel; Torres Redondo, Josefina; Trainer, Melissa; Treiman, Allan; Tretyakov, Vladislav; Ullán-Nieto, Aurora; Urqui-O'Callaghan, Roser; Valentín-Serrano, Patricia; Van Beek, Jason; Van Beek, Tessa; VanBommel, Scott; Vaniman, David; Varenikov, Alexey; Vasavada, Ashwin R.; Vasconcelos, Paulo; de Vicente-Retortillo Rubalcaba, Álvaro; Vicenzi, Edward; Vostrukhin, Andrey; Voytek, Mary; Wadhwa, Meenakshi; Ward, Jennifer; Watkins, Jessica; Webster, Christopher R.; Weigle, Gerald; Wellington, Danika; Westall, Frances; Wiens, Roger; Wilhelm, Mary Beth; Williams, Amy; Williams, Joshua; Williams, Rebecca; Williams, Richard B.; Williford, Kenneth; Wilson, Michael A.; Wilson, Sharon A.; Wimmer-Schweingruber, Robert; Wolff, Michael; Wong, Michael; Wray, James; Yana, Charles; Yen, Albert; Yingst, Aileen; Zeitlin, Cary; Zimdar, Robert; Zorzano Mier, María-Paz Bibcode: 2015Sci...347..415W Altcode: Reports of plumes or patches of methane in the martian atmosphere that vary over monthly time scales have defied explanation to date. From in situ measurements made over a 20-month period by the tunable laser spectrometer of the Sample Analysis at Mars instrument suite on Curiosity at Gale crater, we report detection of background levels of atmospheric methane of mean value 0.69 ± 0.25 parts per billion by volume (ppbv) at the 95% confidence interval (CI). This abundance is lower than model estimates of ultraviolet degradation of accreted interplanetary dust particles or carbonaceous chondrite material. Additionally, in four sequential measurements spanning a 60-sol period (where 1 sol is a martian day), we observed elevated levels of methane of 7.2 ± 2.1 ppbv (95% CI), implying that Mars is episodically producing methane from an additional unknown source. Title: GRB 150318A: Skynet PROMPT-CTIO Observations. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2015GCN.17605....1T Altcode: 2015GCN..17605...1T No abstract at ADS Title: Cosmic radiation exposure of biological test systems during the EXPOSE-R mission Authors: Berger, Thomas; Hajek, Michael; Bilski, Pawel Bibcode: 2015IJAsB..14...27B Altcode: In the frame of the EXPOSE-R mission outside the Russian Zvezda Module of the International Space Station (ISS) passive thermoluminescence dosimeters were applied to measure the radiation exposure of biological samples. The detectors were located beneath the sample carriers to determine the dose levels for maximum shielding. The dose measured beneath the sample carriers varied between 317 +/- 10 and 230 +/- 2 mGy, which amount to an average dose rate of 381 +/- 12 and 276 +/- 2 μGy d-1. These values are close to those assessed for the interior of the ISS and reflect the high shielding of the biological experiments within the EXPOSE-R facility. As a consequence of the high shielding (several g cm-2), the biological samples were predominantly exposed to galactic cosmic heavy ions and trapped protons in the Earth's radiation belts, whereas the trapped electrons did not reach the samples. Title: Estimating the temporal cutoff-rigidity variations and their implication on manned space missions Authors: Herbst, K.; Labrenz, J.; Kopp, A.; Heber, B.; Burmeister, S.; Berger, T. Bibcode: 2014AGUFMSM31A4156H Altcode: Using the PLANETOCOSMICS code the vertical cutoff rigidity or equivalently the minimum energy a particle must have in order to reach a given location on Earth is calculated. The program allows investigations that depend on the Earth's magnetic field strength and geometry as a function of time. Today it is well known that the magnetic field is the subject of temporal variations on long as well as short time-scales which reflects itself, e.g., in the global vertical cutoff-rigidity distribution at 20 km altitude (see Herbst et al., 2013). Focusing on the changes during the era of manned space missions (1961-2014) we extend our analysis of the vertical cutoff rigidity variations to about 450 km i.e. to the International Space Station (ISS) orbit. The outcome of this analysis will be compared to measurements of the DOSimetry TELescope (DOSTEL), an instrument that has been operational for several time periods onboard the ISS, allowing to determine the response function of the instrument. Using the Force-Field parameter derived from neutron monitors (see Usoskin et al., 2011) we will present maps of DOSTEL measurements for more than 50 years that are caused by galactic cosmic ray variations along hypothetical ISS orbits. Title: First High-resolution Spectroscopic Observations by IRIS of a Fast, Helical Prominence Eruption Associated with a Coronal Mass Ejection Authors: Liu, W.; De Pontieu, B.; Okamoto, T. J.; Vial, J. C.; Title, A. M.; Antolin, P.; Berger, T. E.; Uitenbroek, H. Bibcode: 2014AGUFMSH11D..04L Altcode: High-resolution spectroscopic observations of prominence eruptions and associated coronal mass ejections (CMEs) are rare but can provide valuable plasma and energy diagnostics. New opportunities have recently become available with the advent of the Interface Region Imaging Spectrograph (IRIS) mission equipped with high resolution of 0.33-0.4 arcsec in space and 1 km/s in velocity, together with the Hinode Solar Optical Telescope of 0.2 arcsec spatial resolution. We report the first result of joint IRIS-Hinode observations of a spectacular prominence eruption occurring on 2014-May-09. IRIS detected a maximum redshift of 450 km/s, which, combined with the plane-of-sky speed of 800 km/s, gives a large velocity vector of 920 km/s at 30 degrees from the sky plane. This direction agrees with the source location at 30 degrees behind the limb observed by STEREO-A and indicates a nearly vertical ejection. We found two branches of redshifts separated by 200 km/s appearing in all strong lines at chromospheric to transition-region temperatures, including Mg II k/h, C II, and Si IV, suggesting a hollow, rather than solid, cone in the velocity space of the ejected material. Opposite blue- and redshifts on the two sides of the prominence exhibit corkscrew variations both in space and time, suggestive of unwinding rotations of a left-handed helical flux rope. Some erupted material returns as nearly streamline flows, exhibiting distinctly narrow line widths (~10 km/s), about 50% of those of the nearby coronal rain at the apexes of coronal loops, where the rain material is initially formed out of cooling condensation. We estimate the mass and kinetic energy of the ejected and returning material and compare them with those of the associated CME. We will discuss the implications of these observations for CME initiation mechanisms. Title: The Daniel K. Inouye Solar Telescope: A Project Update. Authors: Rimmele, T.; Berger, T.; McMullin, J.; Warner, M.; Casinsi, R.; Kuhn, J.; Lin, H.; Woeger, F.; Schmidt, W.; Tritschler, A.; Inouye, Daniel K.; Solar Telescope Team Bibcode: 2014amos.confE..43R Altcode: The Advanced Technology Solar Telescope will be the largest solar facility ever built. Designed and developed to meet the needs of critical high resolution and high sensitivity spectral and polarimetric observations of the sun, this facility will support key experiments for the study of solar magnetism and its influence on the solar wind, flares, coronal mass ejections and solar irradiance variability. The 4-meter diameter facility will operate over a broad wavelength range (0.35 to 28 microns), using state-of-the-art adaptive optics systems to provide diffraction limited imaging and the ability to resolve features approximately 20 km on the Sun. Five first light instruments will be available at the start of operations. Key subsystems have been designed and fabrication is well underway, including the site construction, which began in December 2012. We provide an update on the development of the facilities both on site at the Haleakala Observatories in Maui and the development of components around the world. We present the overall construction and integration schedule leading to the start of operations in mid-2019 and touch on operations aspects. Title: Construction status of the Daniel K. Inouye Solar Telescope Authors: McMullin, Joseph P.; Rimmele, Thomas R.; Martínez Pillet, Valentin; Berger, Thomas E.; Casini, Roberto; Craig, Simon C.; Elmore, David F.; Goodrich, Bret D.; Hegwer, Steve L.; Hubbard, Robert P.; Johansson, Erik M.; Kuhn, Jeffrey R.; Lin, Haosheng; McVeigh, William; Schmidt, Wolfgang; Shimko, Steve; Tritschler, Alexandra; Warner, Mark; Wöger, Friedrich Bibcode: 2014SPIE.9145E..25M Altcode: The Daniel K. Inouye Solar Telescope (DKIST, renamed in December 2013 from the Advanced Technology Solar Telescope) will be the largest solar facility built when it begins operations in 2019. Designed and developed to meet the needs of critical high resolution and high sensitivity spectral and polarimetric observations of the Sun, the observatory will enable key research for the study of solar magnetism and its influence on the solar wind, flares, coronal mass ejections and solar irradiance variations. The 4-meter class facility will operate over a broad wavelength range (0.38 to 28 microns, initially 0.38 to 5 microns), using a state-of-the-art adaptive optics system to provide diffraction-limited imaging and the ability to resolve features approximately 25 km on the Sun. Five first-light instruments will be available at the start of operations: Visible Broadband Imager (VBI; National Solar Observatory), Visible SpectroPolarimeter (ViSP; NCAR High Altitude Observatory), Visible Tunable Filter (VTF; Kiepenheuer Institut für Sonnenphysik), Diffraction Limited Near InfraRed SpectroPolarimeter (DL-NIRSP; University of Hawai'i, Institute for Astronomy) and the Cryogenic Near InfraRed SpectroPolarimeter (Cryo-NIRSP; University of Hawai'i, Institute for Astronomy). As of mid-2014, the key subsystems have been designed and fabrication is well underway, including the site construction, which began in December 2012. We provide an update on the development of the facilities both on site at the Haleakalā Observatories on Maui and the development of components around the world. We present the overall construction and integration schedule leading to the handover to operations in mid 2019. In addition, we outline the evolving challenges being met by the project, spanning the full spectrum of issues covering technical, fiscal, and geographical, that are specific to this project, though with clear counterparts to other large astronomical construction projects. Title: The Interface Region Imaging Spectrograph (IRIS) Authors: De Pontieu, B.; Title, A. M.; Lemen, J. R.; Kushner, G. D.; Akin, D. J.; Allard, B.; Berger, T.; Boerner, P.; Cheung, M.; Chou, C.; Drake, J. F.; Duncan, D. W.; Freeland, S.; Heyman, G. F.; Hoffman, C.; Hurlburt, N. E.; Lindgren, R. W.; Mathur, D.; Rehse, R.; Sabolish, D.; Seguin, R.; Schrijver, C. J.; Tarbell, T. D.; Wülser, J. -P.; Wolfson, C. J.; Yanari, C.; Mudge, J.; Nguyen-Phuc, N.; Timmons, R.; van Bezooijen, R.; Weingrod, I.; Brookner, R.; Butcher, G.; Dougherty, B.; Eder, J.; Knagenhjelm, V.; Larsen, S.; Mansir, D.; Phan, L.; Boyle, P.; Cheimets, P. N.; DeLuca, E. E.; Golub, L.; Gates, R.; Hertz, E.; McKillop, S.; Park, S.; Perry, T.; Podgorski, W. A.; Reeves, K.; Saar, S.; Testa, P.; Tian, H.; Weber, M.; Dunn, C.; Eccles, S.; Jaeggli, S. A.; Kankelborg, C. C.; Mashburn, K.; Pust, N.; Springer, L.; Carvalho, R.; Kleint, L.; Marmie, J.; Mazmanian, E.; Pereira, T. M. D.; Sawyer, S.; Strong, J.; Worden, S. P.; Carlsson, M.; Hansteen, V. H.; Leenaarts, J.; Wiesmann, M.; Aloise, J.; Chu, K. -C.; Bush, R. I.; Scherrer, P. H.; Brekke, P.; Martinez-Sykora, J.; Lites, B. W.; McIntosh, S. W.; Uitenbroek, H.; Okamoto, T. J.; Gummin, M. A.; Auker, G.; Jerram, P.; Pool, P.; Waltham, N. Bibcode: 2014SoPh..289.2733D Altcode: 2014arXiv1401.2491D; 2014SoPh..tmp...25D The Interface Region Imaging Spectrograph (IRIS) small explorer spacecraft provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33 - 0.4 arcsec spatial resolution, two-second temporal resolution, and 1 km s−1 velocity resolution over a field-of-view of up to 175 arcsec × 175 arcsec. IRIS was launched into a Sun-synchronous orbit on 27 June 2013 using a Pegasus-XL rocket and consists of a 19-cm UV telescope that feeds a slit-based dual-bandpass imaging spectrograph. IRIS obtains spectra in passbands from 1332 - 1358 Å, 1389 - 1407 Å, and 2783 - 2834 Å, including bright spectral lines formed in the chromosphere (Mg II h 2803 Å and Mg II k 2796 Å) and transition region (C II 1334/1335 Å and Si IV 1394/1403 Å). Slit-jaw images in four different passbands (C II 1330, Si IV 1400, Mg II k 2796, and Mg II wing 2830 Å) can be taken simultaneously with spectral rasters that sample regions up to 130 arcsec × 175 arcsec at a variety of spatial samplings (from 0.33 arcsec and up). IRIS is sensitive to emission from plasma at temperatures between 5000 K and 10 MK and will advance our understanding of the flow of mass and energy through an interface region, formed by the chromosphere and transition region, between the photosphere and corona. This highly structured and dynamic region not only acts as the conduit of all mass and energy feeding into the corona and solar wind, it also requires an order of magnitude more energy to heat than the corona and solar wind combined. The IRIS investigation includes a strong numerical modeling component based on advanced radiative-MHD codes to facilitate interpretation of observations of this complex region. Approximately eight Gbytes of data (after compression) are acquired by IRIS each day and made available for unrestricted use within a few days of the observation. Title: The Rayleigh-Taylor Instability and the role of Prominences in the Chromosphere-Corona Mass Cycle Authors: Berger, Thomas; Liu, Wei; Hillier, Andrew; Scullion, Eamon; Low, Boon Chye Bibcode: 2014AAS...22421201B Altcode: We review recent results in the study of so-called "prominence bubbles", a buoyant instability discovered in quiescent solar prominences by the Hinode/SOT instrument in 2007. Analysis of the plasma flows along the boundary of the bubbles indicates that shear flows leading to Kelvin-Helmholtz instability waves can develop into the seed perturbations triggering the Rayleigh-Taylor instability. The non-linear phase of the RT instability leads to the formation of large turbulent plumes that transport the bubble plasma (and presumably magnetic flux) into the overlying coronal flux rope. We propose that the upward turbulent transport of hot bubble plasma and the downflows of cooler chromospheric plasma in the prominence are related aspects of a large-scale "chromosphere-corona mass cycle" in which hot plasma and magnetic flux and helicity from the chromosphere are transported upwards while the cooler prominence plasma downflows, which decouple from the magnetic field they are originally frozen-into, represent the condensation return flows of the cycle. This cycling enables a mechanism by which magnetic flux and helicity build up in the coronal flux rope while mass drains out of the flux rope, eventually triggering a "loss of confinement" eruption in the form of a CME. Title: Evidence of Magnetic Reconnection Involving Partially Ionized Coronal Rain near Null Points Observed by SDO/AIA and IRIS Authors: Liu, Wei; Antolin, Patrick; Sun, Xudong; Berger, Thomas E. Bibcode: 2014shin.confE..50L Altcode: Coronal rain is cool, partially ionized material formed in the hot, fully ionized corona. We report a newly discovered class of coronal rain formed near cusp-shaped portions of coronal loops, indicative of topological null points. We present evidence of cross-field flows associated with magnetic reconnection near such null points from SDO/AIA and IRIS observations, investigate the responsible magnetic environment, and infer clues to where and when catastrophic cooling take place to produce coronal rain. We also discuss the implications of such a cooling process for the enigmatic coronal heating mechanisms (e.g., Antolin et al. 2010) and compare transient coronal rain and persistent prominence downflows. Title: IRIS Observations of Coronal Rain and Prominences: Return Flows of the Chromosphere-Corona Mass Cycle Authors: Liu, Wei; Berger, Thomas; Antolin, Patrick; Schrijver, Karel Bibcode: 2014AAS...22431303L Altcode: It has recently been recognized that a mass cycle (e.g., Berger et al. 2011; McIntosh et al. 2012) between the hot, tenuous solar corona and the cool, dense chromosphere underneath it plays an important role in the mass budget and dynamic evolution of the solar atmosphere. Although the corona ultimately loses mass through the solar wind and coronal mass ejections, a fraction of its mass returns to the chromosphere in coronal rain, downflows of prominences, and other as-yet unidentified processes. We present here analysis of joint observations of IRIS, SDO/AIA, and Hinode/SOT of such phenomena. By utilizing the wide temperature coverage (logT: 4 - 7) provided by these instruments combined, we track the coronal cooling sequence (e.g., Schrijver 2001; Liu et al. 2012; Berger et al. 2012) leading to the formation of such material at transition region or chromospheric temperatures (logT: 4 - 5) in the million-degree corona. We compare the cooling times with those expected from the radiative cooling instability. We also measure the kinematics and densities of such downflows and infer their mass fluxes, which are compared to the upward mass fluxes into the corona, e.g., those associated with spicules and flux emergence. Special attention is paid to coronal rain formed near cusp-shaped portions of coronal loops, funnel-shaped prominences at dips of coronal loops, and their respective magnetic environments. With the information about where and when such catastrophic cooling events take place, we discuss the implications for the enigmatic coronal heating mechanisms (e.g., Antolin et al. 2010). Title: Dose and dose equivalent and related risk during a cruise to Mars Authors: Reitz, Günther; Matthiae, Daniel; Berger, Thomas; Zeitlin, Cary; Hassler, Don; Rafkin, Scott; Ehresmann, Bent; Cucinotta, Francis; Wimmer-Schweingruber, Robert; Boehm, Eckart; Burmeister, Soenke; Guo, Jingnan; Koehler, jan; Martin, Cesar; Boettcher, Stephan; Brinza, David; Posner, Arik Bibcode: 2014EGUGA..1616162R Altcode: The radiation exposure in space can be estimated with numerical simulations applying different models for the galactic cosmic rays (GCR) irradiating a defined shielding geometry or by in situ measurements. A comparison of commonly used GCR models, Badhwar-O'Neill2010, Burger-Usoskin, CREME2009/CREME96, and the recently released Badhwar-O'Neill 2011 with the newly developed DLR model show considerable differences in particle fluences. The differences arising in the calculated radiation exposure by applying these models were quantified in terms of absorbed dose and dose equivalent rates using the GEANT4 Monte-Carlo framework for different shielding thicknesses and the cumulative shielding distribution of the MSL transfer vehicle. The calculations are compared with actual measurement of the Radiation Assessment detector (RAD) of the Mars Science Lab (MSL) on its cruise towards Mars and on the surface of Mars. From the dose equivalents measured and calculated estimates of the upper and lower limits for the risks for a human flight to Mars assuming the radiation environment experienced by MSL-RAD are given using the NASA risk model. Title: GRB 141026A: Skynet PROMPT-CTIO/Yerkes-41 Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Hoette, V.; Cudworth, K.; Harper, D.; Kron, R.; Linder, T.; Russell, R.; Struble, E.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.16967....1T Altcode: 2014GCN..16967...1T No abstract at ADS Title: GRB 140215A: continued skynet PROMPT observations of the optical afterglow. Authors: Lacluyze, A.; Haislip, J.; Reichart, D.; Trotter, A.; Poshyachinda, S.; Rujopakarn, W.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15858....1L Altcode: 2014GCN..15858...1L No abstract at ADS Title: Mars' Surface Radiation Environment Measured with the Mars Science Laboratory's Curiosity Rover Authors: Hassler, Donald M.; Zeitlin, Cary; Wimmer-Schweingruber, Robert F.; Ehresmann, Bent; Rafkin, Scot; Eigenbrode, Jennifer L.; Brinza, David E.; Weigle, Gerald; Böttcher, Stephan; Böhm, Eckart; Burmeister, Soenke; Guo, Jingnan; Köhler, Jan; Martin, Cesar; Reitz, Guenther; Cucinotta, Francis A.; Kim, Myung-Hee; Grinspoon, David; Bullock, Mark A.; Posner, Arik; Gómez-Elvira, Javier; Vasavada, Ashwin; Grotzinger, John P.; MSL Science Team; Kemppinen, Osku; Cremers, David; Bell, James F.; Edgar, Lauren; Farmer, Jack; Godber, Austin; Wadhwa, Meenakshi; Wellington, Danika; McEwan, Ian; Newman, Claire; Richardson, Mark; Charpentier, Antoine; Peret, Laurent; King, Penelope; Blank, Jennifer; Schmidt, Mariek; Li, Shuai; Milliken, Ralph; Robertson, Kevin; Sun, Vivian; Baker, Michael; Edwards, Christopher; Ehlmann, Bethany; Farley, Kenneth; Griffes, Jennifer; Miller, Hayden; Newcombe, Megan; Pilorget, Cedric; Rice, Melissa; Siebach, Kirsten; Stack, Katie; Stolper, Edward; Brunet, Claude; Hipkin, Victoria; Léveillé, Richard; Marchand, Geneviève; Sánchez, Pablo Sobrón; Favot, Laurent; Cody, George; Steele, Andrew; Flückiger, Lorenzo; Lees, David; Nefian, Ara; Martin, Mildred; Gailhanou, Marc; Westall, Frances; Israël, Guy; Agard, Christophe; Baroukh, Julien; Donny, Christophe; Gaboriaud, Alain; Guillemot, Philippe; Lafaille, Vivian; Lorigny, Eric; Paillet, Alexis; Pérez, René; Saccoccio, Muriel; Yana, Charles; Armiens-Aparicio, Carlos; Rodríguez, Javier Caride; Blázquez, Isaías Carrasco; Gómez, Felipe Gómez; Hettrich, Sebastian; Malvitte, Alain Lepinette; Jiménez, Mercedes Marín; Martínez-Frías, Jesús; Martín-Soler, Javier; Martín-Torres, F. Javier; Jurado, Antonio Molina; Mora-Sotomayor, Luis; Caro, Guillermo Muñoz; López, Sara Navarro; Peinado-González, Verónica; Pla-García, Jorge; Manfredi, José Antonio Rodriguez; Romeral-Planelló, Julio José; Fuentes, Sara Alejandra Sans; Martinez, Eduardo Sebastian; Redondo, Josefina Torres; Urqui-O'Callaghan, Roser; Mier, María-Paz Zorzano; Chipera, Steve; Lacour, Jean-Luc; Mauchien, Patrick; Sirven, Jean-Baptiste; Manning, Heidi; Fairén, Alberto; Hayes, Alexander; Joseph, Jonathan; Squyres, Steven; Sullivan, Robert; Thomas, Peter; Dupont, Audrey; Lundberg, Angela; Melikechi, Noureddine; Mezzacappa, Alissa; Berger, Thomas; Matthia, Daniel; Prats, Benito; Atlaskin, Evgeny; Genzer, Maria; Harri, Ari-Matti; Haukka, Harri; Kahanpää, Henrik; Kauhanen, Janne; Kemppinen, Osku; Paton, Mark; Polkko, Jouni; Schmidt, Walter; Siili, Tero; Fabre, Cécile; Wray, James; Wilhelm, Mary Beth; Poitrasson, Franck; Patel, Kiran; Gorevan, Stephen; Indyk, Stephen; Paulsen, Gale; Gupta, Sanjeev; Bish, David; Schieber, Juergen; Gondet, Brigitte; Langevin, Yves; Geffroy, Claude; Baratoux, David; Berger, Gilles; Cros, Alain; d'Uston, Claude; Forni, Olivier; Gasnault, Olivier; Lasue, Jérémie; Lee, Qiu-Mei; Maurice, Sylvestre; Meslin, Pierre-Yves; Pallier, Etienne; Parot, Yann; Pinet, Patrick; Schröder, Susanne; Toplis, Mike; Lewin, Éric; Brunner, Will; Heydari, Ezat; Achilles, Cherie; Oehler, Dorothy; Sutter, Brad; Cabane, Michel; Coscia, David; Israël, Guy; Szopa, Cyril; Dromart, Gilles; Robert, François; Sautter, Violaine; Le Mouélic, Stéphane; Mangold, Nicolas; Nachon, Marion; Buch, Arnaud; Stalport, Fabien; Coll, Patrice; François, Pascaline; Raulin, François; Teinturier, Samuel; Cameron, James; Clegg, Sam; Cousin, Agnès; DeLapp, Dorothea; Dingler, Robert; Jackson, Ryan Steele; Johnstone, Stephen; Lanza, Nina; Little, Cynthia; Nelson, Tony; Wiens, Roger C.; Williams, Richard B.; Jones, Andrea; Kirkland, Laurel; Treiman, Allan; Baker, Burt; Cantor, Bruce; Caplinger, Michael; Davis, Scott; Duston, Brian; Edgett, Kenneth; Fay, Donald; Hardgrove, Craig; Harker, David; Herrera, Paul; Jensen, Elsa; Kennedy, Megan R.; Krezoski, Gillian; Krysak, Daniel; Lipkaman, Leslie; Malin, Michael; McCartney, Elaina; McNair, Sean; Nixon, Brian; Posiolova, Liliya; Ravine, Michael; Salamon, Andrew; Saper, Lee; Stoiber, Kevin; Supulver, Kimberley; Van Beek, Jason; Van Beek, Tessa; Zimdar, Robert; French, Katherine Louise; Iagnemma, Karl; Miller, Kristen; Summons, Roger; Goesmann, Fred; Goetz, Walter; Hviid, Stubbe; Johnson, Micah; Lefavor, Matthew; Lyness, Eric; Breves, Elly; Dyar, M. Darby; Fassett, Caleb; Blake, David F.; Bristow, Thomas; DesMarais, David; Edwards, Laurence; Haberle, Robert; Hoehler, Tori; Hollingsworth, Jeff; Kahre, Melinda; Keely, Leslie; McKay, Christopher; Wilhelm, Mary Beth; Bleacher, Lora; Brinckerhoff, William; Choi, David; Conrad, Pamela; Dworkin, Jason P.; Floyd, Melissa; Freissinet, Caroline; Garvin, James; Glavin, Daniel; Harpold, Daniel; Jones, Andrea; Mahaffy, Paul; Martin, David K.; McAdam, Amy; Pavlov, Alexander; Raaen, Eric; Smith, Michael D.; Stern, Jennifer; Tan, Florence; Trainer, Melissa; Meyer, Michael; Voytek, Mary; Anderson, Robert C.; Aubrey, Andrew; Beegle, Luther W.; Behar, Alberto; Blaney, Diana; Calef, Fred; Christensen, Lance; Crisp, Joy A.; DeFlores, Lauren; Ehlmann, Bethany; Feldman, Jason; Feldman, Sabrina; Flesch, Gregory; Hurowitz, Joel; Jun, Insoo; Keymeulen, Didier; Maki, Justin; Mischna, Michael; Morookian, John Michael; Parker, Timothy; Pavri, Betina; Schoppers, Marcel; Sengstacken, Aaron; Simmonds, John J.; Spanovich, Nicole; Juarez, Manuel de la Torre; Webster, Christopher R.; Yen, Albert; Archer, Paul Douglas; Jones, John H.; Ming, Douglas; Morris, Richard V.; Niles, Paul; Rampe, Elizabeth; Nolan, Thomas; Fisk, Martin; Radziemski, Leon; Barraclough, Bruce; Bender, Steve; Berman, Daniel; Dobrea, Eldar Noe; Tokar, Robert; Vaniman, David; Williams, Rebecca M. E.; Yingst, Aileen; Lewis, Kevin; Leshin, Laurie; Cleghorn, Timothy; Huntress, Wesley; Manhès, Gérard; Hudgins, Judy; Olson, Timothy; Stewart, Noel; Sarrazin, Philippe; Grant, John; Vicenzi, Edward; Wilson, Sharon A.; Hamilton, Victoria; Peterson, Joseph; Fedosov, Fedor; Golovin, Dmitry; Karpushkina, Natalya; Kozyrev, Alexander; Litvak, Maxim; Malakhov, Alexey; Mitrofanov, Igor; Mokrousov, Maxim; Nikiforov, Sergey; Prokhorov, Vasily; Sanin, Anton; Tretyakov, Vladislav; Varenikov, Alexey; Vostrukhin, Andrey; Kuzmin, Ruslan; Clark, Benton; Wolff, Michael; McLennan, Scott; Botta, Oliver; Drake, Darrell; Bean, Keri; Lemmon, Mark; Schwenzer, Susanne P.; Anderson, Ryan B.; Herkenhoff, Kenneth; Lee, Ella Mae; Sucharski, Robert; Hernández, Miguel Ángel de Pablo; Ávalos, Juan José Blanco; Ramos, Miguel; Malespin, Charles; Plante, Ianik; Muller, Jan-Peter; Navarro-González, Rafael; Ewing, Ryan; Boynton, William; Downs, Robert; Fitzgibbon, Mike; Harshman, Karl; Morrison, Shaunna; Dietrich, William; Kortmann, Onno; Palucis, Marisa; Sumner, Dawn Y.; Williams, Amy; Lugmair, Günter; Wilson, Michael A.; Rubin, David; Jakosky, Bruce; Balic-Zunic, Tonci; Frydenvang, Jens; Jensen, Jaqueline Kløvgaard; Kinch, Kjartan; Koefoed, Asmus; Madsen, Morten Bo; Stipp, Susan Louise Svane; Boyd, Nick; Campbell, John L.; Gellert, Ralf; Perrett, Glynis; Pradler, Irina; VanBommel, Scott; Jacob, Samantha; Owen, Tobias; Rowland, Scott; Atlaskin, Evgeny; Savijärvi, Hannu; García, César Martín; Mueller-Mellin, Reinhold; Bridges, John C.; McConnochie, Timothy; Benna, Mehdi; Franz, Heather; Bower, Hannah; Brunner, Anna; Blau, Hannah; Boucher, Thomas; Carmosino, Marco; Atreya, Sushil; Elliott, Harvey; Halleaux, Douglas; Rennó, Nilton; Wong, Michael; Pepin, Robert; Elliott, Beverley; Spray, John; Thompson, Lucy; Gordon, Suzanne; Newsom, Horton; Ollila, Ann; Williams, Joshua; Vasconcelos, Paulo; Bentz, Jennifer; Nealson, Kenneth; Popa, Radu; Kah, Linda C.; Moersch, Jeffrey; Tate, Christopher; Day, Mackenzie; Kocurek, Gary; Hallet, Bernard; Sletten, Ronald; Francis, Raymond; McCullough, Emily; Cloutis, Ed; ten Kate, Inge Loes; Kuzmin, Ruslan; Arvidson, Raymond; Fraeman, Abigail; Scholes, Daniel; Slavney, Susan; Stein, Thomas; Ward, Jennifer; Berger, Jeffrey; Moores, John E. Bibcode: 2014Sci...343D.386H Altcode: The Radiation Assessment Detector (RAD) on the Mars Science Laboratory's Curiosity rover began making detailed measurements of the cosmic ray and energetic particle radiation environment on the surface of Mars on 7 August 2012. We report and discuss measurements of the absorbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on the martian surface for ~300 days of observations during the current solar maximum. These measurements provide insight into the radiation hazards associated with a human mission to the surface of Mars and provide an anchor point with which to model the subsurface radiation environment, with implications for microbial survival times of any possible extant or past life, as well as for the preservation of potential organic biosignatures of the ancient martian environment. Title: Introduction to session F2.3 ``Space Radiation Dosimetry—Measurements and Models, Detector Development and Groundbased Characterisation'' Authors: Berger, Thomas Bibcode: 2014cosp...40E.293B Altcode: Introduction to the session F2.3 "Space Radiation Dosimetry" Title: Prominence Science with ATST Instrumentation Authors: Rimmele, Thomas; Berger, Thomas; Casini, Roberto; Elmore, David; Kuhn, Jeff; Lin, Haosheng; Schmidt, Wolfgang; Wöger, Friedrich Bibcode: 2014IAUS..300..362R Altcode: The 4m Advance Technology Solar Telescope (ATST) is under construction on Maui, HI. With its unprecedented resolution and photon collecting power ATST will be an ideal tool for studying prominences and filaments and their role in producing Coronal Mass Ejections that drive Space Weather. The ATST facility will provide a set of first light instruments that enable imaging and spectroscopy of the dynamic filament and prominence structure at 8 times the resolution of Hinode. Polarimeters allow high precision chromospheric and coronal magnetometry at visible and infrared (IR) wavelengths. This paper summarizes the capabilities of the ATST first-light instrumentation with focus on prominence and filament science. Title: European Crew Personal Active Dosimeter (EuCPAD), a novel dosimetry system utilizing operational and scientific synergies for the benefit of humans in space Authors: Straube, Ulrich; Berger, Thomas Bibcode: 2014cosp...40E3215S Altcode: A significant expansion of Human presence in space can be recognized over the last decade. Not only the frequency of human space mission did rise, but also time in space, mission duration with extended flights lasting half a year or more are becoming "standard". Despite the challenges to human health and well-being are still significant, or may even increase with mission length and work density. Also radiation exposure in space remains one of the inevitable and dominating factors relevant to crew- health, -safety and therefore mission success. The radiation environment that the space crews are exposed to differs significantly as compared to earth. Exposure in flight exceed doses that are usually received by terrestrial radiation workers on ground. Expanding "medical" demands are not a solely characteristics of current and current and upcoming mission scenarios. Likewise the margins for what is understood as "efficient utilization" for the fully operational science platform ISS, are immense. Understanding, accepting and approaching these challenges ESA-HSO did choose a particular pass of implementation for one of their current developments. Exploiting synergies of research, science and medical operational aspects, the "European Crew Personal Active Dosimeter for Astronauts (EuCPAD)" development exactly addresses these circumstances. It becomes novel part of ESA Radiation Protection Initiative for astronauts. The EuCPAD project aims at the development and manufacturing of an active (powered) dosimeter system to measure astronaut's exposures, support risk assessment dose management by providing a differentiated data set. Final goal is the verification of the system capabilities for medical monitoring at highest standards. The EuCPAD consists of several small portable Personal Active Dosimeters (MU = Mobile Unitas) and a rack mounted docking station “Personal Storage Device (PSD)” for MU storage, data read out and telemetry. The PSD furthermore contains a Tissue Equivalent Proportional Counter (TEPC) and an internal MU(iMU) to enable complex environmental measurements and cross calibrations. This presentation will give an introduction to the dosimetry system and of the current status. The EuCPAD project is carried out under ESA Contract No. 4200023059/09/NL/CP, Title: 10Be Production in the Atmosphere by Galactic Cosmic Rays Authors: Matthiä, Daniel; Herbst, Klaudia; Heber, Bernd; Berger, Thomas; Reitz, Günther Bibcode: 2014crh..book..333M Altcode: No abstract at ADS Title: GRB 141221A: Skynet PROMPT-CTIO observations of the optical afterglow. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17210....1T Altcode: 2014GCN..17210...1T No abstract at ADS Title: Dose Measurements on the BION-M1 satellite applying passive detector packages Authors: Stradi, Andrea; Berger, Thomas; Kodaira, Satoshi; Kubancak, Jan; Palfalvi, Jozsef K.; Ambrozova, Iva; Tolochek, Raisa; Shurshakov, Vyacheslav; Szabo, Julianna Bibcode: 2014cosp...40E3214S Altcode: A passive detector package was developed in the past years in the Centre for Energy Research, Hungarian Academy of Science to detect cosmic ray particles, to determine their flux and dose. It consists of thermoluminescent detectors (TLD) and plastic solid state nuclear track detectors (SSNTD). In the frame of a scientific co-operation between the Institute for Biomedical Problems (IBMP) fourteen packages were flow within the new BION-M1 satellite program together with biological samples and detector packages from other participants. Two packages were located outside and the rest ones inside the recoverable capsule. Comparing to the previous BION and similar FOTON experiments, (all together 17 successful ones), this flight was a “champion” with the highest altitude (575 km), orbital inclination (64.9°) and flight duration (30 days). The external exposure provided a unique possibility to study not only the elevated level of cosmic rays but also the behavior of the detector packages in extreme circumstances as low temperature and pressure. The paper will summarize the construction of the detector packages, the calibration and evaluation processes, as well as, the linear energy transfer (LET) spectra, the absorbed dose and the mean quality factor. These quantities will be compared taking into consideration their location inside and outside the capsule and to the results of other participants. Also some comparison of results to the previous BION and FOTON flights and contemporary measurements on the ISS will be presented. Title: GRB 140301A: skynet R-COP observations. Authors: Trotter, A.; Haislip, J.; Lacluyze, A.; Reichart, D.; Verveer, A.; Spuck, T.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15897....1T Altcode: 2014GCN..15897...1T No abstract at ADS Title: Future Diagnostic Capabilities: The 4-meter Daniel K. Inouye Solar Telescope Authors: Berger, Thomas; Reardon, Kevin; Elmore, David; Woeger, Friedrich; Tritschler, Alexandra; Rimmele, Thomas Bibcode: 2014cosp...40E.294B Altcode: We discuss the observational capabilities of the Daniel K. Inouye Solar Telescope (DKSIT), formerly known as the Advanced Technology Solar Telescope (ATST), currently under construction on Haleakala Mountain on the island of Maui, Hawaii, with first light anticipated in mid-2019. The DKIST will be a 4-meter aperture Gregorian telescope with advanced environmental control and adaptive optics capable of producing diffraction-limited resolution in visible light of 0.03" or about 20 km in the solar photosphere. The first light instrument suite will include the Visible Broadband Imager (VBI), an interference filter-based instrument capable of 30 Hz imaging of photospheric and chromospheric magnetic structures in the 380 to 800 nm wavelength range. All VBI images will be reconstructed in near-real-time using the KISIP speckle reconstruction algorithm adapted to the DKIST optical and AO configuration. The Visible Spectropolarimeter (ViSP) instrument being fabricated by the High Altitude Observatory (HAO) will enable high-precision slit-spectropolarimetery in any three spectral regions from 380 to 900 nm. The ViSP instrument will be the highest precision spectropolarimeter ever produced with a spatial resolution of approximately 40 km at 600 nm and temporal resolution of 10s to achieve 1e-03 polarimetric precision. The Visible Tunable Filter (VTF) instrument under fabrication at the Kiepenheuer Institute for Solar Physics (KIS) is a triple-etalon Fabry-Perot imaging spectropolarimeter instrument capable of diffraction limited measurements of the Fe I 630.2 nm and Ca II 854.2 nm spectral lines for Doppler and magnetic measurements in the photosphere and chromosphere, respectively. The VTF will also enable the highest spatial and temporal resolution observations yet achieved in the H-alpha line for detailed studies of chromospheric dynamics in response to photospheric magnetic drivers. The Diffraction-Limited Near-IR Spectropolarimeter (DL-NiRSP) and the Cryogenic Near-IR Spectropolarimeter (Cryo-NiRSP) instruments, both under fabrication at the University of Hawaii, will enable polarimetric and spectroscopic investigations in the largely unexplored infra-red spectral region. The DL-NiRSP will span 900 nm to 2.5 microns in wavelength and include a novel fiber-optic "Integral Field Unit" (IFU) for true imaging spectropolarimetry in three simultaneous spectral regions over a variable field of view. This instrument will enable revolutionary measurements of prominence magnetic fields and will also, in the wider field mode, enable coronal polarimetric studies. The Cryo-NiRSP instrument spans the 1--5 micron wavelength range and will make near-diffraction limited 0.3" resolution slit-scan measurements of the coronal magnetic field out to 1.3 solar radii with temporal resolution measured in minutes. The DKIST facility will undergo extensive polarimetric calibration to ensure that the ultimate goal of 5e-04 polarimetic precision is obtainable under the best conditions. All of the data from the DKIST will be transmitted to the central DKIST data center in Boulder, Colorado where automated reduction and calibration pipelines will rapidly provide the community with calibrated data products for use in science investigations. The DKIST will also be operated in a "Service Mode" access model in which investigators will not be required to travel to the telescope to accomplish their science observations. Title: GRB 140518A: Skynet GORT Detections of the Optical Afterglow. Authors: Trotter, A.; Lacluyze, A.; Haislip, J.; Reichart, D.; McLin, K.; Cominsky, L.; Cromartie, H. T.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Dow, A.; Hinckle, M.; Patterson, A.; Pegues, H.; Pozo, J.; Waddell, D.; Crain, J. A. Bibcode: 2014GCN.16304....1T Altcode: 2014GCN..16304...1T No abstract at ADS Title: Solar Prominence Fine Structure and Dynamics Authors: Berger, Thomas Bibcode: 2014IAUS..300...15B Altcode: We review recent observational and theoretical results on the fine structure and dynamics of solar prominences, beginning with an overview of prominence classifications, the proposal of possible new ``funnel prominence'' classification, and a discussion of the recent ``solar tornado'' findings. We then focus on quiescent prominences to review formation, down-flow dynamics, and the ``prominence bubble'' phenomena. We show new observations of the prominence bubble Rayleigh-Taylor instability triggered by a Kelvin-Helmholtz shear flow instability occurring along the bubble boundary. Finally we review recent studies on plasma composition of bubbles, emphasizing that differential emission measure (DEM) analysis offers a more quantitative analysis than photometric comparisons. In conclusion, we discuss the relation of prominences to coronal magnetic flux ropes, proposing that prominences can be understood as partially ionized condensations of plasma forming the return flow of a general magneto-thermal convection in the corona. Title: Development of a New Radiation Sensor for Satellite Missions Authors: Ritter, Birgit; Berger, Thomas; Reitz, Guenther; Hauslage, Jens; Marsalek, Karel; Aeckerlein, Joachim; M, Hartmut Bibcode: 2014cosp...40E2748R Altcode: The RAMIS (RAdiation Measurements In Space) experiment aims to measure cosmic radiation with energy deposition ranging from minimal ionizing protons up to relativistic iron nuclei. The radiation detector principle uses two silicon detectors, each with an active area of 0.5cm² that are arranged in a telescope configuration. The experiment will fly in 2016 on the first mission of the newly developed DLR (German Aerospace Center) Compact Satellite, which intends to provide an easy accessible platform for scientific research within DLR as well as for international partners and their experiments. As the satellite will orbit Earth at an altitude of about 600 km on a polar orbit, valuable insights are gained not only in the galactic cosmic ray (GCR) component of the radiation field and in solar energetic particles (SEPs) in case of solar events. Also the trapped radiation in the horns of the electron belts around Earth can be studied in detail. Particle fluxes will be monitored and energy deposition spectra recorded from which linear energy transfer spectra will be generated. These spectra give an estimate for the quality of the radiation field. The RAMIS experiment consists of two modules, i.e. two small silicon detector telescopes, with one module being located outside on top of the satellite, while the other one is placed inside next to the primary payload of the satellite, the Eu:CROPIS experiment. Eu:CROPIS is a combined self-sustained biological life support system under Moon and Mars gravity, which uses Euglena as oxygen suppliers, biofilter for wastewater treatment and detoxification, and urine as primary fertilizer. In addition to its scientific output RAMIS will provide dosimetric monitoring for Eu:CROPIS and serve as a radiation exposure information system for the satellite bus. Furthermore the obtained data can be used for benchmarking and improvement of radiation belt models as well as of shielding models by combining the results of both modules. The RAMIS experiment, the prototype performance and first test measurements of the detector system will be presented. Title: Long term dose monitoring onboard the European Columbus module of the International Space Station (ISS) in the frame of the DOSIS and DOSIS 3D project Authors: Berger, Thomas Bibcode: 2014cosp...40E.292B Altcode: The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station (ISS) is therefore needed. For the investigation of the spatial and temporal distribution of the radiation field inside the European Columbus module the experiment “Dose Distribution Inside the ISS” (DOSIS), under the project and science lead of the German Aerospace Center (DLR), was launched on July 15th 2009 with STS-127 to the ISS. The DOSIS experiment consists of a combination of “Passive Detector Packages” (PDP) distributed at eleven locations inside Columbus for the measurement of the spatial variation of the radiation field and two active Dosimetry Telescopes (DOSTELs) with a Data and Power Unit (DDPU) in a dedicated nomex pouch mounted at a fixed location beneath the European Physiology Module rack (EPM) for the measurement of the temporal variation of the radiation field parameters. The DOSIS experiment suite measured during the lowest solar minimum conditions in the space age from July 2009 to June 2011. In July 2011 the active hardware was transferred to ground for refurbishment and preparation for the follow up DOSIS 3D experiment. The hardware for DOSIS 3D was launched with Soyuz 30S to the ISS on May 15th 2012. The PDPs are replaced with each even number Soyuz flight starting with Soyuz 30S. Data from the active detectors is transferred to ground via the EPM rack which is activated once a month for this action. The presentation will give an overview of the DOSIS and DOSIS 3D experiment and focus on the results from the passive radiation detectors from the DOSIS 3D experiment (2012 - 2014) in comparison to the data of the DOSIS experiment (2009 - 2011). The Polish contribution was supported by the National Science Centre (No DEC-2012/06/M/ST9/00423). The CAU contributions to DOSIS and DOSIS 3D are financially supported by BMWi under Grants 50WB0826, 50WB1026 and 50WB1232. Title: GRB 141221A: Continued Skynet PROMPT-CTIO observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17221....1T Altcode: 2014GCN..17221...1T No abstract at ADS Title: GRB 141031A: Skynet PROMPT-CTIO Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17004....1T Altcode: 2014GCN..17004...1T No abstract at ADS Title: GRB140215A: skynet PROMPT optical observations. Authors: Lacluyze, A.; Haislip, J.; Reichart, D.; Trotter, A.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15840....1L Altcode: 2014GCN..15840...1L No abstract at ADS Title: Correction: MAXI J1421-613: skynet PROMPT/R-COP observations. Authors: Trotter, A.; Reichart, D.; Verveer, A.; Spuck, T.; Lacluyze, A.; Haislip, J.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A.; Baumgartner, W. H. Bibcode: 2014GCN.15755....1T Altcode: 2014GCN..15755...1T No abstract at ADS Title: GRB 141022A: Skynet PROMPT-CTIO Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17023....1T Altcode: 2014GCN..17023...1T No abstract at ADS Title: GRB 140213A: continued skynet R-COP/PROMPT detections of a rebrightening optical afterglow. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Verveer, A.; Spuck, T.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15859....1T Altcode: 2014GCN..15859...1T No abstract at ADS Title: GRB 141212A: Skynet R-COP Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Verveer, A.; Spuck, T.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17161....1T Altcode: 2014GCN..17161...1T No abstract at ADS Title: GRB 141017A: Skynet PROMPT-CTIO/SSO Observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Aji, A.; Beauchemin, R.; Berger, T.; Dow, A.; Foster, A.; Frank, N.; Hinckle, M.; Ivarsen, K.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Salemi, C.; Zbinden, L.; Crain, J. A. Bibcode: 2014GCN.17028....1T Altcode: 2014GCN..17028...1T No abstract at ADS Title: GRB 140118A/MAXI J1421-613: skynet PROMPT/R-COP observations. Authors: Trotter, A.; Reichart, D.; Verveer, A.; Spuck, T.; Lacluyze, A.; Haislip, J.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15753....1T Altcode: 2014GCN..15753...1T No abstract at ADS Title: GRB 140213A: continued skynet R-COP/PROMPT observations of the optical afterglow. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Verveer, A.; Spuck, T.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15862....1T Altcode: 2014GCN..15862...1T No abstract at ADS Title: GRB 140213A: skynet R-COP detection of optical afterglow. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Verveer, A.; Spuck, T.; Foster, A.; Frank, N.; Ivarsen, K.; Moore, J.; Nysewander, M.; Beauchemin, R.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Hinckle, M.; Ireland, A.; Maples, M.; Scott, L.; Crain, J. A. Bibcode: 2014GCN.15828....1T Altcode: 2014GCN..15828...1T No abstract at ADS Title: Long term dose monitoring onboard the European Columbus module of the international space station (ISS) in the frame of DOSIS and DOSIS 3D project - results from the active instruments Authors: Burmeister, Soenke; Berger, Thomas; Reitz, Guenther; Boehme, Matthias; Haumann, Lutz; Labrenz, Johannes Bibcode: 2014cosp...40E.434B Altcode: Besides the effects of the microgravity environment, and the psychological and psychosocial problems encountered in confined spaces, radiation is the main health detriment for long duration human space missions. The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones encountered on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station ISS is therefore needed. For the investigation of the spatial and temporal distribution of the radiation field inside the European COLUMBUS module the experiment DOSIS (Dose Distribution Inside the ISS) under the lead of DLR has been launched on July 15 (th) 2009 with STS-127 to the ISS. The experimental package was transferred from the Space Shuttle into COLUMBUS on July 18 (th) . It consists of a combination of passive detector packages (PDP) distributed at 11 locations inside the European Columbus Laboratory and two active radiation detectors (Dosimetry Telescopes = DOSTELs) with a DDPU (DOSTEL Data and Power Unit) in a Nomex pouch (DOSIS MAIN BOX) mounted at a fixed location beneath the European Physiology Module rack (EPM) inside COLUMBUS. The active components of the DOSIS experiment were operational from July 18 (th) 2009 to June 16 (th) 2011. After refurbishment the hardware has been reactivated on May 15 (th) 2012 as active part of the DOSIS 3D experiment and provides continuous data since this activation. The presentation will focus on the latest results from the two DOSTEL instruments as absorbed dose, dose equivalent and the related LET spectra gathered within the DOSIS (2009 - 2011) and DOSIS 3D (2012 - 2014) experiment. The CAU contributions to DOSIS and DOSIS 3D are financially supported by BMWi under Grants 50WB0826, 50WB1026 and 50WB1232 Title: Coronal Condensation in Funnel Prominences as Return Flows of the Chromosphere-Corona Mass Cycle Authors: Liu, Wei; Berger, Thomas E.; Low, B. C. Bibcode: 2014IAUS..300..441L Altcode: We present SDO/AIA observations of a potentially novel type of prominence, called ``funnel prominence'', that forms out of coronal condensation at magnetic dips.

They can drain a large amount of mass (up to ~1015 g day-1) and may play an important role as return flows of the chromosphere-corona mass cycle. Title: Preparation of the Biochip experiment on the EXPOSE-R2 mission outside the International Space Station Authors: Vigier, F.; Le Postollec, A.; Coussot, G.; Chaput, D.; Cottin, H.; Berger, T.; Incerti, S.; Triqueneaux, S.; Dobrijevic, M.; Vandenabeele-Trambouze, O. Bibcode: 2013AdSpR..52.2168V Altcode: Biochips might be suited for planetary exploration. Indeed, they present great potential for the search for biomarkers - molecules that are the sign of past or present life in space - thanks to their size (miniaturized devices) and sensitivity. Their detection principle is based on the recognition of a target molecule by affinity receptors fixed on a solid surface. Consequently, one of the main concerns when developing such a system is the behavior of the biological receptors in a space environment. In this paper, we describe the preparation of an experiment planned to be part of the EXPOSE-R2 mission, which will be conducted on the EXPOSE-R facility, outside the International Space Station (ISS), in order to study the resistance of biochip models to space constraints (especially cosmic radiation and thermal cycling). This experiment overcomes the limits of ground tests which do not reproduce exactly the space parameters. Indeed, contrary to ground experiments where constraints are applied individually and in a limited time, the biochip models on the ISS will be exposed to cumulated constraints during several months. Finally, this ISS experiment is a necessary step towards planetary exploration as it will help assessing whether a biochip can be used for future exploration missions. Title: Estimation of Galactic Cosmic Ray exposure inside and outside the Earth's magnetosphere during the recent solar minimum between solar cycles 23 and 24 Authors: Mrigakshi, Alankrita Isha; Matthiä, Daniel; Berger, Thomas; Reitz, Günther; Wimmer-Schweingruber, Robert F. Bibcode: 2013AdSpR..52..979M Altcode: The evidently low solar activity observed between solar cycles 23 and 24 during the years 2008-2010 led to a substantial increase in the Galactic Cosmic Ray (GCR) intensity in comparison with preceding solar minima. As the GCRs consist of highly-ionizing charged particles having the potential to cause biological damage, they are a subject of concern for manned missions to space. With the enhanced particle fluxes observed between 2008 and 2010, it is reasonable to assume that the radiation exposure from GCR must have also increased to unusually high levels. In this paper, the GCR exposure outside and inside the Earth's magnetosphere is numerically calculated for time periods starting from 1970 to the end of 2011 in order to investigate the increase in dose levels during the years 2008-2010 in comparison with the last three solar minima. The dose rates were calculated in a water sphere, used as a surrogate for the human body, either unshielded or surrounded by aluminium shielding of 0.3, 10 or 40 g/cm2. By performing such a long-term analysis, it was estimated that the GCR exposure during the recent solar minimum was indeed the largest in comparison with previous minima and that the increase was more pronounced for locations outside the magnetosphere. Title: Organ shielding and doses in Low-Earth orbit calculated for spherical and anthropomorphic phantoms Authors: Matthiä, Daniel; Berger, Thomas; Reitz, Günther Bibcode: 2013AdSpR..52..528M Altcode: Humans in space are exposed to elevated levels of radiation compared to ground. Different sources contribute to the total exposure with galactic cosmic rays being the most important component. The application of numerical and anthropomorphic phantoms in simulations allows the estimation of dose rates from galactic cosmic rays in individual organs and whole body quantities such as the effective dose. The male and female reference phantoms defined by the International Commission on Radiological Protection and the hermaphrodite numerical RANDO phantom are voxel implementations of anthropomorphic phantoms and contain all organs relevant for radiation risk assessment. These anthropomorphic phantoms together with a spherical water phantom were used in this work to translate the mean shielding of organs in the different anthropomorphic voxel phantoms into positions in the spherical phantom. This relation allows using a water sphere as surrogate for the anthropomorphic phantoms in both simulations and measurements. Moreover, using spherical phantoms in the calculation of radiation exposure offers great advantages over anthropomorphic phantoms in terms of computational time. In this work, the mean shielding of organs in the different voxel phantoms exposed to isotropic irradiation is presented as well as the corresponding depth in a water sphere. Dose rates for Low-Earth orbit from galactic cosmic rays during solar minimum conditions were calculated using the different phantoms and are compared to the results for a spherical water phantom in combination with the mean organ shielding. For the spherical water phantom the impact of different aluminium shielding between 1 g/cm2 and 100 g/cm2 was calculated. The dose equivalent rates were used to estimate the effective dose rate. Title: The Advanced Technology Solar Telescope Construction Status Report Authors: McMullin, Joseph P.; Rimmele, T. R.; Warner, M.; Berger, T.; Keil, S. L. Bibcode: 2013SPD....4440001M Altcode: The Advanced Technology Solar Telescope (ATST) will provide observing capabilities in the visible through infrared wavelengths with unprecedented resolution and sensitivity. Designed to study solar magnetism that controls the solar wind, flares, CMEs and variability in the Sun's output, the ATST will be capable of detecting and spatially resolving the fundamental astrophysical processes at their intrinsic scales throughout the solar atmosphere. The 4-m class facility is currently under construction in Maui, HI on the Haleakala Observatories site with a scheduled completion of July 2019. Since the start of site construction in December of 2012, significant progress has been made toward the development of the observatory buildings (excavation, foundations, working towards the steel erection). In addition, off-site, the major subsystems of the telescope have been contracted, designs are complete and fabrication is underway. We review the science drivers, design details, technical challenges, and provide a construction status update on the subsystems and their integration. Title: The ATST Instrumentation suite: capabilities, synergies, and science goals Authors: Berger, Thomas; ATST Science Team Bibcode: 2013SPD....4440002B Altcode: The ATST will have a full complement of first generation instrumentation to cover observations of the solar atmosphere from the photosphere to the corona: the Visible Broadband Imager (VBI) will be an interference filter imager providing the highest spatial and temporal resolution image sequences for ATST, spanning from the deep photosphere through the chromosphere, and perhaps providing coronal imaging as well; the Visible Spectropolarimeter (ViSP) will be an advanced slit spectropolarimeter enabling simultaneous multi-line spectropolarimetry from 380 to 900 nm; the Visible Tunable Filter (VTF) will be a dual tunable Fabry-Perot system enabling rapid cadence spectral imaging and spectropolarimetry in the 520 to 870 nm range; the Diffraction-limited Near-IR Spectropolarimeter (DL-NiRSP) will be an advanced fiber-optic image plane spectropolarimeter offering simultaneous imaging and full-profile spectropolarimetry from 900 to 2500 nm; and the Cryogenic Near-IR Spectropolarimeter (Cryo-NiRSP) will provide coronal slit spectropolarimetry from 1--5 microns. We will review the science capabilities of these first generation instruments as well as their synergistic use in multi-instrument observing programs to achieve novel science investigations. Title: Funnel Prominences as Return Flows of the Chromosphere-Corona Mass Cycle: SDO/AIA Observations of Coronal Condensation Authors: Liu, Wei; Berger, T.; Low, B. C. Bibcode: 2013SPD....44...42L Altcode: It has recently been proposed that prominences play an important role as return flows of the chromosphere-corona mass cycle, in which hot plasma is transported upward in forms of spicules and prominence bubbles (likely due to flux emergence), while cool plasma drains downward in forms of vertical prominence threads (Berger et al. 2011 Nature). A critical step in this cycle is the condensation of the million-degree coronal plasma into T<10,000 K prominence material by a radiative cooling instability (i.e., thermal non-equilibrium), as numerically simulated (Karpen & Antiochos 2008; Xia et al. 2012) and first evidenced in recent SDO/AIA observations (Liu et al. 2012; Berger et al. 2012 ApJL). Such a runaway cooling process occurs in coronal loops of various sizes and generally leads to condensation at magnetic dips and formation of funnel-shaped prominences. A moderate-sized prominence can drain a significant mass of typically 10^15 gram/day, which is comparable to the mass of a CME or a fraction of the entire corona. Here we present a survey of funnel prominences that appear to be common in AIA observations at various locations and times. We find longer cooling times in longer/taller coronal loops whose densities are lower, consistent with the expected quadratic dependence on density of the optically-thin radiative loss. We propose that such funnel prominences, usually small in size, can constitute a new type of prominences, and similar processes can produce elementary building blocks of large-scale quiescent prominences in filament channels. This picture is supported by the recent theoretical development on spontaneous formation of current sheets and condensations manifested as prominence threads (Low et al. 2012a, b, ApJ).Abstract (2,250 Maximum Characters): It has recently been proposed that prominences play an important role as return flows of the chromosphere-corona mass cycle, in which hot plasma is transported upward in forms of spicules and prominence bubbles (likely due to flux emergence), while cool plasma drains downward in forms of vertical prominence threads (Berger et al. 2011 Nature). A critical step in this cycle is the condensation of the million-degree coronal plasma into T<10,000 K prominence material by a radiative cooling instability (i.e., thermal non-equilibrium), as numerically simulated (Karpen & Antiochos 2008; Xia et al. 2012) and first evidenced in recent SDO/AIA observations (Liu et al. 2012; Berger et al. 2012 ApJL). Such a runaway cooling process occurs in coronal loops of various sizes and generally leads to condensation at magnetic dips and formation of funnel-shaped prominences. A moderate-sized prominence can drain a significant mass of typically 10^15 gram/day, which is comparable to the mass of a CME or a fraction of the entire corona. Here we present a survey of funnel prominences that appear to be common in AIA observations at various locations and times. We find longer cooling times in longer/taller coronal loops whose densities are lower, consistent with the expected quadratic dependence on density of the optically-thin radiative loss. We propose that such funnel prominences, usually small in size, can constitute a new type of prominences, and similar processes can produce elementary building blocks of large-scale quiescent prominences in filament channels. This picture is supported by the recent theoretical development on spontaneous formation of current sheets and condensations manifested as prominence threads (Low et al. 2012a, b, ApJ). Title: 10Be Production in the Atmosphere by Galactic Cosmic Rays Authors: Matthiä, Daniel; Herbst, Klaudia; Heber, Bernd; Berger, Thomas; Reitz, Günther Bibcode: 2013SSRv..176..333M Altcode: 2011SSRv..tmp..290M Galactic cosmic ray nuclei and energetic protons produced in solar flares and accelerated by coronal mass ejections are the main sources of high-energy particles of extraterrestrial origin in near-Earth space and inside the Earth's atmosphere. The intensity of galactic cosmic rays inside the heliosphere is strongly influenced by the modulation of the interstellar source particles on their way through interplanetary space. Among others, this modulation depends on the activity of the Sun, and the resulting intensity of the energetic particles in the atmosphere is an indicator of the solar activity. Therefore, rare isotopes found in historical archives and produced by spallation reactions of primary and secondary hadrons of cosmic origin in the atmosphere, so-called cosmogenic nuclides, can be used to reconstruct the solar activity in the past. The production rate of 10Be, one of the cosmogenic nuclides most adequate to study the solar activity, is presented showing its variations with geographic latitude and altitude and the dependence on different production cross-sections present in literature. In addition, estimates for altitude integrated production rates of 10Be at different locations since the early nineteen sixties are shown. Title: The Advanced Technology Solar Telescope: Science Drivers and Construction Status Authors: Rimmele, Thomas; Berger, Thomas; McMullin, Joseph; Keil, Stephen; Goode, Phil; Knoelker, Michael; Kuhn, Jeff; Rosner, Robert; Casini, Roberto; Lin, Haosheng; Woeger, Friedrich; von der Luehe, Oskar; Tritschler, Alexandra; Atst Team Bibcode: 2013EGUGA..15.6305R Altcode: The 4-meter Advance Technology Solar Telescope (ATST) currently under construction on the 3000 meter peak of Haleakala on Maui, Hawaii will be the world's most powerful solar telescope and the leading ground-based resource for studying solar magnetism. The solar atmosphere is permeated by a 'magnetic carpet' that constantly reweaves itself to control solar irradiance and its effects on Earth's climate, the solar wind, and space weather phenomena such as flares and coronal mass ejections. Precise measurement of solar magnetic fields requires a large-aperture solar telescope capable of resolving a few tens of kilometers on the solar surface. With its 4 meter aperture, the ATST will for the first time resolve magnetic structure at the intrinsic scales of plasma convection and turbulence. The ATST's ability to perform accurate and precise spectroscopic and polarimetric measurements of magnetic fields in all layers of the solar atmosphere, including accurate mapping of the elusive coronal magnetic fields, will be transformative in advancing our understanding of the magnetic solar atmosphere. The ATST will utilize the Sun as an important astro- and plasma-physics "laboratory" demonstrating key aspects of omnipresent cosmic magnetic fields. The ATST construction effort is led by the US National Solar Observatory. State-of-the-art instrumentation will be constructed by US and international partner institutions. The technical challenges the ATST is facing are numerous and include the design of the off-axis main telescope, the development of a high order adaptive optics system that delivers a corrected beam to the instrument laboratory, effective handling of the solar heat load on optical and structural elements, and minimizing scattered light to enable observations of the faint corona. The ATST project has transitioned from design and development to its construction phase. The project has awarded design and fabrication contracts for major telescope subsystems. Site construction has commenced following the successful conclusion of the site permitting process. Science goals and construction status of telescope and instrument systems will be discussed. Title: Comparison of solar horizontal velocity fields from SDO/HMI and Hinode data Authors: Roudier, Th.; Rieutord, M.; Prat, V.; Malherbe, J. M.; Renon, N.; Frank, Z.; Švanda, M.; Berger, T.; Burston, R.; Gizon, L. Bibcode: 2013A&A...552A.113R Altcode: 2013arXiv1303.4271R Context. The measurement of the Sun's surface motions with a high spatial and temporal resolution is still a challenge.
Aims: We wish to validate horizontal velocity measurements all over the visible disk of the Sun from Solar Dynamics Observatory/ Helioseismic and Magnetic Imager (SDO/HMI) data.
Methods: Horizontal velocity fields are measured by following the proper motions of solar granules using a newly developed version of the coherent structure tracking (CST) code. The comparison of the surface flows measured at high spatial resolution (Hinode, 0.1 arcsec) and low resolution (SDO/HMI, 0.5 arcsec) allows us to determine corrections to be applied to the horizontal velocity measured from HMI white light data.
Results: We derive horizontal velocity maps with spatial and temporal resolutions of respectively 2.5 Mm and 30 min. From the two components of the horizontal velocity vx and vy measured in the sky plane and the simultaneous line of sight component from SDO/HMI dopplergrams vD, we derive the spherical velocity components (vr, vθ, vϕ). The azimuthal component vϕ gives the solar differential rotation with a high precision (± 0.037 km s-1) from a temporal sequence of only three hours.
Conclusions: By following the proper motions of the solar granules, we can revisit the dynamics of the solar surface at high spatial and temporal resolutions from hours to months and years with the SDO data. Title: Simulations of the Dynamics of the Magnetic Rayleigh-Taylor Instability in Solar Prominences Authors: Hillier, A.; Berger, T.; Shibata, K.; Isobe, H. Bibcode: 2013ASPC..474..147H Altcode: The magnetic Rayleigh-Taylor instability plays an important role in the mass and magnetic flux transport in many astrophysical bodies. Solar prominences also display this instability and recent observations using the Solar Optical Telescope onboard the Hinode satellite have revealed these dynamics in amazing detail. The observations show rising plumes, approximately 1 Mm in width, that propagate through the dense prominence material from low-density bubbles, i.e. the situation expected when the magnetic Rayleigh-Taylor instability occurs. To study this phenomenon, we performed 3D simulations of the magnetic Rayleigh-Taylor instability in the Kippenhahn-Schlüter prominence model. The plumes formed in these simulations are filamentary structures that are aligned with the magnetic field created as 3D modes of the magnetic Rayleigh-Taylor instability. The plumes rise, developing large structures from smaller structures through an inverse cascade process driven by nonlinear interaction. The results suggest that the plumes observed in the prominence may be used to study the conditions inside the prominence. Title: How Galactic Cosmic Ray models affect the estimation of radiation exposure in space Authors: Mrigakshi, Alankrita Isha; Matthiä, Daniel; Berger, Thomas; Reitz, Günther; Wimmer-Schweingruber, Robert F. Bibcode: 2013AdSpR..51..825M Altcode: The radiation environment in space is a major concern for human spaceflight because of the adverse effects of high levels of radiation on astronauts' health. Therefore, it is essential to perform radiation risk assessments already during the concept studies of a manned mission. Galactic Cosmic Rays (GCR) have been identified to be one of the primary sources of radiation exposure in space.This work presents an evaluation of the radiation exposure caused by GCR between 1970 and 2011 in near-Earth interplanetary space and at the orbit of the International Space Station (ISS) by making numerical simulations with the Monte-Carlo framework GEANT4. Commonly used GCR models - CREME96, CREME2009 and Badhwar-O'Neill2010 are used to describe the GCR spectra and the differences arising from the application of these different models in terms of absorbed dose and dose equivalent rates are investigated. Additionally, the depth distribution of the dose quantities and the relative contribution of particles with different energies to the total exposure during solar maximum and minimum conditions are studied.The differences in the spectra, described by the models, result in considerable differences in the estimation of the radiation exposure. Title: A ready-to-use galactic cosmic ray model Authors: Matthiä, Daniel; Berger, Thomas; Mrigakshi, Alankrita I.; Reitz, Günther Bibcode: 2013AdSpR..51..329M Altcode: Galactic cosmic ray nuclei close to Earth are of great importance in different fields of research. By studying their intensity in near-Earth interplanetary space and modeling their modulation in the heliosphere it is possible to gain knowledge both about the structure of the heliosphere and the transport processes within. Additionally, secondary phenomena like cloud formation, ionization processes in the atmosphere, cosmogenic nuclide production and radiation exposure in space and at aviation altitudes are related to the intensity of the galactic cosmic rays and their modulation in the heliosphere. In order to improve the knowledge about these processes and underlying mechanisms it is often beneficial to perform numerical simulations. A necessary prerequisite for such simulations is a model describing the galactic cosmic ray intensities for all particle types and energies of importance. Several of these models exist in the literature. However, many of these do not provide essential characteristics like the description of heavier nuclei or it is difficult to associate them to recent or actual solar modulation conditions. In this work a model is presented which describes the galactic cosmic ray spectra of nuclei based on a single parameter. The values of this parameter for different solar modulation conditions are derived from measurements of the Advanced Composition Explorer (ACE) spacecraft and Oulu neutron monitor count rates. Comparing the galactic cosmic ray spectra predicted by the model to a comprehensive set of experimental data from literature shows very good agreement. Title: GRB 130605A: continued Skynet/PROMPT observations. Authors: Trotter, A.; Lacluyze, A.; Reichart, D.; Haislip, J.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Frank, N.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14778....1T Altcode: 2013GCN..14778...1T No abstract at ADS Title: GRB 130514A: Skynet/PROMPT/DSO detections. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; Smith, A.; Caton, D.; Hawkins, L.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.14648....1T Altcode: 2013GCN..14648...1T No abstract at ADS Title: GRB 130912A: skynet DSO-14/Yerkes-41/PROMPT-CTIO observations. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; Smith, A. B.; Caton, D.; Hawkins, L.; Hoette, V.; Cudworth, K.; Harper, D.; Kron, R.; Linder, T.; Russell, R.; Struble, E.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Crain, J. A. Bibcode: 2013GCN.15218....1T Altcode: 2013GCN..15218...1T No abstract at ADS Title: GRB 131117A: skynet PROMPT optical detection of an afterglow. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Frank, N.; Lacluyze, A.; Moore, J.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Ivarsen, K.; Maples, M.; Nysewander, M.; Crain, J. A. Bibcode: 2013GCN.15491....1T Altcode: 2013GCN..15491...1T No abstract at ADS Title: GRB 130831A: continued Skynet/PROMPT-SSO, PROMPT-CTIO and Yerkes-41 detections. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Moore, J.; Frank, N.; Hoette, V.; Harper, D.; Kron, R.; Cudworth, K.; Struble, E.; Russell, R.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Ivarsen, K.; Maples, M.; Nysewander, M.; Crain, J. A. Bibcode: 2013GCN.15164....1T Altcode: 2013GCN..15164...1T No abstract at ADS Title: On MATROSHKA / DOSTEL Data Interpretation Authors: Labrenz, Johannes; Berger, Thomas; Burmeister, Soenke; Heber, Bernd; Reitz, Guenther Bibcode: 2013ICRC...33.2302L Altcode: MATROSHKA (MTR) is an ESA experiment facility under the science and project lead of DLR Cologne. The radiation exposure inside a human phantom is measured by active and passive radiation detectors. The DOSimetry TELescope (DOSTEL), built at CAU Kiel in cooperation with DLR Cologne, is a particle telescope consisting of two Si-semiconductor detectors. Count rates as well as energy deposition spectra are measured by this instrument. The DOSTEL was operating during the first MATROSHKA mission phase (MTR-1) where the phantom was mounted outside the Zvezda module (Service Module SM) of the ISS from Feb. 2004 to Aug. 2005. The DOSTEL count rate measurements showed the expected dependence on the geomagnetic vertical cutoff rigidity (Rc). In this work a time correction method for the DOSTEL data using this Rc dependence will be presented. Title: GRB 130521A: Skynet/PROMPT observations. Authors: James, D.; Foster, C.; Taylor, P.; Carroll, M.; Trotter, A.; Reichart, D.; Lacluyze, A.; Haislip, J.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.14697....1J Altcode: 2013GCN..14697...1J No abstract at ADS Title: GRB 130615A: continued Skynet/PROMPT observations. Authors: Frank, N.; Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14909....1F Altcode: 2013GCN..14909...1F No abstract at ADS Title: The Calibration of the Flight Radiation Environment Detector (FRED) Authors: Möller, T.; Berger, T.; Böttcher, S.; Burmeister, S.; Ehresmann, B.; Heber, B.; Labrenz, J.; Panitzsch, L.; Wimmer-Schweingruber, R. F. Bibcode: 2013ICRC...33.1977M Altcode: The mixed radiation field in the Earth's atmosphere is caused by the interaction of cosmic and trapped radiation with the atmosphere. A plethora of secondary particles is created which, together with the primary radiation, creates this complex natural mixed radiation field. Apart from charged particles (predominantly protons, electrons, muons, pions, and alpha particles)), it also contains neutral particles, i.e., neutrons and gamma rays, which are generally difficult to measure. The Flight Radiation Environment Detector (FRED) was designed to measure quantitatively the contributions of the charged and neutral components. It consists of four segmented silicon solid-state detectors which form a particle telescope and also form an efficient anti-coincidence to separate the neutral radiation. Thus FRED is also designed to measure the respective dose rate from charged and neutral particles. Here we present the general design of FRED and the results of a calibration campaign at the Heavy Ion Medical Accelerator in Chiba (HIMAC) facility at the National Institute of Radiological Sciences (NIRS), Japan. Title: GRB 130907A: skynet DSO-14/Yerkes-41/GORT confirmation of a fading afterglow. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; McLin, K.; Cominsky, L.; Smith, A. B.; Caton, D.; Hawkins, L.; Hoette, V.; Cudworth, K.; Harper, D.; Kron, R.; Linder, T.; Russell, R.; Struble, E.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Crain, J. A. Bibcode: 2013GCN.15193....1T Altcode: 2013GCN..15193...1T No abstract at ADS Title: GRB 130420A: continued Skynet/GORT Observations/Detections. Authors: Trotter, A.; Frank, N.; Lacluyze, A.; Reichart, D.; McLin, K.; Cominsky, L.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Haislip, J.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.14445....1T Altcode: 2013GCN..14445...1T No abstract at ADS Title: Skynet/GORT observations of GRB130420A. Authors: Trotter, A.; Frank, N.; Lacluyze, A.; Reichart, D.; McLin, K.; Cominsky, L.; Berger, T.; Crain, J. A.; Cromartie, H. T.; Egger, R.; Foster, A.; Haislip, J.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E. Bibcode: 2013GCN.14427....1T Altcode: 2013GCN..14427...1T No abstract at ADS Title: GRB 130612A: Skynet/PROMPT detection of the optical afterglow. Authors: Trotter, A.; Hailslip, J.; Reichart, D.; Lacluyze, A.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Frank, N.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14877....1T Altcode: 2013GCN..14877...1T No abstract at ADS Title: GRB 130427A: skynet detections of a possible supernova. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; McLin, K.; Cominsky, L.; Smith, A.; Caton, D.; Hawkins, L.; Holmes, B.; Linder, T.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.14662....1T Altcode: 2013GCN..14662...1T No abstract at ADS Title: GRB 130427A: ten nights of Skynet/PROMPT/GORT observations. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; McLin, K.; Cominsky, L.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.14608....1T Altcode: 2013GCN..14608...1T No abstract at ADS Title: GRB 130427A: Skynet/PROMPT observations. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.14497....1T Altcode: 2013GCN..14497...1T No abstract at ADS Title: GRB 130606A: continued Skynet/PROMPT observations. Authors: Trotter, A.; Lacluyze, A.; Reichart, D.; Haislip, J.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Frank, N.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14826....1T Altcode: 2013GCN..14826...1T No abstract at ADS Title: GRB 130615A: Skynet/PROMPT observations. Authors: Frank, N.; Trotter, A.; Haislip, J.; Reichart, D.; Lacluyze, A.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14901....1F Altcode: 2013GCN..14901...1F No abstract at ADS Title: GRB 130521A: Skynet/PROMPT detection of an extremely red afterglow. Authors: James, D.; Foster, C.; Taylor, P.; Carroll, M.; Trotter, A.; Reichart, D.; Lacluyze, A.; Haislip, J.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.14713....1J Altcode: 2013GCN..14713...1J No abstract at ADS Title: GRB 130610A: Skynet/PROMPT detection of the optical afterglow. Authors: Trotter, A.; Haislip, J.; Lacluyze, A.; Reichart, D.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14844....1T Altcode: 2013GCN..14844...1T No abstract at ADS Title: GRB 130919A: skynet PROMPT-CTIO optical upper limits. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; Moore, J.; Frank, N.; Ivarsen, K.; Nysewander, M.; Foster, A.; Berger, T.; Cromartie, H. T.; Egger, R.; Maples, M.; Crain, J. A. Bibcode: 2013GCN.15235....1T Altcode: 2013GCN..15235...1T No abstract at ADS Title: GRB 130907A: skynet DSO-14/Yerkes-41 detections of a possible afterglow. Authors: Trotter, A.; Haislip, J.; Lacluyze, A.; Moore, J.; Frank, N.; Reichart, D.; Smith, A.; Caton, D.; Hawkins, L.; Hoette, V.; Harper, D.; Kron, R.; Cudworth, K.; Struble, E.; Russell, R.; Linder, T.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Ivarsen, K.; Maples, M.; Nysewander, M.; Crain, J. A. Bibcode: 2013GCN.15191....1T Altcode: 2013GCN..15191...1T No abstract at ADS Title: GRB 131024A: skynet R-COP optical observations. Authors: Trotter, A.; Haislip, J.; Reichart, D.; Verveer, A.; Spuck, T.; Lacluyze, A.; Frank, N.; Moore, J.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Ivarsen, K.; Maples, M.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.15369....1T Altcode: 2013GCN..15369...1T No abstract at ADS Title: GRB 130606A: Skynet/PROMPT detection of the optical afterglow. Authors: Trotter, A.; Lacluyze, A.; Reichart, D.; Haislip, J.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Frank, N.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14815....1T Altcode: 2013GCN..14815...1T No abstract at ADS Title: GRB 131004A: skynet PROMPT/DSO-14 upper limits. Authors: Frank, N.; Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; Smith, A.; Caton, D.; Hawkins, L.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.15317....1F Altcode: 2013GCN..15317...1F No abstract at ADS Title: GRB 130719A: Skynet/PROMPT observations. Authors: Trotter, A.; Reichart, D.; Lacluyze, A.; Haislip, J.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Frank, N.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.15030....1T Altcode: 2013GCN..15030...1T No abstract at ADS Title: GRB 130605A: Skynet/PROMPT detection of a fading afterglow. Authors: Trotter, A.; Lacluyze, A.; Reichart, D.; Haislip, J.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Frank, N.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14776....1T Altcode: 2013GCN..14776...1T No abstract at ADS Title: GRB 130831A: Skynet/PROMPT-SSO detections. Authors: Trotter, A.; Haislip, J.; Lacluyze, A.; Moore, J.; Frank, N.; Reichart, D.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Ivarsen, K.; Maples, M.; Nysewander, M.; Crain, J. A. Bibcode: 2013GCN.15148....1T Altcode: 2013GCN..15148...1T No abstract at ADS Title: GRB 130427A: continued Skynet/PROMPT observations. Authors: Trotter, A.; Reichart, D.; Haislip, J.; Lacluyze, A.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Frank, N.; Ivarsen, K.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Crain, J. A. Bibcode: 2013GCN.14510....1T Altcode: 2013GCN..14510...1T No abstract at ADS Title: GRB 130612A: continued Skynet/PROMPT/GORT/DSO observations. Authors: Carroll, M.; Trotter, A.; Hailslip, J.; Reichart, D.; Lacluyze, A.; McLin, K.; Cominsky, L.; Smith, A.; Caton, D.; Hawkins, L.; Berger, T.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Frank, N.; Ivarsen, K.; James, D.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.14914....1C Altcode: 2013GCN..14914...1C No abstract at ADS Title: GRB 130722A: Skynet/GORT observations. Authors: Trotter, A.; Reichart, D.; McLin, K.; Cominsky, L.; Berger, T.; Carroll, M.; Cromartie, H. T.; Egger, R.; Foster, A.; Foster, C.; Frank, N.; Haislip, J.; Ivarsen, K.; James, D.; Lacluyze, A.; Maples, M.; Moore, J.; Nysewander, M.; Speckhard, E.; Taylor, P.; Crain, J. A. Bibcode: 2013GCN.15017....1T Altcode: 2013GCN..15017...1T No abstract at ADS Title: The Prominence/Coronal Cavity System: A Unified View of Magnetic Structures in the Solar Corona Authors: Berger, T. Bibcode: 2012ASPC..463..147B Altcode: Hinode/SOT and SDO/AIA movies have given us new insights into the dynamic connections between prominences and coronal cavities. The observations suggest that prominences and coronal cavities are elements of a single large-scale structure in the solar corona: a helical magnetic flux rope. We discuss supporting observational evidence such as the relationship between the so-called “prominence bubbles” discovered by Hinode/SOT and coronal cavities, as well as spiral flows in the central regions of coronal cavities observed by AIA. We hypothesize that coronal cavity flux ropes support a form of magneto-thermal convection in which hot plasma and magnetic flux are transported upward into the coronal cavity flux rope with subsequent radiative cooling and condensation forming the partially ionized prominence return flows seen in visible light observations. Understanding the mass, magnetic flux, and helicity transport of this complex system will lead to better understanding of quiet Sun coronal mass ejections (CMEs). Title: Radiation exposure in the moon environment Authors: Reitz, Guenther; Berger, Thomas; Matthiae, Daniel Bibcode: 2012P&SS...74...78R Altcode: During a stay on the moon humans are exposed to elevated radiation levels due to the lack of substantial atmospheric and magnetic shielding compared to the Earth's surface. The absence of magnetic and atmospheric shielding allows cosmic rays of all energies to impinge on the lunar surface. Beside the continuous exposure to galactic cosmic rays (GCR), which increases the risk of cancer mortality, exposure through particles emitted in sudden nonpredictable solar particle events (SPE) may occur. SPEs show an enormous variability in particle flux and energy spectra and have the potential to expose space crew to life threatening doses. On Earth, the contribution to the annual terrestrial dose of natural ionizing radiation of 2.4 mSv by cosmic radiation is about 1/6, whereas the annual exposure caused by GCR on the lunar surface is roughly 380 mSv (solar minimum) and 110 mSv (solar maximum). The analysis of worst case scenarios has indicated that SPE may lead to an exposure of about 1 Sv. The only efficient measure to reduce radiation exposure is the provision of radiation shelters. Measurements on the lunar surface performed during the Apollo missions cover only a small energy band for thermal neutrons and are not sufficient to estimate the exposure. Very recently some data were added by the Radiation Dose Monitoring (RADOM) instrument operated during the Indian Chandrayaan Mission and the Cosmic Ray Telescope (CRaTER) instrument of the NASA LRO (Lunar Reconnaisance Orbiter) mission. These measurements need to be complemented by surface measurements. Models and simulations that exist describe the approximate radiation exposure in space and on the lunar surface. The knowledge on the radiation exposure at the lunar surface is exclusively based on calculations applying radiation transport codes in combination with environmental models. Own calculations are presented using Monte-Carlo simulations to calculate the radiation environment on the moon and organ doses on the surface of the moon for an astronaut in an EVA suit and are compared with measurements. Since it is necessary to verify/validate such calculations with measurement on the lunar surface, a description is given of a radiation detector for future detailed surface measurements. This device is proposed for the ESA Lunar Lander Mission and is capable to characterize the radiation field concerning particle fluencies, dose rates and energy transfer spectra for ionizing particles and to measure the dose contribution of secondary neutrons. Title: The Mobile Dosimetric Telescope - A Small Size Active Personal Dosimeter for Application at High Altitudes and Onboard the International Space Station Authors: Ritter, B.; Marsalek, K.; Berger, T.; Burmeister, S.; Reitz, G.; Heber, B. Bibcode: 2012AGUFMSM23B2308R Altcode: The radiation environment at cruising altitudes, as well as in Low Earth Orbit - like on the International Space Station - differs significantly from the natural radiation environment on Earth. Especially in Low Earth Orbit it poses one of the main health risks for long duration human missions. Therefore, it is essential to monitor the properties of the radiation field in such environments. The Mobile Dosimetric Telescope MDT, is a small size battery driven personal dosimeter based on silicon detector technology that has been developed to observe absorbed dose and dose rate in real time. Two silicon diodes are arranged in a telescope configuration, which allows the measurement of the ionizing constituents of the radiation field and partially the neutral contribution to the dose. The absorbed dose is obtained by considering every particle in either of the detectors. Particles traversing both diodes are detected as coincidence events that enable to derive linear energy transfer (LET) spectra. From these the quality factor of the field is determined, which is necessary for the estimation of the dose equivalent. The detection range of the device covers energy depositions from minimal ionizing particles up to relativistic heavy ions. Calibrations of the detector system have been performed with various radioactive sources and with heavy ions at the Heavy Ion Medical Accelerator (HIMAC) facility at the National Institute for Radiological Sciences (NIRS) in Chiba, Japan. Additionally, the MDT has been successfully tested onboard aircraft. The results of these measurements are in good agreement with those from other radiation detectors. The presentation will focus on data taken during long haul flights in the northern hemisphere. Title: 2nd ATST-EAST Workshop in Solar Physics: Magnetic Fields from the Photosphere to the Corona Authors: Rimmele, T. R.; Tritschler, A.; Wöger, F.; Collados Vera, M.; Socas-Navarro, H.; Schlichenmaier, R.; Carlsson, M.; Berger, T.; Cadavid, A.; Gilbert, P. R.; Goode, P. R.; Knölker, M. Bibcode: 2012ASPC..463.....R Altcode: No abstract at ADS Title: Assessment of Galactic Cosmic Ray Models and Implications on the Estimation of Radiation Exposure in Space Authors: Mrigakshi, A. I.; Matthiä, D.; Berger, T.; Reitz, G.; Wimmer-Schweingruber, R. F. Bibcode: 2012AGUFMSM23B2309M Altcode: Astronauts are subjected to elevated levels of high-energy ionizing radiation in space which poses a substantial risk to their health. Therefore, the assessment of the radiation exposure for long duration manned spaceflight is essential. This is done by measuring dose using various detector techniques and by performing numerical simulations utilizing radiation transport codes which allow to predict radiation exposure for future missions and for conditions where measurements are not feasible or available. A necessary prerequisite for an accurate estimation of the exposure using the latter approach is a reliable description of the radiation spectra. Accordingly, in order to estimate the exposure from the Galactic Cosmic Rays (GCRs), which are one of the major sources of radiation exposure in space, GCR models are required. This work presents an evaluation of GCR models for dosimetry purposes and the effect of applying these models on the estimation of GCR exposure in space outside and inside the Earth's magnetosphere. To achieve this, widely used GCR models - Badhwar-O'Neill2010, Burger-Usoskin, CREME2009 and CREME96, were evaluated by comparing model spectra for light and heavy nuclei with measurements from various high-altitude balloon and space missions over several decades. Additionally a new model, based on the GCR-ISO model, developed at the German Aerospace Centre (DLR) was also investigated. The differences arising in the radiation exposure by applying these models are quantified in terms of absorbed dose and dose equivalent rates that were estimated numerically using the GEANT4 Monte-Carlo framework. During certain epochs in the last decade, there are large discrepancies between the model and the measured spectra. All models exhibit weaknesses in describing the increased GCR flux that was observed in 2009-2010. The differences in the spectra, described by the models, result in considerable differences in the estimated dose quantities. Title: Supporting Mars exploration: BIOMEX in Low Earth Orbit and further astrobiological studies on the Moon using Raman and PanCam technology Authors: de Vera, Jean-Pierre; Boettger, Ute; Noetzel, Rosa de la Torre; Sánchez, Francisco J.; Grunow, Dana; Schmitz, Nicole; Lange, Caroline; Hübers, Heinz-Wilhelm; Billi, Daniela; Baqué, Mickael; Rettberg, Petra; Rabbow, Elke; Reitz, Günther; Berger, Thomas; Möller, Ralf; Bohmeier, Maria; Horneck, Gerda; Westall, Frances; Jänchen, Jochen; Fritz, Jörg; Meyer, Cornelia; Onofri, Silvano; Selbmann, Laura; Zucconi, Laura; Kozyrovska, Natalia; Leya, Thomas; Foing, Bernard; Demets, René; Cockell, Charles S.; Bryce, Casey; Wagner, Dirk; Serrano, Paloma; Edwards, Howell G. M.; Joshi, Jasmin; Huwe, Björn; Ehrenfreund, Pascale; Elsaesser, Andreas; Ott, Sieglinde; Meessen, Joachim; Feyh, Nina; Szewzyk, Ulrich; Jaumann, Ralf; Spohn, Tilman Bibcode: 2012P&SS...74..103D Altcode: The Low Earth Orbit (LEO) experiment Biology and Mars Experiment (BIOMEX) is an interdisciplinary and international space research project selected by ESA. The experiment will be accommodated on the space exposure facility EXPOSE-R2 on the International Space Station (ISS) and is foreseen to be launched in 2013. The prime objective of BIOMEX is to measure to what extent biomolecules, such as pigments and cellular components, are resistant to and able to maintain their stability under space and Mars-like conditions. The results of BIOMEX will be relevant for space proven biosignature definition and for building a biosignature data base (e.g. the proposed creation of an international Raman library). The library will be highly relevant for future space missions such as the search for life on Mars. The secondary scientific objective is to analyze to what extent terrestrial extremophiles are able to survive in space and to determine which interactions between biological samples and selected minerals (including terrestrial, Moon- and Mars analogs) can be observed under space and Mars-like conditions. In this context, the Moon will be an additional platform for performing similar experiments with negligible magnetic shielding and higher solar and galactic irradiation compared to LEO. Using the Moon as an additional astrobiological exposure platform to complement ongoing astrobiological LEO investigations could thus enhance the chances of detecting organic traces of life on Mars. We present a lunar lander mission with two related objectives: a lunar lander equipped with Raman and PanCam instruments which can analyze the lunar surface and survey an astrobiological exposure platform. This dual use of testing mission technology together with geo- and astrobiological analyses will significantly increase the science return, and support the human preparation objectives. It will provide knowledge about the Moon's surface itself and, in addition, monitor the stability of life-markers, such as cells, cell components and pigments, in an extraterrestrial environment with much closer radiation properties to the surface of Mars. The combination of a Raman data base of these data together with data from LEO and space simulation experiments, will lead to further progress on the analysis and interpretation of data that we will obtain from future Moon and Mars exploration missions. Title: Science with Large Solar Telescopes: Addressing Key Science Questions with New Observing Modes Authors: Berger, T. Bibcode: 2012IAUSS...6E.201B Altcode: We review the capabilities of existing and future large solar telescopes with an emphasis on the key science questions that these instruments must address. Large solar telescopes coming online now, as well as the 4-meter ATST coming online in 2018 are tasked with extending high resolution and polarimetric investigations from the lower atmospheric regions into the higher regions and connecting the dynamics between the two. The overall goal is to understand the interaction of flows and magnetic fields in the convection zone down to O(10) km scales and the magnetohydrodynamic transport, storage, and release of energy in the upper atmosphere leading to coronal heating and eruptive events. The ATST in particular will have unique opportunities to address this goal with new observations of the infrared atmosphere at very high spatial resolution and with coronagraphic capabilities. We discuss some of the multi-instrument ATST observing programs that will investigate such topics as small-scale magnetoconvection and energetic events in the lower atmosphere and energy release in filament eruptions. Title: SDO/AIA Detection of Solar Prominence Formation within a Coronal Cavity Authors: Berger, Thomas E.; Liu, Wei; Low, B. C. Bibcode: 2012ApJ...758L..37B Altcode: 2012arXiv1208.3431B We report the first analyses of SDO/AIA observations of the formation of a quiescent polar crown prominence in a coronal cavity. The He II 304 Å (log T max ~ 4.8 K) data show both the gradual disappearance of the prominence due to vertical drainage and lateral transport of plasma followed by the formation of a new prominence 12 hr later. The formation is preceded by the appearance of a bright emission "cloud" in the central region of the coronal cavity. The peak brightness of the cloud progressively shifts in time from the Fe XIV 211 Å channel, through the Fe XII 193 Å channel, to the Fe IX 171 Å channel (log T max ~ 6.2, 6.1, 5.8 K, respectively) while simultaneously decreasing in altitude. Filter ratio analysis estimates the initial temperature of the cloud to be approximately log T ~ 6.25 K with evidence of cooling over time. The subsequent growth of the prominence is accompanied by darkening of the cavity in the 211 Å channel. The observations imply prominence formation via in situ condensation of hot plasma from the coronal cavity, in support of our previously proposed process of magnetothermal convection in coronal magnetic flux ropes. Title: Numerical Simulations of the Magnetic Rayleigh-Taylor Instability in the Kippenhahn-Schlüter Prominence Model. II. Reconnection-triggered Downflows Authors: Hillier, Andrew; Isobe, Hiroaki; Shibata, Kazunari; Berger, Thomas Bibcode: 2012ApJ...756..110H Altcode: 2011arXiv1106.2613H The launch of the Hinode satellite has allowed high-resolution observations of supersonic bright downflows in quiescent prominences, known as prominence knots. We present observations in the Ca II H spectral line using the Solar Optical Telescope on board the Hinode satellite of a descending plasma knot of size ~900 km. The knot initially undergoes ballistic motion before undergoing impulsive accelerations at the same time as experiencing increases in intensity. We also present a subset of our three-dimensional magnetohydrodynamic simulations, performed to investigate the nonlinear stability of the Kippenhahn-Shlüter prominence model to the magnetic Rayleigh-Taylor instability in which interchange reconnection occurs. The interchange reconnection in the model breaks the force balance along the field lines which initiates the downflows. The downflows propagate with a downward fluid velocity of ~15 km s-1 and a characteristic size of ~700 km. We conclude that the observed plasma blob and the simulated downflow are driven by the breaking of the force balance along the magnetic field as a result of a change in magnetic topology caused by reconnection of the magnetic field. Title: The interface region imaging spectrograph for the IRIS Small Explorer mission Authors: Wülser, Jean-Pierre; Title, Alan M.; Lemen, James R.; De Pontieu, Bart; Kankelborg, Charles C.; Tarbell, Theodore D.; Berger, Thomas E.; Golub, Leon; Kushner, Gary D.; Chou, Catherine Y.; Weingrod, Isaac; Holmes, Buck; Mudge, Jason; Podgorski, William A. Bibcode: 2012SPIE.8443E..08W Altcode: The Interface Region Imaging Spectrograph (IRIS) is a NASA SMall EXplorer mission scheduled for launch in January 2013. The primary goal of IRIS is to understand how the solar atmosphere is energized. The IRIS investigation combines advanced numerical modeling with a high resolution UV imaging spectrograph. IRIS will obtain UV spectra and images with high resolution in space (0.4 arcsec) and time (1s) focused on the chromosphere and transition region of the Sun, a complex interface region between the photosphere and corona. The IRIS instrument uses a Cassegrain telescope to feed a dual spectrograph and slit-jaw imager that operate in the 133-141 nm and 278-283 nm ranges. This paper describes the instrument with emphasis on the imaging spectrograph, and presents an initial performance assessment from ground test results. Title: The Hydromagnetic Interior of a Solar Quiescent Prominence. II. Magnetic Discontinuities and Cross-field Mass Transport Authors: Low, B. C.; Liu, W.; Berger, T.; Casini, R. Bibcode: 2012ApJ...757...21L Altcode: This second paper of the series investigates the transverse response of a magnetic field to the independent relaxation of its flux tubes of fluid seeking hydrostatic and energy balance, under the frozen-in condition and suppression of cross-field thermal conduction. The temperature, density, and pressure naturally develop discontinuities across the magnetic flux surfaces separating the tubes, requiring the finite pressure jumps to be compensated by magnetic-pressure jumps in cross-field force balance. The tangentially discontinuous fields are due to discrete currents in these surfaces, δ-function singularities in the current density that are fully admissible under the rigorous frozen-in condition but must dissipate resistively if the electrical conductivity is high but finite. The magnetic field and fluid must thus endlessly evolve by this spontaneous formation and resistive dissipation of discrete currents taking place intermittently in spacetime, even in a low-β environment. This is a multi-dimensional effect in which the field plays a central role suppressed in the one-dimensional (1D) slab model of the first paper. The study begins with an order-of-magnitude demonstration that of the weak resistive and cross-field thermal diffusivities in the corona, the latter is significantly weaker for small β. This case for spontaneous discrete currents, as an important example of the general theory of Parker, is illustrated with an analysis of singularity formation in three families of two-dimensional generalizations of the 1D slab model. The physical picture emerging completes the hypothesis formulated in Paper I that this intermittent process is the origin of the dynamic interiors of a class of quiescent prominences revealed by recent Hinode/SOT and SDO/AIA high-resolution observations. Title: Quiescent Prominence Dynamics: An Update on Hinode/SOT Discoveries Authors: Berger, T. Bibcode: 2012ASPC..454...79B Altcode: Hinode/SOT has revealed two new flow systems in quiescent prominences: large-scale (order 10 Mm) “bubbles” or “arches” that “inflate” below prominences to create dark cavities in the prominence, and small-scale (order 1 Mm) dark plumes that rise with constant velocity to heights of 10-20 Mm above their origin at the base of prominences. Both flow systems are highly dynamic with ascent speeds ranging from 1-30 km s-1 and evidence in the small-scale plumes of Kelvin-Helmholtz instabilities and turbulent mixing. Neither flow system has been observed in active region prominences. Multi-instrument analysis of one typical cavity shows the column density to be at least a factor of 5 less than the overlying prominence plasma. We discuss the developing understanding of these flow systems in the context of a single formation mechanism: buoyancy instabilities in an emerging flux rope that interacts with the overlying prominence. Measurements of plume and bubble sizes and occurrence frequencies, combined with the column density finding, implies that these flows are a significant source of mass and magnetic flux for quiescent prominences and coronal cavities, respectively. Title: Plasma Instabilities in Quiescent Prominences Authors: Ryutova, M.; Berger, T.; Frank, Z.; Title, A.; Tarbell, T. Bibcode: 2012ASPC..454..143R Altcode: We study dynamics of quiescent prominences using several data sets taken with the SOT on Hinode. We find a number of processes occurring at different stages of the prominence evolution that are common for all the chosen cases, and having universal character, can be related to a fundamental plasma instabilities. We combine the observational evidence and theory to identify these instabilities. Here we discuss only two examples: (1) Coronal cavity formation under a prominence body and its evolution associated with screw pinch instability, and (2) Development of a regular series of plumes and spikes typical to the Rayleigh-Taylor instability modified by solenoidal magnetic field. Title: Simulations of Buoyant Plumes in Solar Prominences Authors: Hurlburt, N.; Berger, T. Bibcode: 2012ASPC..454..137H Altcode: 2012arXiv1201.4352H Observations of solar prominences reveal a complex, dynamic flow field within them. The flow field within quiescent prominences is characterized by long "threads" and dark "bubbles" that fall and rise (respectively) in a thin sheet. The flow field in active prominences display more helical motions that travel along the axis of the prominence. We explore the possible dynamics of both of these with the aid of 2.5D MHD simulations. Our model, compressible plasma possesses density and temperature gradients and resides in magnetic field configurations that mimc those of a solar prominence. We present results of various configurations and discuss the nonlinear behavior of the resulting dynamics. Title: The Hydromagnetic Interior of a Solar Quiescent Prominence. I. Coupling between Force Balance and Steady Energy Transport Authors: Low, B. C.; Berger, T.; Casini, R.; Liu, W. Bibcode: 2012ApJ...755...34L Altcode: 2012arXiv1203.1056L This series of papers investigates the dynamic interiors of quiescent prominences revealed by recent Hinode and SDO/AIA high-resolution observations. This first paper is a study of the static equilibrium of the Kippenhahn-Schlüter diffuse plasma slab, suspended vertically in a bowed magnetic field, under the frozen-in condition and subject to a theoretical thermal balance among an optically thin radiation, heating, and field-aligned thermal conduction. The everywhere-analytical solutions to this nonlinear problem are an extremely restricted subset of the physically admissible states of the system. For most values of the total mass frozen into a given bowed field, force balance and steady energy transport cannot both be met without a finite fraction of the total mass having collapsed into a cold sheet of zero thickness, within which the frozen-in condition must break down. An exact, resistive hydromagnetic extension of the Kippenhahn-Schlüter slab is also presented, resolving the mass-sheet singularity into a finite-thickness layer of steadily falling dense fluid. Our hydromagnetic result suggests that the narrow, vertical prominence Hα threads may be falling across magnetic fields, with optically thick cores much denser and ionized to much lower degrees than conventionally considered. This implication is discussed in relation to (1) the recent SDO/AIA observations of quiescent prominences that are massive and yet draining mass everywhere in their interiors, (2) the canonical range of 5-60 G determined from spectral polarimetric observations of prominence magnetic fields over the years, and (3) the need for a more realistic multi-fluid treatment. Title: Assessment of galactic cosmic ray models Authors: Mrigakshi, Alankrita Isha; Matthiä, Daniel; Berger, Thomas; Reitz, Günther; Wimmer-Schweingruber, Robert F. Bibcode: 2012JGRA..117.8109M Altcode: 2012JGRA..11708109M Among several factors involved in the development of a manned space mission concept, the astronauts' health is a major concern that needs to be considered carefully. Galactic cosmic rays (GCRs), which mainly consist of high-energetic nuclei ranging from hydrogen to iron and beyond, pose a major radiation health risk in long-term space missions. It is therefore required to assess the radiation exposure of astronauts in order to estimate their radiation risks. This can be done either by performing direct measurements or by making computer based simulations from which the dose can be derived. A necessary prerequisite for an accurate estimation of the exposure using simulations is a reliable description of the GCR spectra. The aim of this work is to compare GCR models and to test their applicability for the exposure assessment of astronauts. To achieve this, commonly used models capable of describing both light and heavy GCR particle spectra were evaluated by investigating the model spectra for various particles over several decades. The updated Badhwar-O'Neill model published in the year 2010, CREME2009 which uses the International Standard model for GCR, CREME96 and the Burger-Usoskin model were examined. Hydrogen, helium, oxygen and iron nuclei spectra calculated by the different models are compared with measurements from various high-altitude balloon and space-borne experiments. During certain epochs in the last decade, there are large discrepancies between the GCR energy spectra described by the models and the measurements. All the models exhibit weaknesses in describing the increased GCR flux that was observed in 2009-2010. Title: The Power Spectrum of the Solar Surface Flows from Hinode Data and First Observations with MOF/CALAS Pic-du-Midi Authors: Roudier, T.; Rieutord, M.; Rincon, F.; Malherbe, J. -M.; Brito, D.; Berger, T.; Frank, Z.; Parés, L.; Bourrec, E.; Beigbeder, F. Bibcode: 2012ASPC..454...47R Altcode: Many features of solar surface turbulence, like the supergranulation, are still poorly understood.We use long time series of images taken by the Solar Optical Telescope on board the Hinode satellite to determine the velocity fields. The dynamics in the subgranulation range can be investigated with unprecedented precision thanks to the absence of seeing effects and the use of the MTF of SOT for correcting the spectra. The first MOF/CALAS/Pic-du-Midi results are also shown. Title: Simulations of MATROSHKA experiment outside the ISS using PHITS Authors: Puchalska, M.; Sihver, L.; Sato, T.; Berger, T.; Reitz, G. Bibcode: 2012AdSpR..50..489P Altcode: The radiation environment at the altitude of the International Space Station (ISS) is substantially different than anything typically encountered on Earth in both the character of the radiation field and the significantly higher dose rates. Concerns about the biological effects on humans of this highly complex natural radiation field are increasing due to higher amount of astronauts performing long-duration missions onboard the ISS and especially if looking into planned future manned missions to Mars. In order to begin the process of predicting the dose levels seen by the organs of an astronaut, being the prerequisite for radiation risk calculations, it is necessary to understand the character of the radiation environment both in- and outside of the ISS as well as the relevant contributions from the radiation field to the organ doses. In this paper the three-dimensional Monte Carlo Particle and Heavy Ion Transport code System (PHITS) and a voxel-based numerical human model NUNDO (Numerical RANDO) were used to estimate the radiation load of human organs during a long term activity outside the ISS. The baseline measured data was generated with the MATROSHKA-1 (MTR-1) experiment taking place from February 2004 up to October 2005 outside the Russian Zvezda module of the ISS, thereby simulating a long term extravehicular activity (EVA) of an astronaut. The organ absorbed dose values calculated by PHITS for the inner organs are in a good agreement with the experimental data. However, a rather large disagreement was observed for the most outer organs. This disagreement appears to be due to the strong dependence that the thickness of the applied carbon fiber container, acting as the EVA suit of the astronaut, has on the effects caused by the trapped electron (TE) component. The organ dose equivalent values for the deeper organs are a factor of two lower than the experimental data. The detailed reason behind this is still under investigation. Title: The DOSIS and DOSIS 3D Experiments onboard the International Space Station - Results from the Active DOSTEL Instruments Authors: Burmeister, Soenke; Berger, Thomas; Reitz, Guenther; Beaujean, Rudolf; Boehme, Matthias; Haumann, Lutz; Labrenz, Johannes; Kortmann, Onno Bibcode: 2012cosp...39..261B Altcode: 2012cosp.meet..261B Besides the effects of the microgravity environment, and the psychological and psychosocial problems experienced in confined spaces, radiation is the main health detriment for long duration human space missions. The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones present on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station ISS is therefore needed. For the investigation of the spatial and temporal distribution of the radiation field inside the European COLUMBUS module the experiment DOSIS (Dose Distribution Inside the ISS) under the lead of DLR was launched on July 15th 2009 with STS-127 to the ISS. The experimental package was transferred from the Space Shuttle into COLUMBUS on July 18th. It consists of a combination of passive detector packages (PDP) distributed at 11 locations inside the European Columbus Laboratory and two active radiation detectors (DOSTELs) with a DDPU (DOSTEL Data and Power Unit) in a nomex pouch (DOSIS MAIN BOX) mounted at a fixed location beneath the European Physiology Module rack (EPM) inside COLUMBUS. The DOSTELs measured during the lowest solar minimum conditions in the space age from July 18th 2009 to June 16th 2011. In July 2011 the active hardware was transferred to ground for refurbishment and preparation for the DOSIS-3D experiment. The hardware will be launched with the Soyuz 30S flight to the ISS on May 15th 2012 and activated approximately ten days later. Data will be transferred from the DOSTEL units to ground via the EPM rack which is activated approximately every four weeks for this action. First Results for the active DOSIS-3D measurements such as count rate profiles, dose rates and LET spectra will be presented in comparison to the data of the DOSIS experiment as well as the DOSMAP experiment which has been performed during solar maximum in 2001. Title: Presentation of the Biochip experiment on the EXPOSE-R2 facility aboard the International Space Station Authors: Vigier, Flavie; Cottin, Hervé; Dobrijevic, Michel; Berger, Thomas; Coussot, Gaelle; Incerti, Sebastien; Vandenabeele-Trambouze, Odile; Le Postollec, Aurelie; Chaput, Didier Bibcode: 2012cosp...39.2091V Altcode: 2012cosp.meet.2091V No abstract at ADS Title: Biological Weighting of Depth Dose Distribution in a Heavy Ion Exposed Phantom Head Authors: Hellweg, Christine; Baumstark-Khan, Christa; Schmitz, Claudia; Berger, Thomas; Reitz, Guenther; Chishti, Arif Ali; Koerner, Dipl. -(FH). Christine; Feles, Sebastian; La Tessa, Chiara; Lau, Patrick Bibcode: 2012cosp...39..745H Altcode: 2012cosp.meet..745H No abstract at ADS Title: Intercomparison of luminescence detectors for space radiation dosimetry within Proton-ICCHIBAN experiments Authors: Uchihori, Yukio; Ploc, Ondrej; Yasuda, Nakahiro; Berger, Thomas; Hajek, Michael; Kodaira, Satoshi; Benton, Eric; Ambrozova, Iva; Kitamura, Hisashi Bibcode: 2012cosp...39.2025U Altcode: 2012cosp.meet.2025U Luminescence detectors for space radiation dosimetry are frequently used to estimate personal and environmental doses in the International Space Station and other space vehicles. Detector responses for cosmic rays and their secondaries were investigated for a long time and it is well-known that luminescence detectors have dependencies of response on LET (Linear Energy Transfer). Some of luminescence detectors show over-response to gamma rays (used for routine calibration) and others have similar responses to gamma rays. But, because of lack of sufficient and reliable calibration data in the low LET region (about 1 keV/μm), it is the responses of these detectors at LET is poorly known. Protons make up the dominant portion of the fluence from space radiation, so the LET region corresponding to energetic protons must be characterized very well. For that purpose, calibration and intercomparison experiments were performed using relatively low energy (30 to 80 MeV) proton beams at the National Institute of Radiological Sciences, Chiba, Japan. In this paper, the results of these intercomparison experiments, including high energy protons and light ions, are reported and illustrate the response of luminescence detectors in the low LET region. This research will help improve our understanding of space dosimeters and reliable dose measurement for astronauts and cosmonauts in low earth orbit. Title: The Mobile Dosimetric Telescope (MDT) - Development of a small size active personal dosimeter for application at high altitudes and onboard the International Space Station Authors: Ritter, Birgit; Berger, Thomas; Reitz, Guenther; Burmeister, Soenke; Heber, Bernd; Marsalek, Karel Bibcode: 2012cosp...39.1615R Altcode: 2012cosp.meet.1615R The radiation environment in space poses one of the main health risks for long duration human missions as it differs significantly from the natural radiation environment on Earth. Therefore, it is essential to monitor the properties of the radiation field in such environments. The aim of this work is to develop a small size battery driven personal dosimeter, based on silicon detector technology. Two silicon detectors are arranged in a telescope configuration, which allows the measurement of the ionizing constituents of the field and partially of the neutral contribution to the dose. The absorbed dose is obtained by measuring every particle in either of the detectors. Additionally, particles traversing both diodes are detected as coincidences. From these measurements linear energy transfer (LET) spectra will be generated from which the quality factor of the field will be determined. Quality factor times absorbed dose in the detector gives the dose equivalent - a central quantity in radiation protection. Calibrations of the detector system have been and will further be performed with various radioactive sources, and with heavy ions at the Heavy Ion Medical Accelerator (HIMAC) facility at NIRS in Chiba, Japan. Title: MATROSHKA - Results from the exposure inside the Japanese KIBO Module - and comparison with previous missions Authors: Berger, Thomas Bibcode: 2012cosp...39..147B Altcode: 2012cosp.meet..147B No abstract at ADS Title: Altitude Dependence of the Dose Rate From Ground up to the Stratosphere. Authors: Möller, Thomas; Berger, Thomas; Ehresmann, Bent; Burmeister, Soenke; Labrenz, Johannes; Heber, Bernd; Wimmer-Schweingruber, Robert; Panitzsch, Lauri Bibcode: 2012cosp...39.1266M Altcode: 2012cosp.meet.1266M No abstract at ADS Title: Assessment of Galactic Cosmic Ray Models Authors: Isha Mrigakshi, Alankrita; Matthiä, Daniel; Berger, Thomas; Reitz, Guenther; Wimmer-Schweingruber, Robert Bibcode: 2012cosp...39.1285I Altcode: 2012cosp.meet.1285I No abstract at ADS Title: Simulations of the radiation exposure outside and inside the Earth's magnetosphere Authors: Isha Mrigakshi, Alankrita; Matthiä, Daniel; Berger, Thomas; Reitz, Guenther; Wimmer-Schweingruber, Robert Bibcode: 2012cosp...39.1286I Altcode: 2012cosp.meet.1286I No abstract at ADS Title: Acoustic Events in the Solar Atmosphere from Hinode/SOT NFI Observations Authors: Malherbe, J. -M.; Roudier, T.; Rieutord, M.; Berger, T.; Franck, Z. Bibcode: 2012SoPh..278..241M Altcode: 2012arXiv1207.1170M We investigate the properties of acoustic events (AEs), defined as spatially concentrated and short duration energy flux, in the quiet Sun, using observations of a 2D field of view (FOV) with high spatial and temporal resolution provided by the Solar Optical Telescope (SOT) onboard Hinode. Line profiles of Fe I 557.6 nm were recorded by the Narrow-band Filter Imager (NFI) on a 82″×82″ FOV during 75 min with a time step of 28.75 s and 0.08″ pixel size. Vertical velocities were computed at three atmospheric levels (80, 130, and 180 km) using the bisector technique, allowing the determination of energy flux to be made in the range 3 - 10 mHz using two complementary methods (Hilbert transform and Fourier power spectrum). Horizontal velocities were computed using local correlation tracking (LCT) of continuum intensities providing divergences. We found that the net energy flux is upward. In the range 3 - 10 mHz, a full FOV space and time averaged flux of 2700 W m−2 (lower layer 80 - 130 km) and 2000 W m−2 (upper layer 130 - 180 km) is concentrated in less than 1 % of the solar surface in the form of narrow (0.3″) AE. Their total duration (including rise and decay) is of the order of 103 s. Inside each AE, the mean flux is 1.6×105 W m−2 (lower layer) and 1.2×105 W m−2 (upper). Each event carries an average energy (flux integrated over space and time) of 2.5×1019 J (lower layer) to 1.9×1019 J (upper). More than 106 events could exist permanently on the Sun, with a birth and decay rate of 3500 s−1. Most events occur in intergranular lanes, downward velocity regions, and areas of converging motions. Title: Simulations of the Magnetic Rayleigh-Taylor Instability in the Kippenhahn-Schlüter Prominence Model Authors: Hillier, A.; Berger, T.; Shibata, K.; Isobe, H. Bibcode: 2012ASPC..456..157H Altcode: The launch of the Hinode satellite, with the Solar Optical Telescope, allowed for high resolution, high time cadence observations of prominences to be performed in the seeing free environment of space. The most striking discovery from these observations is of plumes, approximately 1 Mm in width, that propagate through the prominence material. The plumes initiate from underdense bubbles that form beneath prominences, rise at constant speeds of approximately 20 km s-1 and are formed in the conditions required for the magnetic Rayleigh-Taylor instability to occur. To study this phenomenon, we performed 3D simulations of the magnetic Rayleigh-Taylor instability in the Kippenhahn-Schlüter prominence model. The plumes formed in these simulations are filamentary structures that are aligned with the magnetic field created as 3D modes of the magnetic Rayleigh-Taylor instability. The plumes rise, developing large structures from smaller structures through an inverse cascade process driven by nonlinear interaction. The results suggest that the plumes observed in the prominence may be used to study the conditions inside the prominence. Title: The Rayleigh-taylor Instability In The Solar Corona: Prominence Coronal-cavity Interactions And The Evolution To Eruptive States Authors: Berger, Thomas Bibcode: 2012AAS...22050801B Altcode: We review the discovery and analysis of the Rayleigh-Taylor instability in quiescent solar prominences by the Hinode/SOT and SDO/AIA instruments. The instability is apparently caused by the emergence of magnetic flux near the polarity inversion line below the prominences. The emerging flux is rapidly heated to coronal temperatures of 1 MK or higher and the resulting large temperature gradient with the cool overlying prominence plasma leads to a "magneto-thermal" convective instability that develops into a classic Rayleigh-Taylor system of plumes and downflows. The significance of the discovery is that it offers a mechanism by which magnetic flux and helicity are periodically injected into the coronal cavity flux ropes overlying solar prominences. The increasing flux and helicity in the cavity develop a quasi-steady evolution eventually terminating in the eruption of a slow coronal mass ejection (Fan & Gibson 2007; Zhang, Flyer, & Low 2006). We suggest further investigations using SDO/AIA, ground-based observatories, and the upcoming IRIS mission to verify and extend the SOT and AIA findings. Title: Some Dynamic Analysis of the Photosphere from Hinode/SOT and SDO/HMI Observations Authors: Roudier, T.; Malherbe, J.; Rieutord, M.; Berger, T.; Frank, Z.; Prat, V.; Renon, N.; Gizon, L.; Svanda, M. Bibcode: 2012ASPC..456...65R Altcode: We first present the important role played by the families of granule (or Tree of Fragmenting granules) in the formation of the photospheric network. Then, we describe the occurence and characteristics of acoustic events (AE), defined as spatially concentrated energy flux, in the quiet Sun. Finally, we present how horizontal velocities obtained from SDO/HMI data are calibrated by using Hinode/SOT observations. Title: Emergence of Twisted Flux in Prominence Observations Authors: Okamoto, T. J.; Tsuneta, S.; Berger, T. E.; Lites, B. W. Bibcode: 2012ASPC..455..123O Altcode: The emergence of twisted flux is a key process for supply of magnetic flux into the corona as well as solar dynamic activities such as sunspot formation and trigger of coronal mass ejections. In particular, there are numerous discussions about the role and necessity of twisted flux emergence for origin of prominences. However, the difficulty to measure vector magnetic fields has not allowed us to investigate the detailed relationship between emerging twisted flux and prominence. Hinode has changed the situation. The Spectro-Polarimeter aboard Hinode has high sensitivity to weaker magnetic fields of fine structures, and provides opportunities to detect weak horizontal magnetic fields. As a result, we have obtained signatures of twisted flux emergence associated with prominences: The observational features are "broadening and narrowing of a region dominated by horizontal magnetic field" and "rotating direction of horizontal field" on the photosphere. Moreover, the data show the interaction between the emerging twisted flux and granules, and that the flux rope has high intrinsic strength 650 G, while the flux density is as low as 100 G. Theoretical research with numerical simulation on the basis of these results is active. In addition, we investigate activities of a coronal cavity overlying a prominence on the limb, and suggest the existence of twisted flux rope to explain the activities of prominence and the coronal cavity comprehensively. Here we introduce both these observational and theoretical results, and discuss the details about emerging twisted flux. Title: SDO/AIA Observations of Sustained Coronal Condensation in Prominences as Return Flows of the Chromosphere-Corona Mass Cycle Authors: Liu, Wei; Berger, T.; Low, B. C. Bibcode: 2012AAS...22020708L Altcode: It has recently been proposed that prominences are manifestations of a magneto-thermal convection process that involves ever-present dynamic descents of cool material threads and upflows of hot bubbles (Berger et al. 2011 Nature). On global scales, prominences may play an important role as the return flows of the chromosphere-corona mass cycle, in which hot mass is originally transported upward through spicules. A critical step in this cycle is the condensation of million-degree coronal plasma into T<10,000 K prominence material by radiative cooling instability. However, direct observation of coronal condensation has been difficult in the past, a situation recently changed. We present here the first example observed with SDO/AIA, in which hours of gradual cooling through multiple EUV channels (from 2 MK to 80,000 K) in large-scale loops leads to eventual condensation at magnetic dips, where we find evidence of magnetic reconnection and subsequent outflows. A moderate-size prominence of 10^14 gram is then formed. Its mass is not static but maintained by a continual supply through condensation at a high rate of 10^10 gram/s against a comparable drainage through numerous vertical threads at less than free-fall speeds. Most of the total condensation of 10^15 gram, comparable to a CME mass and an order of magnitude more than the instantaneous mass of the prominence itself, is drained in merely one day. These new observations show that a macroscopically quiescent prominence is microscopically dynamic (Liu, Berger, Low 2012 ApJL), involving the passage of a significant mass that bears important implications for the chromosphere-corona mass cycle. This interpretation is further supported by the recent theoretical development on spontaneous formation of current sheets and cool condensations (Low, Berger, Casini, & Liu, 2012 submitted to ApJ). Title: Cosmic Radiation Exposure of Biological Test Systems During the EXPOSE-E Mission Authors: Berger, Thomas; Hajek, Michael; Bilski, Pawel; Körner, Christine; Vanhavere, Filip; Reitz, Günther Bibcode: 2012AsBio..12..387B Altcode: No abstract at ADS Title: Quasi full-disk maps of solar horizontal velocities using SDO/HMI data Authors: Roudier, Th.; Rieutord, M.; Malherbe, J. M.; Renon, N.; Berger, T.; Frank, Z.; Prat, V.; Gizon, L.; Švanda, M. Bibcode: 2012A&A...540A..88R Altcode: 2012arXiv1203.0514R
Aims: For the first time, the motion of granules (solar plasma on the surface on scales larger than 2.5 Mm) has been followed over the entire visible surface of the Sun, using SDO/HMI white-light data.
Methods: Horizontal velocity fields are derived from image correlation tracking using a new version of the coherent structure tracking algorithm. The spatial and temporal resolutions of the horizontal velocity map are 2.5 Mm and 30 min, respectively.
Results: From this reconstruction, using the multi-resolution analysis, one can obtain to the velocity field at different scales with its derivatives such as the horizontal divergence or the vertical component of the vorticity. The intrinsic error on the velocity is ~0.25 km s-1 for a time sequence of 30 min and a mesh size of 2.5 Mm. This is acceptable compared to the granule velocities, which range between 0.3 km s-1 and 1.8 km s-1. A high correlation between velocities computed from Hinode and SDO/HMI has been found (85%). From the data we derive the power spectrum of the supergranulation horizontal velocity field, the solar differential rotation, and the meridional velocity. Title: The Hydromagnetic Nature of Quiescent Prominences Authors: Low, B. C.; Berger, T.; Casini, R.; Liu, W. Bibcode: 2012decs.confE..84L Altcode: High-resolution observations of quiescent prominences with Hinode and SDO have revealed within their interiors the ever-¬present descent at less than free-fall speeds of cool, vertical dense filaments interspersed among upward, narrow streams at comparable speeds of heated, low-density plasma. We address the physical nature of this dynamical state. Despite the high magnetic Reynolds numbers characterizing this hydromagnetic environment, magnetic reconnection takes place via spontaneous formation and dissipation of current sheets by the coupled effects of highly-anisotropic thermal conduction, gravity, optically-thin radiation, heating, and high electrical conductivity. In this interesting new version of the theory of Parker (1994, Spontaneous current sheets in magnetic fields, Cambridge U Press), pervasive reconnections produce a perennial local descent of dense condensations under gravity along newly reconnected magnetic field lines and a concurrent turbulent rise of buoyant pockets of heated magnetized plasma through the large-scale magnetic structure. This mechanism may explain the massive downward drainage through a quiescent prominence observed recently (Liu et al. 2012 ApJ 745, L21) and, in the broader context, relate the quiescent prominence to the surrounding chromosphere/corona as a novel, large-scale, magneto-thermal convective phenomenon (Berger et al. 2011, Nature 472, 197). Title: SDO/AIA Observations of Sustained Coronal Condensation and Mass Drainage in Prominences as Return Flows of the Chromosphere-Corona Mass Cycle Authors: Liu, Wei; Berger, Thomas; Low, B. C. Bibcode: 2012decs.confE..90L Altcode: It has recently been proposed that prominences are manifestations of a magneto-thermal convection process that involves ever-present dynamic descents of cool material threads and upflows of hot bubbles (Berger et al. 2011 Nature). On global scales, prominences may play an important role as the return flows of the chromosphere-corona mass cycle, in which hot mass is originally transported upward through spicules. A critical step in this cycle is the condensation of million-degree coronal plasma into T<10,000 K prominence material by radiative cooling instability. However, direct observation of coronal condensation has been difficult in the past, a situation recently changed with the launch of the Hinode/SOT and SDO/AIA. We present here the first example observed with SDO/AIA, in which hours of gradual cooling through multiple EUV channels (from 2 MK to 80,000 K) in large-scale loops leads to eventual condensation at magnetic dips, forming a moderate-size prominence of 10^14 gram. The prominence mass is not static but maintained by a continual supply through condensation at a high rate of 10^10 gram/s against a comparable drainage through numerous vertical threads at less than free-fall speeds. Most of the total condensation of 10^15 gram, comparable to a CME mass and an order of magnitude more than the instantaneous mass of the prominence itself, is drained in merely one day. These new observations show that a macroscopically quiescent prominence is microscopically dynamic, involving the passage of a significant mass that bears important implications for the chromosphere-corona mass cycle. This interpretation is further supported by the recent theoretical development on spontaneous formation of current sheets and cool condensations (Low, Berger, Casini, & Liu, this meeting). Title: The Prominence/Coronal Cavity Connection: using Hinode, AIA, and IRIS to explore the source of quiet-Sun CMEs Authors: Berger, Thomas Bibcode: 2012decs.confE..29B Altcode: The Hinode and SDO/AIA missions have revolutionized our view of prominences and coronal cavities. Hinode/SOT observations have established that quiescent prominences are extremely dynamic structures with constant filamentary downflows, rising magnetic "bubbles" that lead to Rayleigh-Taylor instability flows, and various MHD wave modes. SDO/AIA has shown that coronal cavities have helical magnetic topology and that quiescent prominences and coronal cavities should be viewed as elements of a single magnetic system: magnetic flux ropes in the corona, by far the largest coherent magnetic structures on the Sun and the source of all quiet-Sun CMEs. In this talk we review the Hinode/SOT and SDO/AIA observations of prominences and coronal cavities to demonstrate the unification of these previously disparate topics. We conclude with a look at possible measurements using IRIS to further our understanding of this complex chromospheric/coronal magnetic system. Title: First SDO/AIA Observation of Solar Prominence Formation Following an Eruption: Magnetic Dips and Sustained Condensation and Drainage Authors: Liu, Wei; Berger, Thomas E.; Low, B. C. Bibcode: 2012ApJ...745L..21L Altcode: Imaging solar coronal condensation forming prominences was difficult in the past, a situation recently changed by Hinode and the Solar Dynamics Observatory (SDO). We present the first example observed with the SDO/Atmospheric Imaging Assembly, in which material gradually cools through multiple EUV channels in a transequatorial loop system that confines an earlier eruption. Nine hours later, this leads to eventual condensation at the dips of these loops, forming a moderate-size prominence of ~1014 g, to be compared to the characteristic 1015 g mass of a coronal mass ejection (CME). The prominence mass is not static but maintained by condensation at a high estimated rate of 1010 g s-1 against a comparable, sustained drainage through numerous vertical downflow threads, such that 96% of the total condensation (~1015 g) is drained in approximately one day. The mass condensation and drainage rates temporally correlate with the total prominence mass. The downflow velocity has a narrow Gaussian distribution with a mean of 30 km s-1, while the downward acceleration distribution has an exponential drop with a mean of ~1/6 g , indicating a significant canceling of gravity, possibly by the Lorentz force. Our observations show that a macroscopically quiescent prominence is microscopically dynamic, involving the passage of a significant mass through it, maintained by a continual mass supply against a comparable mass drainage, which bears important implications for CME initiation mechanisms in which mass unloading is important. Title: Numerical Simulations of the Magnetic Rayleigh-Taylor Instability in the Kippenhahn-Schlüter Prominence Model. I. Formation of Upflows Authors: Hillier, Andrew; Berger, Thomas; Isobe, Hiroaki; Shibata, Kazunari Bibcode: 2012ApJ...746..120H Altcode: The launch of the Hinode satellite led to the discovery of rising plumes, dark in chromospheric lines, that propagate from large (~10 Mm) bubbles that form at the base of quiescent prominences. The plumes move through a height of approximately 10 Mm while developing highly turbulent profiles. The magnetic Rayleigh-Taylor instability was hypothesized to be the mechanism that drives these flows. In this study, using three-dimensional (3D) MHD simulations, we investigate the nonlinear stability of the Kippenhahn-Schlüter prominence model for the interchange mode of the magnetic Rayleigh-Taylor instability. The model simulates the rise of a buoyant tube inside the quiescent prominence model, where the interchange of magnetic field lines becomes possible at the boundary between the buoyant tube and the prominence. Hillier et al. presented the initial results of this study, where upflows of constant velocity (maximum found 6 km s-1) and a maximum plume width ≈1.5 Mm which propagate through a height of approximately 6 Mm were found. Nonlinear interaction between plumes was found to be important for determining the plume dynamics. In this paper, using the results of ideal MHD simulations, we determine how the initial parameters for the model and buoyant tube affect the evolution of instability. We find that the 3D mode of the magnetic Rayleigh-Taylor instability grows, creating upflows aligned with the magnetic field of constant velocity (maximum found 7.3 km s-1). The width of the upflows is dependent on the initial conditions, with a range of 0.5-4 Mm which propagate through heights of 3-6 Mm. These results are in general agreement with the observations of the rising plumes. Title: Simulations of the magnetic Rayleigh-Taylor instability in a quiescent prominence model to study the dark upflows observed in prominences Authors: Hillier, A. S.; Berger, T. E.; Shibata, K.; Isobe, H. Bibcode: 2011AGUFMSH33A2033H Altcode: Observations of quiescent prominences by the Solar Optical Telescope (SOT) on board the Hinode satellite show plumes of hot, underdense material rising through the prominence. These plumes form at the boundary between the prominence and low density bubbles, approximately 10 Mm in size, that appear beneath the prominence, and then rise through the prominence material at speeds of approximately 20 km/s and widths of approximately 1.5 Mm. The plume profile ranges from highly turbulent to smooth, suggesting that the prominence conditions, as well as those of the bubble, are important in determining the dynamics. To investigate this phenomenon, we perform simulations of the magnetic Rayleigh-Taylor instability in a local prominence model. The instability creates rising plumes of hot, underdense material that propagate through the prominence material at a velocity of approximately 6-7 km/s and widths of approximately 1.5 Mm, in rough agreement with the Hinode observations. Nonlinear effects, in which the interaction between plumes drives an inverse cascade process creating large plumes from smaller plumes, are found to be important. Increasing the magnetic field strength creates smoother plume structures. The addition of a strong guide field, which is suggested in some prominence models, does not hinder plume formation but does change the dynamic scaling. The Rayleigh-Taylor instability drives an upward flow of magnetic energy and a downward flow of mass. The results from the simulations well match the characteristics of the observed plumes, suggesting that the magnetic Rayleigh-Taylor instability could be important in determining prominence structure as well as changing the magnetic energy distribution in overlying coronal cavities which ultimately erupt as coronal mass ejections. Title: Quiescent Prominences, Coronal Cavities, and Coronal Mass Ejections: a unified systems viewpoint Authors: Berger, T. E. Bibcode: 2011AGUFMSH33A2034B Altcode: We review the observed relationships between polar crown quiescent prominences, coronal cavities, and polar crown CMEs with the goal of understanding these phenomena as aspects of a single magnetic system. We propose that the fundamental structure is a helical magnetic flux rope suspended in the corona. Coronal cavities are the (view-angle dependent) markers of the density depletion in the core of the flux rope. Quiescent prominences are plasma flow systems in the current sheet region below the flux rope. The recently discovered coronal prominence bubbles that propagate via a Rayleigh-Taylor instability through the prominence region are injections of new magnetic flux and helicity into the coronal flux rope. Flux ropes erupt as slow coronal mass ejections when the magnetic energy density exceeds that of the overlying "arcade" fields, essentially forming a "magnetic bubble" that "floats" away from the Sun. We emphasize that this system and its mechanism of eruption may not be applicable to the much stronger magnetic fields in active region prominence formations. Title: Numerical Simulations of the Magnetic Rayleigh-Taylor Instability in the Kippenhahn-Schlüter Prominence Model Authors: Hillier, Andrew; Isobe, Hiroaki; Shibata, Kazunari; Berger, Thomas Bibcode: 2011ApJ...736L...1H Altcode: 2011arXiv1107.4882A The launch of the Hinode satellite has allowed unprecedented high-resolution, stable images of solar quiescent prominences to be taken over extended periods of time. These new images led to the discovery of dark upflows that propagated from the base of prominences, developing highly turbulent profiles. As yet, how these flows are driven is not fully understood. To study the physics behind these phenomena, we use three-dimensional magnetohydrodynamic simulations to investigate the nonlinear stability of the Kippenhahn-Shlüter prominence model to the magnetic Rayleigh-Taylor instability. The model simulates the rise of a buoyant tube inside a quiescent prominence, where the upper boundary between the tube and prominence model is perturbed to excite the interchange of magnetic field lines. We found upflows of constant velocity (maximum found 6 km s-1) and a maximum plume width ≈1500 km which propagate through a height of approximately 6 Mm in the no guide field case. The case with the strong guide field (initially By = 2Bx ) results in a large plume that rises through the prominence model at ~5 km s-1 with width ~900 km (resulting in width of 2400 km when viewed along the axis of the prominence), reaching a height of ~3.1 Mm. In both cases, nonlinear processes were important for determining plume dynamics. Title: Flares Producing Well-organized Post-flare Arcades (Slinkies) Have Early Precursors Authors: Ryutova, M. P.; Frank, Z.; Hagenaar, H.; Berger, T. Bibcode: 2011ApJ...733..125R Altcode: Exploding loop systems producing X-ray flares often, but not always, bifurcate into a long-living, well-organized system of multi-threaded loop arcades resembling solenoidal slinkies. The physical conditions that cause or prevent this process are not known. To address this problem, we examined most of the major (X-class) flares that occurred during the last decade and found that the flares that bifurcate into long-living slinky arcades have different signatures than those that do not "produce" such structures. The most striking difference is that, in all cases of slinky formation, GOES high energy proton flux becomes significantly enhanced 10-24 hr before the flare occurs. No such effect was found prior to the "non-slinky" flares. This fact may be associated with the difference between energy production by a given active region and the amount of energy required to bring the entire system into the form of well-organized, self-similar loop arcades. As an example illustrating the process of post-flare slinky formation, we present observations taken with the Hinode satellite, in several wavelengths, showing a time sequence of pre-flare and flare activity, followed by the formation of dynamically stable, well-organized structures. One of the important features revealed is that post-flare coronal slinky formation is preceded by scale invariant structure formation in the underlying chromosphere/transition region. We suggest that the observed regularities can be understood within the framework of self-organized critical dynamics characterized by scale invariant structure formation with critical parameters largely determined by energy saturation level. The observed regularities per se may serve as a long-term precursor of strong flares and may help to study predictability of system behavior. Title: SDO/AIA Observations of Coronal Condensation Leading to Prominence Formation Authors: Liu, Wei; Berger, T.; Low, B. C.; Casini, R. Bibcode: 2011SPD....42.2119L Altcode: 2011BAAS..43S.2119L Coronal condensation takes place when million degree coronal plasma undergoes radiative cooling instability. Direct observation of coronal condensation in prominences has been difficult in the past, but with the launch of the Hinode/SOT and SDO/AIA instruments, numerous observations of plasma condensing "out of nowhere" high up in quiescent prominences have been captured. We present here one such event seen with SDO/AIA. On 25-Nov-2010, a prominence above the southwest limb is swept away by a nearby eruption, and for next a few hours there is no visible 304 A material in the local corona. Then, a portion of the coronal loops at the same location progressively sags and forms a local dip, where the first sign of new, cool material appears, 7.5 hours after the eruption. This is a clear indication of coronal condensation, and the gradual sag of the loops is likely a result of increasing weight of the condensed material that has been accumulated at the dip. Similar condensation occurs nearby at a larger rate and leads to the formation of a moderate-size prominence. The estimated prominence mass increases linearly for about 7 hours at a rate of 2.6e10 grams/sec and reaches approximately 6e14 grams. Simultaneously, the prominence drains through vertical flows of approximately 32 km/s, bringing the mass back to the chromosphere. We estimate the mass drain rate to be 2.7e10 grams/sec, which, together with the estimated mass accumulation rate, implies a coronal condensation rate of approximately 5.3e10 grams/sec. This study can provide critical information about the coupling between condensation energetics and MHD, prominence mass cycles, and coronal mass ejections initiated by loss of anchoring prominence mass (e.g., Low 2001). Title: Filament and Prominence Research with the Advanced Technology Solar Telescope Authors: Berger, Thomas Bibcode: 2011SPD....42.0802B Altcode: 2011BAAS..43S.0802B Recent advances in our understanding of solar filaments on the disk and prominences off the limb have come primarily from the Hinode/Solar Optical Telescope (SOT) and the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA). These moderate spatial and temporal resolution instruments offer the huge advantage of seeing-free, low-scattering, observations from space. However they are limited in their abilities to provide spectral and/or polarimetric information. In contrast, the ATST will provide extremely high spatial and temporal resolution images of both filaments and prominences in a wide variety of spectral lines and polarimetric modes. We review recent SOT and AIA research as well as the current science questions regarding the formation and dynamics of filaments and prominences and their role in active and quiet-region coronal mass ejections. We then discuss key measurements that the ATST is expected to make and how these measurements will significantly advance our understanding of these enigmatic markers of magnetic energy storage in the solar corona. Title: A Droplet Model of Quiescent Prominence Downflows Authors: Haerendel, G.; Berger, T. Bibcode: 2011ApJ...731...82H Altcode: Observations of quiescent prominences with the Solar Optical Telescope on the Hinode satellite have revealed the ubiquitous existence of downflows forming coherent thin and highly structured vertically oriented threads with velocities between 10 and 20 km s-1. Their widths range between 300 and 500 km. They are often initiated at the top of the visible prominence, but sometimes also at intermediate level. We propose that the downflows are made of plasma packets that squeeze themselves through the dominantly horizontal field under the action of gravity. Their origin is assumed to be hot plasma supplied from either inside or the immediate vicinity of the prominence and condensing at its top. Under compression and further cooling, the matter overflows to the flanks of the prominence dragging its magnetic field with it. Under the increasing action of gravity, vertical structures are forming which eventually disconnect from the field of the inflow channel thus forming finite plasma packets. This process is reminiscent of water flowing over a mountain ridge and breaking up into a multitude of droplets. Like water droplets being subject to air drag, the falling plasma droplets experience a drag force by the horizontal prominence field and assume a steady vertical velocity. This happens via the excitation of Alfvén waves. Lateral confinement by the prominence field determines their spatial extent. The small scales of the droplets and the directional balance of their internal tangled magnetic fields can explain the absence of appreciable vertical components in magnetic field measurements. On the basis of the observed width and vertical speed of the downflows and by adopting a prominence field of about 8 G, we derive central density and temperature of the droplets, which turn out to be quite consistent with known prominence characteristics. In the formulation of the drag force a dimensionless "magnetic drag coefficient" has been introduced with a value well below unity. Title: Magneto-thermal convection in solar prominences Authors: Berger, Thomas; Testa, Paola; Hillier, Andrew; Boerner, Paul; Low, Boon Chye; Shibata, Kazunari; Schrijver, Carolus; Tarbell, Ted; Title, Alan Bibcode: 2011Natur.472..197B Altcode: Coronal cavities are large low-density regions formed by hemispheric-scale magnetic flux ropes suspended in the Sun's outer atmosphere. They evolve over time, eventually erupting as the dark cores of coronal mass ejections. Although coronal mass ejections are common and can significantly affect planetary magnetospheres, the mechanisms by which cavities evolve to an eruptive state remain poorly understood. Recent optical observations of high-latitude `polar crown' prominences within coronal cavities reveal dark, low-density `bubbles' that undergo Rayleigh-Taylor instabilities to form dark plumes rising into overlying coronal cavities. These observations offered a possible mechanism for coronal cavity evolution, although the nature of the bubbles, particularly their buoyancy, was hitherto unclear. Here we report simultaneous optical and extreme-ultraviolet observations of polar crown prominences that show that these bubbles contain plasma at temperatures in the range (2.5-12)×105 kelvin, which is 25-120 times hotter than the overlying prominence. This identifies a source of the buoyancy, and suggests that the coronal cavity-prominence system supports a novel form of magneto-thermal convection in the solar atmosphere, challenging current hydromagnetic concepts of prominences and their relation to coronal cavities. Title: Chromospheric Jet and Growing "Loop" Observed by Hinode: New Evidence of Fan-spine Magnetic Topology Resulting from Flux Emergence Authors: Liu, Wei; Berger, Thomas E.; Title, Alan M.; Tarbell, Theodore D.; Low, B. C. Bibcode: 2011ApJ...728..103L Altcode: 2010arXiv1012.1897L We present observations of a chromospheric jet and growing "loop" system that show new evidence of a fan-spine topology resulting from magnetic flux emergence. This event, occurring in an equatorial coronal hole on 2007 February 9, was observed by the Hinode Solar Optical Telescope in the Ca II H line in unprecedented detail. The predecessor of the jet is a bundle of fine material threads that extend above the chromosphere and appear to rotate about the bundle axis at ~50 km s-1 (period lsim200 s). These rotations or transverse oscillations propagate upward at velocities up to 786 km s-1. The bundle first slowly and then rapidly swings up, with the transition occurring at the onset of an A4.9 flare. A loop expands simultaneously in these two phases (velocity: 16-135 km s-1). Near the peak of the flare, the loop appears to rupture; simultaneous upward ejecta and mass downflows faster than free-fall appear in one of the loop legs. The material bundle then swings back in a whip-like manner and develops into a collimated jet, which is orientated along the inferred open-field lines with transverse oscillations continuing at slower rates. Some material falls back along smooth streamlines, showing no more oscillations. At low altitudes, the streamlines bifurcate at presumably a magnetic null point and bypass an inferred dome, depicting an inverted-Y geometry. These streamlines closely match in space the late Ca II H loop and X-ray flare loop. These observations are consistent with the model that flux emergence in an open-field region leads to magnetic reconnection, forming a jet and fan-spine topology. We propose that the material bundle and collimated jet represent the outer spine in quasi-static and eruptive stages, respectively, and the growing loop is a two-dimensional projection of the three-dimensional fan surface. Title: MHD simulations of quiescent prominence upflows in the Kippenhahn-Schlüter prominence model Authors: Hillier, A. S.; Isobe, H.; Shibata, K.; Berger, T. E. Bibcode: 2011ASInC...2..331H Altcode: Images from the Hinode satellite have led to the discovery of dark upflows that propagate from the base of prominences, developing highly turbulent profiles. The magnetic Rayleigh-Taylor instability has been hypothesized as the mechanism to create these plumes. To study the physics behind this phenomenon we use 3D magnetohydrodynamic simulations to investigate the nonlinear stability of the Kippenhahn-Shlüter prominence model to the magnetic Rayleigh-Taylor instability. The model simulates the rise of a buoyant tube inside a quiescent prominence, where the upper boundary between the tube and prominence model is perturbed to excite the interchange of magnetic field lines. We find upflows of constant velocity (maximum found 6 km s^{-1}) and a maximum plume width ≈ 1500 km which propagate through a height of approximately 6 Mm, in general agreement with the Hinode observations. Title: Greenhouse effect in quiescent prominences Authors: Ryutova, M.; Berger, T. E.; Title, A. M. Bibcode: 2010AGUFMSH51A1664R Altcode: Quiescent prominences, by definition, are huge ``clouds'' of cool, dense plasma overlying rarefied hot corona and supported by a complex magnetic field anchored in the photosphere along the magnetic polarity inversion line. One of the most prominent features in their dynamics is formation, growth and collapse of bubble/cavities filled by coronal plasma and emerging, often repeatedly, under a prominence body. As such, prominence/corona interface itself is subject of fundamental plasma instabilities, which include development of a regular series of plumes and spikes typical to the Rayleigh-Taylor instability, the Kelvin-Helmholtz instability, often followed by a sudden collimated mass upflow, which, in nonlinear stage having an explosive character may be responsible for CMEs. These were only recently studied in detail with high cadence, high resolution data obtained from the Hinode satellite. Even more surprises are brought by the SDO/AIA instrument showing the Sun's atmosphere in 12 visible and EUV wavelengths. AIA multi-wavelength images in a temperature range from 105 ~K to 2 × 106 ~K combined with the Hinode/SOT data show that plasma inside the prominence cavity, being as expected, at coronal temperatures, in fact exceeds the temperature of the ambient corona. We suggest that an energetically open highly dynamic processes releasing energy at the prominence/cavity interface accompanied by the ``radiative exchange'', may cause additional increase of temperature and/or density inside cavity. Given pervasive character of prominences, future studies will allow us to perform quantitative and statistical analysis, and reveal relations between the size of cavity, its temperature, and magnetic properties. Title: Coordinated observations of solar prominences with Hinode/SOT and SDO/AIA Authors: Berger, T. E.; Tarbell, T. D.; Schrijver, C. J.; Title, A. M.; Boerner, P.; Shine, R. A. Bibcode: 2010AGUFMSH21C..04B Altcode: We show the first detailed study of a solar quiescent prominence using simultaneous observations from the Hinode/SOT and SDO/AIA instruments. The prominence studied is a polar crown prominence located at the base of a large coronal cavity on the NW solar limb on 22-June-2010. Hinode observed the prominence for 2.75 hours running the HOP 73 prominence observation program to acquire Ca II H-line filtergrams and H-alpha doppler observations at a 20-second cadence. SOT observations in Ca II H-line and H-alpha spectral lines reveal the common dynamics of filamentary downflows and large-scale oscillations of the prominence body. In addition a dark cavity is observed to rise into the prominence and stagnate before going unstable to form Rayleigh-Taylor plume upflows. AIA observations in the 304, 171, 193, and 211 channels with 14 second cadence reveal that both the cavity and the plume upflows are bright in these hotter passbands. Filter ratio measurements as well as preliminary EM estimates imply that the cavity and plume plasma temperature is at least 10^6 K. Plasma at this temperature has never been detected or theorized in a confined configuration in the lower chromosphere below a prominence. Assuming an electron number density of 3e09 cm-3, the balance between thermal pressure in the cavity and magnetic pressure in the overlying prominence implies a magnetic flux density of order 10 gauss, in line with earlier measurements of prominence magnetic fields. However the cavity likely contains a significant magnetic energy density of its own implying that the prominence magnetic fields may need to be significantly higher to balance the cavity buoyancy. The existence of 10^6 K plasma confined below a quiescent prominence and the subsequent onset of buoyancy instabilities present new challenges to theories of prominence and coronal cavity formation and suggest new avenues for supply of mass and magnetic flux to the associated coronal cavity systems that make up the bulk of CMEs. Hinode/SOT Ca II H-line image overlain on SDO/AIA 304A image of a quiescent solar prominence. Title: Space Based Observations of Coronal Cavities in Conjunction with the Total Solar Eclipse of July 2010 Authors: Kucera, T. A.; Berger, T. E.; Boerner, P.; Dietzel, M.; Druckmuller, M.; Gibson, S. E.; Habbal, S. R.; Morgan, H.; Reeves, K. K.; Schmit, D. J.; Seaton, D. B. Bibcode: 2010AGUFMSH51A1666K Altcode: In conjunction with the total solar eclipse on July 11, 2010 we coordinated a campaign between ground and space based observations. Our specific goal was to augment the ground based measurement of coronal prominence cavity temperatures made using iron lines in the IR (Habbal et al. 2010 ApJ 719 1362) with measurements performed by space based instruments. Included in the campaign were Hinode/EIS, XRT and SOT, PROBA2/SWAP, SDO/AIA, SOHO/CDS and STEREO/SECCHI/EUVI, in addition to the ground based IR measurements. We plan to use a combination of line ratio and forward modeling techniques to investigate the density and temperature structure of the cavities at that time. Title: A rising cool column associated with formation of prominence and coronal cavity Authors: Okamoto, T. J.; Tsuneta, S.; Berger, T. E. Bibcode: 2010AGUFMSH51A1665O Altcode: A prominence consists of relatively cool chromospheric plasma found above the solar limb at coronal heights where the temperature and density are typically two order of magnitude higher and lower, respectively. Prominences are frequently associated with larger coronal structures known as coronal cavities. There are numerous observational studies on prominences with multi-wavelength and with high-spatial resolution and also on the relationship between cavities and coronal mass ejections, while less analyses on activities inside coronal cavities. Continuous observations were performed of a quiescent prominence with the Hinode satellite on 2006 December 23 and 24. In the Ca II H-line channel of the Solar Optical Telescope we observed a peculiar slowly-rising column of cool material from the lower atmosphere. The apparent ascent speed of the column is 2 km/s, while the fine structures of the column exhibit much faster motion of up to 20 km/s. The column eventually becomes a faint low-lying prominence. An overlying coronal cavity associated with the appearance of the column seen in the X-ray and EUV moves upward at 5 km/s. We discuss the relationship between these episodes and suggest that they are due to the emergence of a helical flux rope that undergoes reconnection with lower coronal fields, possibly carrying material into the coronal cavity. Under the assumption of the emerging flux scenario, the lower velocity of 2 km/s and the higher one of 20 km/s in the column are attributed to the rising motion of the emerging flux and to the outflow driven by magnetic reconnection between the emerging flux and the pre-existing coronal field, respectively. Our presentation gives a coherent explanation of the enigmatic phenomenon of the rising column with the emergence of the helical rope and its effect on the corona. Title: Observation of Plasma Instabilities in Quiescent Prominences Authors: Ryutova, M.; Berger, T.; Frank, Z.; Tarbell, T.; Title, A. Bibcode: 2010SoPh..267...75R Altcode: 2010SoPh..tmp..170R We study dynamics of quiescent prominences using several data sets taken with the Solar Optical Telescope (SOT) on Hinode. We find a number of processes occurring at different stages of prominence evolution that are common for all of our chosen cases and, having universal character, can be related to fundamental plasma instabilities. We combine the observational evidence and theory to identify these instabilities. Here we discuss three examples: i) prominence cavity formation and its evolution, associated with a screw-pinch instability; ii) development of a regular series of plumes and spikes typical to the Rayleigh - Taylor (RT) instability; and iii) the appearance of growing ripples at the prominence/corona interface, often followed by a sudden collimated mass upflow, attributed to the Kelvin - Helmholtz (KH) instability. The conditions for transition from a linear (rippling mode) to nonlinear stage of the KH instability, known to have an explosive character, are specified. Given excellent Hinode data, all three aspects of prominence dynamics allow quantitative analysis. Title: PHITS simulations of the Matroshka experiment Authors: Gustafsson, K.; Sihver, L.; Mancusi, D.; Sato, T.; Reitz, G.; Berger, T. Bibcode: 2010AdSpR..46.1266G Altcode: The radiation environment in space is very different from the one encountered on Earth. In addition to the sparsely ionizing radiation, there are particles of different Z with energies ranging from keV up to hundreds of GeV which can cause severe damage to both electronics and humans. It is therefore important to understand the interactions of these highly ionizing particles with different materials such as the hull of space vehicles, human organs and electronics. We have used the Particle and Heavy-Ion Transport code System (PHITS), which is a three-dimensional Monte Carlo code able to calculate interactions and transport of particles and heavy ions with energies up to 100 GeV/nucleon in most matter. PHITS is developed and maintained by a collaboration between RIST (Research Organization for Information Science & Technology), JAEA (Japan Atomic Energy Agency), KEK (High Energy Accelerator Research Organization), Japan and Chalmers University of Technology, Sweden. For the purpose of examining the applicability of PHITS to the shielding design we have simulated the ESA facility Matroshka (MTR) designed and lead by the German Aerospace Center (DLR). Preliminary results are presented and discussed in this paper. Title: HAMLET- Human Model MATROSHKA for Radiation Exposure Determination of Astronauts Authors: Reitz, G.; Berger, T. Bibcode: 2010OLEB...40..601R Altcode: The exploration of space as seen in specific projects from the European Space Agency (ESA) for example, the search for life on Mars (ExoMars), acts as groundwork for human long duration space missions. One of the main constraints for long duration human missions, besides the psychological factors and the impact of microgravity on the human physiological system, is radiation. The radiation load on astronauts and cosmonauts in space (as for the ISS) is a factor of 100 higher than the natural radiation on earth. This radiation load will further increase should humans travel to Mars. In preparation for long duration space missions it is important to evaluate the impact of space radiation in order to secure the safety of the astronauts and minimize their radiation risks. To determine the radiation risk on humans one has to measure the radiation doses to radiosensitive organs within the human body. One way to approach this is the European Space Agencys (ESA) facility MATROSHKA (MTR) under the scientific and project lead of DLR. It is dedicated to determine the radiation load on astronauts within and outside the International Space Station (ISS), and was launched in January 2004. MTR is currently in its fourth experimental phase. MTR, which mimics a human head and torso, is an anthropomorphic phantom containing over 6,000 radiation detectors to determine the depth dose and organ dose distribution in the body. It is the largest international research initiative ever performed in the field of space dosimetry and combines the expertise of leading research institutions around the world. It consequently generates a huge pool of data of potentially immense value for research. Aiming at optimal scientific exploitation, the collaborative project HAMLET is bringing together a European expert committee, consisting exclusively of members of the MTR consortium, to process and compile the data acquired individually by the participating laboratories. Based on experimental input as well as on radiation transport calculations, a three-dimensional model for the distribution of radiation dose in an astronauts body will be built up. The results will describe the exposure conditions both for extra-vehicular activities (MTR-1, 20042005) and inside the ISS (MTR-2A/B/KIBO, 200620010). The scientific achievements contribute essentially to radiation risk estimations for future interplanetary space exploration by humans, putting them on a solid experimental and theoretical basis. Maximum public outreach is assured by making the carefully processed data and related reports directly available to the scientific community and the public via a web-based database. The HAMLET project is funded by the European Commission under the EUs Seventh Framework Programme (FP7) under Project Nr: 218817 and coordinated by the German Aerospace Center (DLR) http://www-fp7-hamlet.eu Title: A Rising Cool Column as a Signature of Helical Flux Emergence and Formation of Prominence and Coronal Cavity Authors: Okamoto, Takenori J.; Tsuneta, Saku; Berger, Thomas E. Bibcode: 2010ApJ...719..583O Altcode: 2010arXiv1006.4633O Continuous observations were performed of a quiescent prominence with the Solar Optical Telescope on board the Hinode satellite on 2006 December 23 and 24. A peculiar slowly rising column of ~104 K plasma develops from the lower atmosphere during the observations. The apparent ascent speed of the column is 2 km s-1, while the fine structures of the column exhibit much faster motion of up to 20 km s-1. The column eventually becomes a faint low-lying prominence. An overlying coronal cavity associated with the appearance of the column seen in the X-ray and EUV moves upward at ~5 km s-1. We discuss the relationship between these episodes and suggest that they are due to the emergence of a helical flux rope that undergoes reconnection with lower coronal fields, possibly carrying material into the coronal cavity. Under the assumption of the emerging flux scenario, the lower velocity of 2 km s-1 and the higher one of 20 km s-1 in the column are attributed to the rising motion of the emerging flux and to the outflow driven by magnetic reconnection between the emerging flux and the pre-existing coronal field, respectively. The present paper gives a coherent explanation of the enigmatic phenomenon of the rising column with the emergence of the helical rope and its effect on the corona. We discuss the implications that the emergence of such a helical rope has on the dynamo process in the convection zone. Title: High Survival of Rock Inhabiting Photosynthetic Organisms in a Simulated Interplanetary Transfer Authors: de la Torre, R.; Sancho, L. G.; Horneck, G.; Rettberg, P.; Berger, T.; Ascaso, C.; de los Rios, A.; Wierzchos, J.; de Vera, J. P.; Ott, S.; Cockell, C.; Olsson, K.; Frias, J. M.; Demets, R.; Onofri, S. Bibcode: 2010OLEB...40..539D Altcode: Interplanetary transfer of rock inhabiting life by means of meteorites is a step supported by the hypothesis of lithopanspermia, which argues that impact-expelled rocks from a planets surface serve as vehicles for spreading living material from one planet of the solar system to another. To test the survival of prokaryotic- and eukaryotic symbiotic organisms in relation to lithopanspermia, three experiments have been performed in space, the first two on a short mission, on board of Biopan of the Foton satellite, and the third one in a long-term mission on the EXPOSE facility of the International Space Station ISS. The first experiment, called LICHENS (May 2005), has demonstrated for the first time the high survival capacity of eukaryotic symbiotic organisms in space (bipolar epilithic lichen species Rhizocarpon geographicum and Xanthoria elegans during 16 days in BIOPAN-5). In the following experiment Lithopanspermia (Biopan-6, FOTON-M3 satellite, 14.09.07) we have pursued a more ambitious aim, to demonstrate- and intercompare the survival capacity, not only of these eukaryotic symbiotic organisms, this time also that of prokaryotic symbiotic organisms. For this test, we have selected the previously tested species R. geographicum and X. elegansbut this time prepared with- and without cortex and lichenic substances, their reproductive structures, endoevaporitic microbial communities, epilithic microbial communities with cyanobacterial akinetes of Anabaena, and a vagrant lichen species, Aspicilia fruticulosa. Exposure to different UV-conditions of a low Earth orbit (LEO, 300 km) were performed: solar extraterrestrial UV-radiation, Mars simulated UVclimate, UV-B radiation and PAR, space vacuum at 106mB, microgravity and temperatures between23C and +16C. After flight, the first analysis with chlorophyll a- fluorescence confirmed a high and fast recovery of the biological activity of A. fruticulosa and of the epilithic lichen with cortex and with lichenic substances, comparable to the high survival rates observed in the experiment Lichens (de la Torre et al. 2007; Sancho et al., 2007); a high germination capacity of the ascospores and the survival of the resting state cells of Anabaena were also observed, as also a certain level of survival of the endoevaporitic microorganisms from the halite rock (the Atacama Desert) (LIFE/DEAD assay and fluorescent microscopy). These experiments have demonstrated that organisms adapted to tolerate extreme conditions on our planet, like epilitihic lichens and resting state phototrophic organisms of microbial communities, could resist an interplanetary travel through space. The third experiment, LIFE (LIchensand Fungi Experiment), was a long term experiment (February 2008-August 2009) where desiccated lichens, fungi and cryptoendolithic communities were exposed to environmental space- and Mars simulated conditions on the EXPOSE facility of the ISS. The results will contribute to the likelihood of Lithopanspermia, demonstrating the limits for life. Title: Survival of lichens and bacteria exposed to outer space conditions - Results of the Lithopanspermia experiments Authors: de la Torre, Rosa; Sancho, Leopoldo G.; Horneck, Gerda; Ríos, Asunción de los; Wierzchos, Jacek; Olsson-Francis, Karen; Cockell, Charles S.; Rettberg, Petra; Berger, Thomas; de Vera, Jean-Pierre P.; Ott, Sieglinde; Frías, Jesus Martinez; Melendi, Pablo Gonzalez; Lucas, Maria Mercedes; Reina, Manuel; Pintado, Ana; Demets, René Bibcode: 2010Icar..208..735D Altcode: In the space experiments Lithopanspermia, experimental support was provided to the likelihood of the lithopanspermia concept that considers a viable transport of microorganisms between the terrestrial planets by means of meteorites. The rock colonising lichens Rhizocarpon geographicum and Xanthoria elegans, the vagrant lichen Aspicilia fruticulosa, and endolithic and endoevaporitic communities of cyanobacteria and bacteria with their natural rock substrate were exposed to space for 10 days onboard the Biopan facility of the European Space Agency (ESA). Biopan was closed during launch and re-entry. In addition, in the Stone facility, one sample of R. geographicum on its natural granitic substrate was attached at the outer surface of the re-entry capsule close to the stagnation point, only protected by a thin cover of glass textolite. Post-flight analysis, which included determination of the photosynthetic activity, LIVE/DEAD staining, and germination capacity of the ascospores, demonstrated that all three lichen were quite resistant to outer space conditions, which include the full spectrum of solar extraterrestrial electromagnetic radiation or selected wavelength ranges. This high resistance of the lichens to space appears to be due to their symbiotic nature and protection by their upper pigmented layer, the cortex. In contrast, the rock- or halite-inhabiting bacteria were severely damaged by the same exposure. After atmospheric re-entry, the granite of the Stone sample was transformed into a glassy, nearly homogenous material, with several friction striae. None of the lichen cells survived this re-entry process. The data suggest that lichens are suitable candidates for testing the concept of lithopanspermia, because they are extremely resistant to the harsh environment of outer space. The more critical event is the atmospheric re-entry after being captured by a planet. Experiments simulating the re-entry process of a microbe-carrying meteoroid did not show any survivors. Title: Emergence of Helical Flux and the Formation of an Active Region Filament Channel Authors: Lites, B. W.; Kubo, M.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Okamoto, T. J.; Otsuji, K. Bibcode: 2010ApJ...718..474L Altcode: We present comprehensive observations of the formation and evolution of a filament channel within NOAA Active Region (AR) 10978 from Hinode/Solar Optical Telescope and TRACE. We employ sequences of Hinode spectro-polarimeter maps of the AR, accompanying Hinode Narrowband Filter Instrument magnetograms in the Na I D1 line, Hinode Broadband Filter Instrument filtergrams in the Ca II H line and G-band, Hinode X-ray telescope X-ray images, and TRACE Fe IX 171 Å image sequences. The development of the channel resembles qualitatively that presented by Okamoto et al. in that many indicators point to the emergence of a pre-existing sub-surface magnetic flux rope. The consolidation of the filament channel into a coherent structure takes place rapidly during the course of a few hours, and the filament form then gradually shrinks in width over the following two days. Particular to this filament channel is the observation of a segment along its length of horizontal, weak (500 G) flux that, unlike the rest of the filament channel, is not immediately flanked by strong vertical plage fields of opposite polarity on each side of the filament. Because this isolated horizontal field is observed in photospheric lines, we infer that it is unlikely that the channel formed as a result of reconnection in the corona, but the low values of inferred magnetic fill fraction along the entire length of the filament channel suggest that the bulk of the field resides somewhat above the low photosphere. Correlation tracking of granulation in the G band presents no evidence for either systematic flows toward the channel or systematic shear flows along it. The absence of these flows, along with other indications of these data from multiple sources, reinforces (but does not conclusively demonstrate) the picture of an emerging flux rope as the origin of this AR filament channel. Title: Quiescent Prominence Dynamics Observed with the Hinode Solar Optical Telescope. I. Turbulent Upflow Plumes Authors: Berger, Thomas E.; Slater, Gregory; Hurlburt, Neal; Shine, Richard; Tarbell, Theodore; Title, Alan; Lites, Bruce W.; Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Magara, Tetsuya; Suematsu, Yoshinori; Shimizu, Toshifumi Bibcode: 2010ApJ...716.1288B Altcode: Hinode/Solar Optical Telescope (SOT) observations reveal two new dynamic modes in quiescent solar prominences: large-scale (20-50 Mm) "arches" or "bubbles" that "inflate" from below into prominences, and smaller-scale (2-6 Mm) dark turbulent upflows. These novel dynamics are related in that they are always dark in visible-light spectral bands, they rise through the bright prominence emission with approximately constant speeds, and the small-scale upflows are sometimes observed to emanate from the top of the larger bubbles. Here we present detailed kinematic measurements of the small-scale turbulent upflows seen in several prominences in the SOT database. The dark upflows typically initiate vertically from 5 to 10 Mm wide dark cavities between the bottom of the prominence and the top of the chromospheric spicule layer. Small perturbations on the order of 1 Mm or less in size grow on the upper boundaries of cavities to generate plumes up to 4-6 Mm across at their largest widths. All plumes develop highly turbulent profiles, including occasional Kelvin-Helmholtz vortex "roll-up" of the leading edge. The flows typically rise 10-15 Mm before decelerating to equilibrium. We measure the flowfield characteristics with a manual tracing method and with the Nonlinear Affine Velocity Estimator (NAVE) "optical flow" code to derive velocity, acceleration, lifetime, and height data for several representative plumes. Maximum initial speeds are in the range of 20-30 km s-1, which is supersonic for a ~10,000 K plasma. The plumes decelerate in the final few Mm of their trajectories resulting in mean ascent speeds of 13-17 km s-1. Typical lifetimes range from 300 to 1000 s (~5-15 minutes). The area growth rate of the plumes (observed as two-dimensional objects in the plane of the sky) is initially linear and ranges from 20,000 to 30,000 km2 s-1 reaching maximum projected areas from 2 to 15 Mm2. Maximum contrast of the dark flows relative to the bright prominence plasma in SOT images is negative and ranges from -10% for smaller flows to -50% for larger flows. Passive scalar "cork movies" derived from NAVE measurements show that prominence plasma is entrained by the upflows, helping to counter the ubiquitous downflow streams in the prominence. Plume formation shows no clear temporal periodicity. However, it is common to find "active cavities" beneath prominences that can spawn many upflows in succession before going dormant. The mean flow recurrence time in these active locations is roughly 300-500 s (5-8 minutes). Locations remain active on timescales of tens of minutes up to several hours. Using a column density ratio measurement and reasonable assumptions on plume and prominence geometries, we estimate that the mass density in the dark cavities is at most 20% of the visible prominence density, implying that a single large plume could supply up to 1% of the mass of a typical quiescent prominence. We hypothesize that the plumes are generated from a Rayleigh-Taylor instability taking place on the boundary between the buoyant cavities and the overlying prominence. Characteristics, such as plume size and frequency, may be modulated by the strength and direction of the cavity magnetic field relative to the prominence magnetic field. We conclude that buoyant plumes are a source of quiescent prominence mass as well as a mechanism by which prominence plasma is advected upward, countering constant gravitational drainage. Title: Astrobiological Aspects of the Mutagenesis of Cosmic Radiation on Bacterial Spores Authors: Moeller, Ralf; Reitz, Günther; Berger, Thomas; Okayasu, Ryuichi; Nicholson, Wayne L.; Horneck, Gerda Bibcode: 2010AsBio..10..509M Altcode: Based on their unique resistance to various space parameters, Bacillus endospores are one of the model systems used for astrobiological studies. In this study, spores of B. subtilis were used to study the effects of galactic cosmic radiation (GCR) on spore survival and induced mutagenesis. In interplanetary space, outside Earth's protective magnetic field, spore-containing rocks would be exposed to bombardment by high-energy charged particle radiation from galactic sources and from the Sun, which consists of photons (X-rays, γ rays), protons, electrons, and heavy, high-energy charged (HZE) particles. B. subtilis spores were irradiated with X-rays and accelerated heavy ions (helium, carbon, silicon and iron) in the linear energy transfer (LET) range of 2-200 keV/μm. Spore survival and the rate of the induced mutations to rifampicin resistance (RifR) depended on the LET of the applied species of ions and radiation, whereas the exposure to high-energy charged particles, for example, iron ions, led to a low level of spore survival and increased frequency of mutation to RifR compared to low-energy charged particles and X-rays. Twenty-one RifR mutant spores were isolated from X-ray and heavy ion-irradiated samples. Nucleotide sequencing located the RifR mutations in the rpoB gene encoding the β-subunit of RNA polymerase. Most mutations were primarily found in Cluster I and were predicted to result in amino acid changes at residues Q469L, A478V, and H482P/Y. Four previously undescribed alleles in B. subtilis rpoB were isolated: L467P, R484P, and A488P in Cluster I and H507R in the spacer between Clusters I and II. The spectrum of RifR mutations arising from spores exposed to components of GCR is distinctly different from those of spores exposed to simulated space vacuum and martian conditions. Title: Direct Imaging of an Emerging Flux Rope and a Resulting Chromospheric Jet Observed by Hinode Authors: Liu, Wei; Berger, T.; Title, A. M.; Tarbell, T. D.; DeRosa, M. Bibcode: 2010AAS...21640307L Altcode: 2010BAAS...41R.878L Magnetic flux emergence has been traditionally observed on the disk by identifying changes in magnetograms. Observations near the limb offer an alternative perspective and allow direct imaging of emerging flux ropes. We present Hinode/SOT Ca II H observations of such an event in an equatorial coronal hole on 2007 February 9. The precursor of the event was a bundle of fine material threads that extended at an oblique angle above the chromosphere and appeared to rotate about a common axis. This bundle first slowly and then rapidly swung up, accompanied by a loop that appeared at the base of the bundle and expanded at comparable rates. During the first (slow rise) stage, the apex of the loop ascended at 16 km/s, a velocity similar to that of H-alpha arch filaments (e.g., Chou & Zirin) and of emerging flux ropes expanding into the corona as found in MHD simulations (e.g., Fan & Gibson; Martinez-Sykora). The second stage started at the onset of a GOES A5 flare and the loop expansion accelerated, reaching a velocity of 130 km/s when the loop appeared to rupture near the peak of the flare. The material bundle then swung back in a whiplike manner and developed into a collimated jet, exhibiting oscillatory transverse motions across its axis, as expected from unwinding twists. Some jet material fell back along smooth streamlines, which bypass an unseen dome and presumably a null point in the low corona, depicting an inverted-Y shape. Some of these observations resemble the model (e.g., Uchida & Shibata) of the emergence of a twisted flux rope into an open field region that leads to reconnection and formation of a jet. Some observations are, however, not predicted in previous models and we will discuss their implications. Title: Quasistable radiation belt in the slot region Authors: Labrenz, Johannes; Burmeister, Sönke; Berger, Thomas; Reitz, Günther; Heber, Bernd; Beaujean, Rudolf Bibcode: 2010EGUGA..1210920L Altcode: MATROSHKA is an ESA experiment under leadership of DLR Cologne. The radiation exposure inside a human phantom is measured by active and passive detectors. The DOSimetry TELescope (DOSTEL) was built at CAU Kiel in cooperation with DLR Cologne; it consists of two Si-semiconductor detectors forming a telescope. Count rates as well as energy deposit spectra are measured by this instrument. MATROSHKA is on board ISS since January 2004. The active instruments were operating during the first mission phase (MTR1) where the phantom was mounted outside the ISS from February 2004 to august 2005. In 2008 the active instruments were operating again in another mission phase (MTR2b). During (MTR2b) MATROSHKA was mounted inside the Service Module of the ISS. The DOSTEL measurements shows the expected transits through the inner radiation belt (SAA) over the South Atlantic and transits through the outer radiation belt at the highest geomagnetic latitudes. In Sept. and Oct. 2004 an additional radiation belt in the so called slot region appeared. In this work the measurements of this quasi stable slot region belt will be presented and compared to results of other experiments. Title: Inside the Meteorite — Bacterial Spore Survival After Exposure to Galactic Cosmic Radiation Authors: Moeller, R.; Berger, T.; Matthiä, D.; Okayasu, R.; Kato, T.; Kitamura, H.; Reitz, G. Bibcode: 2010LPICo1538.5218M Altcode: Based on their unique resistance to various space parameters, bacterial spores are one of the model systems used for astrobiological studies. In our research, we studied the response of Bacillus subtilis spores to the exposure of galactic cosmic radiation. Title: On the power spectrum of solar surface flows Authors: Rieutord, M.; Roudier, T.; Rincon, F.; Malherbe, J. -M.; Meunier, N.; Berger, T.; Frank, Z. Bibcode: 2010A&A...512A...4R Altcode: 2009arXiv0911.3319R Context. The surface of the Sun provides us with a unique and very detailed view of turbulent stellar convection. Studying its dynamics can therefore help us make significant progress in stellar convection modelling. Many features of solar surface turbulence like the supergranulation are still poorly understood.
Aims: The aim of this work is to give new observational constraints on these flows by determining the horizontal scale dependence of the velocity and intensity fields, as represented by their power spectra, and to offer some theoretical guidelines to interpret these spectra.
Methods: We use long time-series of images taken by the Solar Optical Telescope (SOT) on board the Hinode satellite; we reconstruct both horizontal (by granule tracking) and vertical (by Doppler effect) velocity fields in a field-of-view of ~ 75 × 75 Mm2. The dynamics in the subgranulation range can be investigated with unprecedented precision thanks to the absence of seeing effects and the use of the modulation transfer function of SOT for correcting the spectra.
Results: At small subgranulation scales down to 0.4 Mm the spectral density of kinetic energy associated with vertical motions exhibits a k-10/3-like power law, while the intensity fluctuation spectrum follows either a k-17/3 or a k-3-like power law at the two continuum levels investigated (525 and 450 nm respectively). We discuss the possible physical origin of these scalings and interpret the combined presence of k-17/3 and k-10/3 power laws for the intensity and vertical velocity as a signature of buoyancy-driven turbulent dynamics in a strongly thermally diffusive regime. In the mesogranulation range and up to a scale of 25 Mm, we find that the amplitude of the vertical velocity field decreases like λ-3/2 with the horizontal scale λ. This behaviour corresponds to a k2 spectral power law. Still in the 2.5-10 Mm mesoscale range, we find that intensity fluctuations in the blue continuum also follow a k2 power law. In passing we show that granule tracking cannot sample scales below 2.5 Mm. We finally further confirm the presence of a significant supergranulation energy peak at 30 Mm in the horizontal velocity power spectrum and show that the emergence of a pore erases this spectral peak. We tentatively estimate the scale height of the vertical velocity field in the supergranulation range and find 1 Mm; this value suggests that supergranulation flows are shallow. Title: Relative nuclear abundances in ISS with Altcriss experiment Authors: Casolino, Marco; Picozza, Piergiorgio; Narici, Livio; Pugliese, Mariagabriella; Durante, Marco; di Fino, Luca; Zaconte, Veronica; Nagamatsu, Aiko; Berger, Thomas; Benghin, Victor; Sihver, Lembit; Lobascio, Cesare Bibcode: 2010cosp...38.3199C Altcode: 2010cosp.meet.3199C The Altcriss project aims to perform a long term survey of the radiation environment on board the International Space Station. Measurements were performed with active and passive devices in different locations and orientations of the Russian segment of the station. The goal is to perform a detailed evaluation of the differences in particle fluence and nuclear composition due to different shielding material and attitude of the station. The Sileye-3/Alteino detector is used to identify nuclei up to Iron in the energy range above ' 60 MeV/n. Several passive dosimeters (TLDs, CR39) are also placed in the same location of Sileye-3 detector. Polyethylene shielding is periodically interposed in front of the detectors to evaluate the effectiveness of shielding on the nuclear component of the cosmic radiation. In this work we will discuss results obtained with active and passive detectors in various location of the station during expedition 12 to 16. Title: Dosimetry of charged and neutral particles onboard a stratospheric balloon Authors: Dönsdorf, Esther Miriam; Burmeister, Soenke; Heber, Bernd; Benton, Eric; Berger, Thomas Bibcode: 2010cosp...38.3225D Altcode: 2010cosp.meet.3225D The interaction of the primary galactic cosmic rays with constituents of the atmosphere leads to a complex secondary radiation field at high altitudes. Of special interest for aviation and thereby also for radiation protection is the height up to 30 km where the radiation field consists of charged and neutral particles. For the determination of the dose rates up to this altitude in the Earth's atmosphere a stratopheric balloon flight will be performed in central Oklahoma which has a cutoff rigidity of about 4 GV. Onboard there will be two different active radiation detector systems to measure the dose of charged and neutral particles in the stratosphere. The first one is a silicon telescope which consists of two 2 cm2 silicon PIN-photodiodes used as semiconductor detectors. This instrument will mainly be used to measure the charged component of the radiation field due to the fact that the silicon detectors have a rather low efficiency for the detection of neutrons and gammas with energies higher than 60 keV. The second instrument is a so called phoswich detector. It is composed of two dissimilar scintillators optically coupled to each other and to a common photomultiplier tube. For this experimental setup a combination of a fast plastic scintillator BC412 and a slow inorganic scintillator CsI(Na) is used. The pulses from the two scintillators will be separated by applying pulse shape analysis. These two different scintillator materials have been chosen because BC412 is hydrogen rich and thus the cross section for fast neutrons is relatively high and CsI(Na) has a high cross section for gamma radiation. The objective of the phoswich detector is to distinguish between gammas and neutrons but it is also possible to measure charged particles with this setup. The aim of the balloon flight is to determine the dose measured with these two different instruments and in particular to differentiate between the dose induced by charged particles and by the different neutral components of the secondary radiation field at high altitudes. A description of the concept and the assembly of the two instruments as well as first calibration results will be presented. Title: MHD simulations of upflows in the Kippenhahn-Schlueter prominence model Authors: Hillier, Andrew; Shibata, Kazunari; Isobe, Hiroaki; Berger, Thomas Bibcode: 2010cosp...38.2914H Altcode: 2010cosp.meet.2914H The launch of SOT on the Hinode satellite, with it's previously unprecedented high resolution, high cadence images of solar prominences, led to the discovery of small scale, highly dynamic flows in quiescent prominences. Berger et al. (2008) reported dark upflows that propagated from the base of the prominence through a height of approximately 10 Mm before ballooning into the familiar mushroom shape often associated with the Rayleigh-Taylor instability. Whether such phenomena can be driven by instabilities and, if so, how the instability evolve is yet to be fully investigated. In this study, we use the Kippenhahn-Schlueter (K-S) prominence model as the base for 3D numerical MHD simulations. The K-S prominence model is linearly stable for ideal MHD perturbationss, but can be made unstable through nonlinear perturbations, which we impose through inserting a low density (high temperature) tube through the centre of the prominence. Our simulations follow the linear and nonlinear evolution of upflows propagating from the hot tube through the K-S prominence model. We excited Rayleigh-Taylor like modes inside the K-S model with a wave along the contact discontinuity created between the hot tube and the K-S prominence, and solved the pertur-bations of this system. For such a complex setting, the linear evolution of the instability has 0.7 not been studied, and we found the growth rate to be ∼ ( ρ+ -ρ- - 0.05)k 0.22 . The most ρ+ +ρ- unstable wavelength was ∼ 100 km which, through the inverse cascade process, created upflows of ∼ 300 km. The rising plumes obtained a constant rise velocity in the nonlinear stage due to the creation of adverse magnetic and gas pressure gradients at the top of the plume. Title: Determination of nuclear tracks parameters on sequentially etched PADC detectors Authors: Horwacik, Tomasz; Bilski, Pawel; Koerner, Christine; Facius, Rainer; Berger, Thomas; Nowak, Tomasz; Reitz, Guenther; Olko, Pawel Bibcode: 2010cosp...38.3227H Altcode: 2010cosp.meet.3227H Polyallyl Diglycol Carbonate (PADC) detectors find many applications in radiation protection. One of them is the cosmic radiation dosimetry, where PADC detectors measure the linear energy transfer (LET) spectra of charged particles (from protons to heavy ions), supplementing TLD detectors in the role of passive dosemeter. Calibration exposures to ions of known LET are required to establish a relation between parameters of track observed on the detector and LET of particle creating this track. PADC TASTRAK nuclear track detectors were exposed to 12 C and 56 Fe ions of LET in H2 O between 10 and 544 keV/µm. The exposures took place at the Heavy Ion Medical Accelerator (HIMAC) in Chiba, Japan in the frame of the HIMAC research project "Space Radiation Dosimetry-Ground Based Verification of the MATROSHKA Facility" (20P-240). Detectors were etched in water solution of NaOH with three different temperatures and for various etching times to observe the appearance of etched tracks, the evolution of their parameters and the stability of the etching process. The applied etching times (and the solution's concentrations and temperatures) were: 48, 72, 96, 120 hours (6.25 N NaOH, 50 O C), 20, 40, 60, 80 hours (6.25 N NaOH, 60 O C) and 8, 12, 16, 20 hours (7N NaOH, 70 O C). The analysis of the detectors involved planimetric (2D) measurements of tracks' entrance ellipses and mechanical measurements of bulk layer thickness. Further track parameters, like angle of incidence, track length and etch rate ratio were then calculated. For certain tracks, results of planimetric measurements and calculations were also compared with results of optical track profile (3D) measurements, where not only the track's entrance ellipse but also the location of the track's tip could be directly measured. All these measurements have been performed with the 2D/3D measurement system at DLR. The collected data allow to create sets of V(LET in H2 O) calibration curves suitable for short, intermediate and long etching time and will be use during analysis of detectors exposed on the International Space Station during DOSIS and MATROSHKA experiments. The help and support of Yukio Uchihori and Hisashi Kitamura during the irradiations at HIMAC is highly appreciated. This work was supported by the Polish Ministry of Science and Higher Education, grants: No N N505 261535 and No. DWM/N118/ESA/2008. Title: A droplet model for downflows in hedgerow prominences Authors: Haerendel, Gerhard; Berger, Thomas Bibcode: 2010cosp...38.2915H Altcode: 2010cosp.meet.2915H Observations of hedgerow prominences with the Solar Optical Telescope of the Hinode mission have revealed the ubiquitous existence of downflows forming coherent thin and highly structured near-vertical threads with velocities between 10 and 20 km/s. Their widths range between 300 and 500 km. They are often initiated at the top of the visible prominence, but sometimes also at intermediate level. We propose that the downflows are made of plasma packets that squeeze themselves through the dominantly horizontal field under the action of gravity. Their origin is assumed to be hot plasma either supplied from outside along the arcade field overarching the prominence and condensing at its top, or along the spine field of the prominence itself. Under compression and further cooling, the matter sinks into the prominence dragging its magnetic field with it, but eventually disconnecting it from the arcade field thus forming finite packets. The horizontal prominence field exerts a drag force on the downward moving packets like air on a falling droplet. Balancing the gravitational and drag forces yields an upper limit on their length of the order of 1000 km. Lateral pressure balance limits their width to about 500 km. Pushing themselves at high speed through the horizontal field, the plasma "droplets" excite a multitude of incoherent Alfvén waves. Nonlinear interactions of these waves fill the prominence with a spectrum of oscillatory and propagating wave modes. Absorption of part of that wave energy, whose ultimate source is gravitational energy, and radiative cooling constitute the energy balance of the falling matter and determine the mean fall speed ( 14 km/s). The small scales of the "droplets" and thus of their frozen-in magnetic fields explain the absence of vertical components in magnetic field measurements. The above estimates of the droplet characteristics rest on prominence parameters with mean density of 2.5x1012 cm-3, temperature of 7500 K, and horizontal fields of order 8 G. Title: MATSIM -The Development and Validation of a Numerical Voxel Model based on the MATROSHKA Phantom Authors: Beck, Peter; Rollet, Sofia; Berger, Thomas; Bergmann, Robert; Hajek, Michael; Latocha, Marcin; Vana, Norbert; Zechner, Andrea; Reitz, Guenther Bibcode: 2010cosp...38.3204B Altcode: 2010cosp.meet.3204B The AIT Austrian Institute of Technology coordinates the project MATSIM (MATROSHKA Simulation) in collaboration with the Vienna University of Technology and the German Aerospace Center. The aim of the project is to develop a voxel-based model of the MATROSHKA anthro-pomorphic torso used at the International Space Station (ISS) as foundation to perform Monte Carlo high-energy particle transport simulations for different irradiation conditions. Funded by the Austrian Space Applications Programme (ASAP), MATSIM is a co-investigation with the European Space Agency (ESA) ELIPS project MATROSHKA, an international collaboration of more than 18 research institutes and space agencies from all over the world, under the science and project lead of the German Aerospace Center. The MATROSHKA facility is designed to determine the radiation exposure of an astronaut onboard ISS and especially during an ex-travehicular activity. The numerical model developed in the frame of MATSIM is validated by reference measurements. In this report we give on overview of the model development and compare photon and neutron irradiations of the detector-equipped phantom torso with Monte Carlo simulations using FLUKA. Exposure to Co-60 photons was realized in the standard ir-radiation laboratory at Seibersdorf, while investigations with neutrons were performed at the thermal column of the Vienna TRIGA Mark-II reactor. The phantom was loaded with passive thermoluminescence dosimeters. In addition, first results of the calculated dose distribution within the torso are presented for a simulated exposure in low-Earth orbit. Title: The DOSIS -Experiment onboard the Columbus Laboratory of the International Space Station -First Mission Results from the Active DOSTEL Instruments Authors: Burmeister, Soenke; Berger, Thomas; Beaujean, Rudolf; Boehme, Matthias; Haumann, Lutz; Kortmann, Onno; Labrenz, Johannes; Reitz, Guenther Bibcode: 2010cosp...38.3195B Altcode: 2010cosp.meet.3195B Besides the effects of the microgravity environment, and the psychological and psychosocial problems encountered in confined spaces, radiation is the main health detriment for long dura-tion human space missions. The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones encountered on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station ISS is therefore needed. For the investigation of the spatial and temporal distribution of the radiation field inside the European COLUMBUS module the DLR experiment DOSIS (Dose Distribution Inside the ISS) was launched on July 15th 2009 with STS-127 to the ISS. The experimental package was transferred from the Space Shuttle into COLUMBUS on July 18th. It consists in a first part of a combination of passive detector packages (PDP) distributed at 11 locations inside the European Columbus Laboratory. The second part are two active radiation detectors (DOSTELs) with a DDPU (DOSIS Data and Power Unit) in a nomex pouch (DOSIS MAIN BOX) mounted at a fixed location beneath the European Physiology Module (EPM) inside COLUMBUS. After the successful installation the active part has been activated on the 18th July 2009. Each of the DOSTEL units consists of two 6.93 cm PIPS silicon detectors forming a telescope with an opening angle of 120. The two DOSTELs are mounted with their telescope axis perpendicular to each other to investigate anisotropies of the radiation field inside the COLUMBUS module especially during the passes through the South Atlantic Anomaly (SAA) and during Solar Particle Events (SPEs). The data from the DOSTEL units are transferred to ground via the EPM rack which is activated approximately every four weeks for this action. The first data downlink was performed on July 31st 2009. First Results for the DOSTEL measurements such as count rate profiles, dose rates and LET spectra will be presented in comparison to the data obtained by other experiments. Title: Depth dose distribution study within a phantom torso after irradiation with a simulated Solar Particle Event at NSRL Authors: Berger, Thomas; Matthiä, Daniel; Koerner, Christine; George, Kerry; Rhone, Jordan; Cucinotta, Francis A.; Reitz, Guenther Bibcode: 2010cosp...38.3205B Altcode: 2010cosp.meet.3205B The adequate knowledge of the radiation environment and the doses incurred during a space mission is essential for estimating an astronaut's health risk. The space radiation environment is complex and variable, and exposures inside the spacecraft and the astronaut's body are com-pounded by the interactions of the primary particles with the atoms of the structural materials and with the body itself. Astronauts' radiation exposures are measured by means of personal dosimetry, but there remains substantial uncertainty associated with the computational extrap-olation of skin dose to organ dose, which can lead to over-or under-estimation of the health risk. Comparisons of models to data showed that the astronaut's Effective dose (E) can be pre-dicted to within about a +10In the research experiment "Depth dose distribution study within a phantom torso" at the NASA Space Radiation Laboratory (NSRL) at BNL, Brookhaven, USA the large 1972 SPE spectrum was simulated using seven different proton energies from 50 up to 450 MeV. A phantom torso constructed of natural bones and realistic distributions of human tissue equivalent materials, which is comparable to the torso of the MATROSHKA phantom currently on the ISS, was equipped with a comprehensive set of thermoluminescence detectors and human cells. The detectors are applied to assess the depth dose distribution and radiation transport codes (e.g. GEANT4) are used to assess the radiation field and interactions of the radiation field with the phantom torso. Lymphocyte cells are strategically embedded at selected locations at the skin and internal organs and are processed after irradiation to assess the effects of shielding on the yield of chromosome damage. The first focus of the pre-sented experiment is to correlate biological results with physical dosimetry measurements in the phantom torso. Further on the results of the passive dosimetry using the anthropomorphic phantoms represent the best tool to generate reliable to benchmark computational radiation transport models in a radiation field of interest. The presentation will give first results of the physical dose distribution, the comparison with GEANT4 computer simulations, based on a Voxel model of the phantom, and a comparison with the data from the chromosome aberration study. The help and support of Adam Russek and Michael Sivertz of the NASA Space Radiation Laboratory (NSRL), Brookhaven, USA during the setup and the irradiation of the phantom are highly appreciated. The Voxel model describing the human phantom used for the GEANT4 simulations was kindly provided by Monika Puchalska (CHALMERS, Gothenburg, Sweden). Title: Simulation of the radiation exposure in space during a large solar energetic particle event with GEANT4 Authors: Matthiä, Daniel; Berger, Thomas; Puchalska, Monika; Reitz, Guenther Bibcode: 2010cosp...38.3226M Altcode: 2010cosp.meet.3226M The radiation field in space is complex due to the various contributing sources and astronauts at the International Space Station (ISS) in low Earth orbit or beyond are exposed to significantly increased doses compared to on ground or in the lower atmosphere. The main sources of the increased radiation level are Galactic Cosmic Ray (GCR) particles, mainly fully charged ions from hydrogen to iron with energies up to hundreds of GeV per nucleon and more, trapped protons from the radiation belts with energies up to several hundreds of MeV, and solar energetic particles up to several GeV released in large eruptions on the sun related to solar x-ray flares and coronal mass ejections. While the intensities of Galactic Cosmic Rays and trapped protons are relatively stable and changing slowly over the solar cycle, solar energetic particle events last for several hours up to days and are characterized by strong increases in the particle intensity. The radiation exposure during a large particle event can be very harmful to astronauts especially during extra vehicular activities and outside the protective magnetic field of the Earth. The MATROSHKA human phantom was and is used on the International Space Station to measure the radiation exposure in and outside ISS in order to evaluate the radiation risk in low Earth orbit. A voxel-based description of the MATROSHKA phantom (NUNDO-Numerical RANDO Model) was used in the present work to numerically estimate the radiation exposure of the human body and the individual organs during a large solar particle event. The transport of primary protons following an exponential energy distribution was simulated in order to calculate the energy deposition and organ doses in the MATROSHKA phantom during such an event taking into account different amounts of shielding provided by a surrounding aluminum shell. The primary particle energy distribution used in this work follows the description of the spectrum of the solar energetic particle event in August 1972 in the energy range from 45 MeV to 1 GeV. The transport calculations of the energetic particles through the shielding and the phantom model were performed using the Monte-Carlo code GEANT4. Title: HAMLET -Human Model MATROSHKA for Radiation Exposure Determination of Astronauts -Current status and results Authors: Reitz, Guenther; Berger, Thomas; Bilski, Pawel; Burmeister, Soenke; Labrenz, Johannes; Hager, Luke; Palfalvi, Jozsef K.; Hajek, Michael; Puchalska, Monika; Sihver, Lembit Bibcode: 2010cosp...38.3202R Altcode: 2010cosp.meet.3202R The exploration of space as seen in specific projects from the European Space Agency (ESA) acts as groundwork for human long duration space missions. One of the main constraints for long duration human missions is radiation. The radiation load on astronauts and cosmonauts in space (as for the ISS) is a factor of 100 higher than the natural radiation on Earth and will further increase should humans travel to Mars. In preparation for long duration space missions it is important to evaluate the impact of space radiation in order to secure the safety of the astronauts and minimize their radiation risks. To determine the radiation risk on humans one has to measure the radiation doses to radiosensitive organs within the human body. One way to approach this is the ESA facility MATROSHKA (MTR), under the scientific and project lead of DLR. It is dedicated to determining the radiation load on astronauts within and outside the International Space Station (ISS), and was launched in January 2004. MTR is currently preparing for its fourth experimental phase inside the Japanese Experimental Module (JEM) in summer 2010. MTR, which mimics a human head and torso, is an anthropomorphic phantom containing over 6000 radiation detectors to determine the depth dose and organ dose distribution in the body. It is the largest international research initiative ever performed in the field of space dosimetry and combines the expertise of leading research institutions around the world, thereby generating a huge pool of data of potentially immense value for research. Aiming at optimal scientific exploitation, the FP7 project HAMLET aims to process and compile the data acquired individually by the participating laboratories of the MATROSHKA experiment. Based on experimental input from the MATROSHKA experiment phases as well as on radiation transport calculations, a three-dimensional model for the distribution of radiation dose in an astronaut's body will be built up. The scientific achievements contribute essentially to radiation risk estimations for future interplanetary space exploration by humans, putting them on a solid experimental and theoretical basis. The talk will give an overview of the current status of the MATROSHKA data evaluation and results and comparisons of the first three MTR experimental phases (MTR-1, 2A and 2B). The HAMLET project is funded by the European Commission under the EUs Seventh Frame-work Programme (FP7) under Project Nr: 218817 and coordinated by the German Aerospace Center (DLR) http://www-fp7-hamlet.eu Title: Hinode/SOT Measurements of Flows and Waves in Solar Prominences Authors: Berger, Thomas; Okamoto, Takenori; Schmieder, Brigitte Bibcode: 2010cosp...38.2913B Altcode: 2010cosp.meet.2913B We review Hinode Solar Optical Telescope (SOT) measurements of flows and waves in quies-cent and active solar prominences. In quiescent prominences, Hinode/SOT observations have revealed a new mode of buoyant transport in the form of dark upflows that originate at the chromospheric base of the prominence. The upflows can take the form of large-scale (10 Mm) "bubbles" that rise through the entire prominence into the overlying coronal cavity, or they can take the form of numerous small-scale (1 Mm) plumes that generate from an apparent Rayleigh-Taylor instability on the boundary between the prominence and the impinging buoy-ant flow system. The episodic flows directly inject mass, magnetic flux, and helicity into the overlying coronal cavity, moving the system towards destabilization and eruption in the form of CMEs. Hinode/SOT quiescent prominence observations have also verified the existence of ubiquitous downflow streams and vortex flows confirming that prominences are far from magne-tostatic conditions. Tracking and doppler measurements of prominence downflows find speeds of 5-15 km s-1 and imply that the trajectories are not strictly vertical. Active region promi-nence studies find counter-streaming flows along horizontal magnetic field lines with velocities of 20-30 km s-1 ; upflows, downflow streams, and rotational flows have not been observed in these systems. Active Region prominence field lines exhibit transverse oscillations indicative of Alfv`n waves with periods of several minutes, amplitudes of 1 Mm, and wavelengths of 250 Mm or more. These properties are consistent with magnetic field strengths of 50 gauss or more at typical prominence density conditions and carry enough energy to heat the surrounding prominence/corona transition region (PCTR). Title: Space activities and radiation protection of crew members Authors: Straube, Ulrich; Berger, Thomas; Reitz, Guenther; Facius, Rainer; Reiter, Thomas; Kehl, Marcel; Damann, M. D. Volker; Tognini, Michel Bibcode: 2010cosp...38.3193S Altcode: 2010cosp.meet.3193S Personnel working as crew in space-based activities e.g. professional astronauts and cosmo-nauts but also -to a certain extend-space flight participants ("space tourists"), demand health and safety considerations that have to include radiation protection measures. The radiation environment that a crew is exposed to during a space flight, differs significantly to that found on earth including commercial aviation, mainly due to the presence of heavy charged particles with great potential for biological damage. The exposure exceeds those routinely received by terrestrial radiation workers. A sequence of activities has to be conducted targeting to mitigate adverse effects of space radiation. Considerable information is available and applied through the joint efforts of the Space Agencies that are involved in the operations of the International Space Station, ISS. This presentation will give an introduction to the current measures for ra-diation monitoring and protection of astronauts of the European Space Agency (ESA). It will include information: on the radiation protection guidelines that shall ensure the proper imple-mentation and execution of radiation protection measures, the operational hardware used for radiation monitoring and personal dosimetry on ISS, as well as information about operational procedures that are applied. Title: HAMLET -Matroshka IIA and IIB experiments aboard the ISS: comparison of organ doses Authors: Kato, Zoltan; Reitz, Guenther; Berger, Thomas; Bilski, Pawel; Hajek, Michael; Sihver, Lembit; Palfalvi, Jozsef K.; Hager, Luke; Burmeister, Soenke Bibcode: 2010cosp...38.3219K Altcode: 2010cosp.meet.3219K The Matroshka experiments and the related FP7 HAMLET project aimed to study the dose burden of the cosmic rays in the organs of the crew working inside and outside the ISS. Two of the experiments will be discussed. They were performed in two different locations inside the ISS: during the Matroshka 2A (in 2006) the phantom was stored in the Russian Docking Module (Pirs), while during the Matroshka 2B (in 2007-08) it was inside the Russian Service Module (Zvezda). Both experiments were performed in the decreasing phase of the solar cycle. Solid state nuclear track detectors (SSNTD) were applied to investigate the dose contribution of the high LET radiation above ∼10 keV/µm. Two configurations of SSNTDs stacks were constructed: one for the exposure in the so called organ dose boxes (in the lung and kidney), another one for the skin dose measurements, embedded in the nomex poncho of the Phantom. In addition a reference package was placed outside the phantom. After exposure the detectors were transferred to the Earth for data evaluation. Short and long etching procedures were applied to distinguish the high and low LET particles, respectively. The particle tracks were evaluated by a semi automated image analyzer. Addi-tionally manual track parameter measurements were performed on very long tracks. As the result of measurements the LET spectra were deduced. Based on these spectra, the absorbed dose, the dose equivalent and the mean quality factor were calculated. The configuration of the stacks, the methods of the calibration and evaluation and finally the results will be presented and compared. The multiple etching and the combined evaluation method allowed to determine the fraction of the dose originated from HZE particles (Z>2 and range > major axis). Further on, data eval-uation was performed to separate the secondary particles (target fragments) from the primary particles. Although the number of high LET particles above a ∼80 keV/µm was found to be higher during the Matroshka 2B experiment than in the previous phase it was not possible to attribute this observation to the lower Sun activity in 2008, since the locations inside the ISS were different. The HAMLET project is funded by the European Commission under the EUs Seventh Frame-work Programme (FP7) under Project Nr: 218817 and coordinated by the German Aerospace Center (DLR) http://www-fp7-hamlet.eu Title: Dosimetry and Vibration measurements in BIOLAB and EMCS (Dos-ViBE) Authors: Ideström, Johan Olof; Hendrik Anken, Ralf; Reitz, Guenther; Berger, Thomas; Hauslage, Jens; Schuber, Marianne; Fossum, Knut R.; Vanhavere, Filip Bibcode: 2010cosp...38.3217I Altcode: 2010cosp.meet.3217I Space irradiation and vibrations in even small dosages can impact biological experiments and have not yet been measured in the biological payloads of the Columbus module at the Interna-tional Space Station (ISS). Installing active dosimeters and accelerometers in the Experiment Containers (EC) of Biolab and the European Modular Cultivation System (EMCS), to sur-vey in-situ the radiation and vibrations in these facilities, should be performed to serve as a reference of the space conditions to future experiments. To monitor the radiation field, the space radiation should be measured with an active dosime-ter inside the Multi-User-Facilities, as close to the actual shielding conditions of the biological experiments as possible. To measure the full spectrum of vibration frequencies, several instru-ments with different measurement ranges and sensitivity should be combined. The radiation and vibrations should be measured simultaneously in Biolab and EMCS to compare their radiation shielding and sensitivities to vibrations from the ISS. The radiation could also be measured with passive dosimeters. On the one hand this would be a back-up to the active dosimeter and on the other hand it would provide additional data since the passive dosimeters can give additional information on the radiation LET spectrum. As a response to ESA's Announcement of Opportunity (ILSRA-2009), a joint experiment in Biolab and EMCS, entitled Dos-ViBE, was proposed by the co-authors. The objectives and experimental flow of Dos-ViBE are outlined in this presentation. Title: Bacterial spore survival after exposure to HZE particle bombardment -implication for the lithopanspermia hypothesis. Authors: Moeller, Ralf; Berger, Thomas; Matthiä, Daniel; Okayasu, Ryuichi; Kitamura, H.; Reitz, Guenther Bibcode: 2010cosp...38.3313M Altcode: 2010cosp.meet.3313M Based on their unique resistance to various space parameters, bacterial spores (mainly spores of Bacillus subtilis) are one of the model systems used for astrobiological studies. More re-cently, spores of B. subtilis have been applied for experimental research on the likelihood of interplanetary transfer of life. Since its first postulation by Arrhenius in 1903, the pansper-mia hypothesis has been revisited many-times, e.g. after the discovery of several lunar and Martian meteorites on Earth [1,2]. These information provided intriguing evidence that rocks may naturally be transferred between the terrestrial planets. The scenario of panspermia, now termed "lithopanspermia" involves three basic hypothetical steps: (i) the escape process, i.e. removal to space of biological material, which has survived being lifted from the surface to high altitudes; (ii) interim state in space, i.e., survival of the biological material over time scales comparable with interplanetary or interstellar passage; (iii) the entry process, i.e. nondestruc-tive deposition of the biological material on another planet [2]. In our research, spores of B. subtilis were used to study the effects of galactic cosmic radiation on spore survival and induced mutations. On an interplanetary journey, outside a protective magnetic field, spore-containing rocks would be exposed to bombardment by high-energy charged particle radiation from galac-tic sources and from the sun. Air-dried spore layers on three different host materials (i.e., non-porous igneous rocks (gabbro), quartz, and spacecraft analog material (aluminum)) were irradiated with accelerated heavy ions (Helium and Iron) with a LET (linear energy transfer) ˆ of 2 and 200 keV/Am, at the Heavy Ion Medical Accelerator (HIMAC) at the National In-stitute of Radiological Sciences, (NIRS), Chiba, Japan in the frame of the HIMAC research project 20B463 "Characterization of heavy ion-induced damage in Bacillus subtilis spores and their global transcriptional response during spore germination" (Moeller et al., 2008 [3]). To simulate the interplanetary journey of a meteorite, stacks of spore-samples on gabbro slides in different depths were exposed. Spore survival and the rate of the induced mutations (i.e., sporulation-deficiency (Spo-)) depended on the LET of the applied species of ions as well as on the location (and depth) of the irradiated spores in the artificial meteorite. The exposure to high LET iron ions led to a low level of spore survival and increased frequency of mutation to Spo-compared to low-energy charged particles compared to the low LET helium ions. In order to obtain insights on the role of DNA repair by nonhomologous end joining (NHEJ), homologous recombination (HR) and apurinic/apyrimidinic (AP) endonucleases in B. subtilis spore resistance to high-energy charged particles has been studied in parallel. Spores deficient in NHEJ and AP endonucleases were significantly more sensitive to HZE particle bombardment than were the HR-mutant and wild-type spores, indicating that NHEJ and AP endonucleases provide DNA break repair pathways during spore germination. ((References: [1] Arrhenius, S. 1903. Die Verbreitung des Lebens im Weltenraum. Umschau 7:481-485.; [2] Nicholson, W. L. 2009. Ancient micronauts: interplanetary transport of microbes by cosmic impacts. Trends Mi-crobiol. 17:243-250.; [3] Moeller, R., P. Setlow, G. Horneck, T. Berger, G. Reitz, P. Rettberg, A. J. Doherty, R. Okayasu, and W. L. Nicholson. 2008. Roles of the major, small, acid-soluble spore proteins and spore-specific and universal DNA repair mechanisms in resistance of Bacillus subtilis spores to ionizing radiation from X-rays and high-energy charged-particle bombardment. J. Bacteriol. 190:1134-1140.)) Title: Preparation and Current Situation of Proton-ICCHIBAN-2 Experiment Authors: Uchihori, Yukio; Yasuda, Nakahiro; Kitamura, H.; Kodaira, S.; Benton, Eric; Hajek, Michael; Berger, Thomas; Jadrnickova, Iva; Ploc, Ondrej Bibcode: 2010cosp...38.3208U Altcode: 2010cosp.meet.3208U The ICCHIBAN (Inter Comparison for Cosmicrays with Heavy Ion Beams at NIRS) working group has organized and performed various ICCHIBAN runs for active and passive radiation detectors at HIMAC, NIRS, Japan, Loma Linda and Brookhaven, USA and CERN, Switzer-land since the start of the ICCHIBAN project in the year 2002. One of the main focus points of this project is to understand the response of the applied detector systems (either active or passive) for personal and area dosimetry in space environment to a simulated sub-set of the space radiation environment, focusing on the heavy ion response. This is of special importance for the further intercomparison of space radiation data gathered by various international in-stitutes and universities for space radiation experiments as MATROSHKA, DOSIS, DOBIES, BRADOS, MATROSHKA-R etc. The ICCHIBAN experiments have created a big database of response data, especially for all the different passive radiation detectors and detector materials (Thermoluminescence (TLD) and Optical Luminescence (OSL)) over the last 7 years, resulting in a better understanding of how and why we still have differences in the measurement results from common space experiments -as the Space ICCHIBAN 2 experiment. One of the reasons why for the differences in the TLD/OSL results is the lack of intercomparison and response data for low LET particles up to around 10 keV/m, especially protons. Due to the fact, that the main contribution to absorbed dose in low earth orbit is due to protons, the ICCHIBAN working group has started the set-up of a Proton ICCHIBAN intercomparison experiment at NIRS. The Proton ICCHIBAN run has been performed at the cyclotron at NIRS, Chiba in February 2010. 15 institutes from 12 countries sent or brought their dosimeters and exposed them to 40 and 70 MeV proton beams with the same doses and exposure conditions. In this paper, the experiment procedures and current situation of the intercomparision experiments will be shown. Title: The DOSIS -Experiment onboard the Columbus Laboratory of the International Space Station -Overview and first mission results Authors: Reitz, Guenther; Berger, Thomas; Kürner, Christine; Burmeister, Sünke; Hajek, Michael; Bilski, Pawel; Horwacik, Tomasz; Vanhavere, Filip; Spurny, Frantisek; Jadrnickova, Iva; Pálfalvi, József K.; O'Sullivan, Denis; Yasuda, Nakahiro; Uchihori, Yukio; Kitamura, Hisashi; Kodaira, Satoshi; Yukihara, Eduardo; Benton, Eric; Zapp, Neal; Gaza, Ramona; Zhou, Dazhuang; Semones, Edward; Roed, Yvonne; Boehme, Matthias; Haumann, Lutz Bibcode: 2010cosp...38.3194R Altcode: 2010cosp.meet.3194R Besides the effects of the microgravity environment, and the psychological and psychosocial problems encountered in confined spaces, radiation is the main health detriment for long dura-tion human space missions. The radiation environment encountered in space differs in nature from that on earth, consisting mostly of high energetic ions from protons up to iron, resulting in radiation levels far exceeding the ones encountered on earth for occupational radiation workers. Accurate knowledge of the physical characteristics of the space radiation field in dependence on the solar activity, the orbital parameters and the different shielding configurations of the International Space Station ISS is therefore needed. The DOSIS (Dose Distribution inside the ISS) experiment, under the project and science lead of DLR, aims for the spatial and tempo-ral measurement of the radiation field parameters inside the European Columbus laboratory onboard the International Space Station. This goal is achieved by applying a combination of passive (Thermo-and Optical luminescence detectors and Nuclear track etch detectors) and active (silicon telescope) radiation detectors. The passive radiation detectors -so called pas-sive detector packages (PDP) are mounted at eleven positions within the Columbus laboratory -aiming for a spatial dose distribution measurement of the absorbed dose, the linear energy transfer spectra and the dose equivalent with an average exposure time of six months. Two active silicon telescopes -so called Dosimetry Telescopes (DOSTEL 1 and DOSTEL 2) together with a Data and Power Unit (DDPU) are mounted within the DOSIS Main Box at a fixed loca-tion beneath the European Physiology Module (EPM) rack. The DOSTEL 1 and DOSTEL 2 detectors are positioned at a 90 angle to each other for a precise measurement of the temporal and spatial variation of the radiation field, especially during crossing of the South Atlantic Anomaly (SAA). The DOSIS hardware was launched with the Space Shuttle Endeavour to the International Space Station on 15 July 2009 and installed by European Astronaut Frank de Winne on 18 July 2009. The first PDP set was downloaded after an exposure time of 124 days in November 2009 and a second PDP set was installed in November 2009. The active part of the instrument suit is working since July 2009. The presentation will give an overview about the DOSIS experiment as well as first results from the passive and active radiation detector measurements. The Austrian activities within this experiment were supported by the Austrian Space Appli-cations Programme (ASAP) of the Federal Ministry for Transport, Innovation and Technology under contract no. 819643. The Polish contribution to this work was supported by the Min-istry of Science and Higher Education, grant No. DWM/N118/ESA/2008. The Hungarian contribution was supported by the ESA PECS grant No. C98066. Title: Simulations of MATROSHKA experiments at ISS using PHITS Authors: Puchalska, Monika; Sihver, L.; Sato, T.; Berger, T.; Reitz, G. Bibcode: 2010cosp...38.3203P Altcode: 2010cosp.meet.3203P Concerns about the biological effects of space radiation are increasing rapidly due to the per-spective of long-duration manned missions, both in relation to the International Space Station (ISS) and to manned interplanetary missions to Moon and Mars in the future. As a prepara-tion for these long duration space missions it is important to ensure an excellent capability to evaluate the impact of space radiation on human health in order to secure the safety of the astronauts/cosmonauts and minimize their risks. It is therefore necessary to measure the radi-ation load on the personnel both inside and outside the space vehicles and certify that organ and tissue equivalent doses can be simulated as accurate as possible. In this paper we will present simulations using the three-dimensional Monte Carlo Particle and Heavy Ion Transport code System (PHITS) of long term dose measurements performed with the ESA supported ex-periment MATROSHKA (MTR), which is an anthropomorphic phantom containing over 6000 radiation detectors, mimicking a human head and torso. The MTR experiment, led by the German Aerospace Center (DLR), was launched in January 2004 and has measured the ab-sorbed dose from space radiation both inside and outside the ISS. In this paper preliminary comparisons of measured and calculated dose and organ doses in the MTR located outside the ISS will be presented. The results confirm previous calculations and measurements which indicate that PHITS is a suitable tool for estimations of dose received from cosmic radiation and when performing shielding design studies of spacecraft. Acknowledgement: The research leading to these results has received funding from the Euro-pean Commission in the frame of the FP7 HAMLET project (Project 218817). Title: Response of the Chromosphere to Penumbral Dynamics: Bow Shocks and Microjets Authors: Ryutova, M.; Berger, T.; Frank, Z.; Title, A. Bibcode: 2009ASPC..415..373R Altcode: We have analyzed the data sets obtained with the SOT instrument on Hinode during the disc passage of AR 10923 (November 10--20, 2006). Along with a limited number of jet-like features (Katsukawa 2007), we found other kinds of bright chromospheric transients abundantly pervading the entire penumbra and drifting as a whole in a direction perpendicular to their long axes. Quantitative analysis based on our recent penumbral model (Ryutova et al. 2008a) shows that they have all the signatures of bow shocks produced in the overlying chromosphere by post-reconnection penumbral filaments. Title: Supergranulation, Network Formation, and TFGs Evolution from Hinode Observations Authors: Roudier, T.; Rincon, F.; Rieutord, M.; Brito, D.; Beigbeder, F.; Parès, L.; Malherbe, J. -M.; Meunier, N.; Berger, T.; Frank, Z. Bibcode: 2009ASPC..415..203R Altcode: In this paper, we analyse a a 48h high-resolution time sequence of the quiet Sun photosphere obtained with the Solar Optical Telescope onboard Hinode. Using floating corks advected by velocity fields inferred from photometry measurements, we show that long-living Trees of Fragmenting Granules play a crucial role in the advection of small-scale magnetic fields and in the build-up of the magnetic network. Title: Hinode/SOT Observations of Quiescent Prominence Dynamics Authors: Berger, T. Bibcode: 2009ASPC..415..109B Altcode: Hinode/SOT observations of quiescent, or ``Quiet Sun,'' prominences (QSPs) have confirmed and extended several dynamic characteristics known from previous ground-based observations: filamentary downflow streams, large-scale vortex flows, long-period body oscillations, and counter-streaming flows have been seen in most QSPs to date. Beyond these known characteristics, we have discovered completely new dynamics in QSPs, primary among which are large-scale (up to 50 Mm diameter) ``bubbles'' that inflate below prominences, as well as dark turbulent plume upflows that intermittently traverse them to heights of 15 Mm or more above the chromospheric spicules. Here we briefly review the prominence dynamics seen in the SOT dataset and provide quantitative measures of some of their characteristics. In general we conclude that there is no such thing as a static prominence---all quiescent prominences are in constant motion, primarily in downflow streams along apparently vertical streamlines. The constant draining motion implies that there is no need for ``suspension against gravity'' of the prominence gas. Fully 3-D dynamic models that take into account non-steady prominence mass transport are required to advance our understanding of these enigmatic objects. Title: ON THE DOWNFLOWS IN HEDGEROW PROMINENCES Authors: Berger, T. E.; Haerendel, G. Bibcode: 2009AGUFMSH44A..07B Altcode: We analyze the downflows in quiescent prominences with respect to width, vertical velocity and acceleration, using sequences of images from the Solar Optical Telescope (SOT) of the Hinode mission. SOT sequences in both 656.3 nm H-alpha and 396.8 nm Ca II H-line bandpasses show that the downflows have typical widths of 300 km, lengths up to 15 Mm, and speeds on the order of 10--20 km/s. Most downflows initiate near the top of the visible-light prominence in the form of bright knots and show an initial acceleration before achieving relatively constant speeds. Downflows typically end either in the chromosphere below the prominence or on large arches that sometimes form lower boundaries to the prominences. In some cases, downflows are strongly deflected by arches indicating a large gradient in the magnetic field at those locations. The vertical coherence of most of the threads over much of the prominence height suggests a continuous stream of plasma. The frozen-field condition implies the presence of vertical magnetic field dragged by the downflow with balanced up and down polarity. This explains the absence of vertical components in magnetic field measurements. The large-scale horizontal field plays an important role in the dynamics of the downflow, in two ways. It compresses the thread plasma and field and presents an obstacle to the downflow. The energy gained by falling in the gravitational field is in part expended in stretching the vertical field, in part in pushing the horizontal field out of the way and in part by covering the radiative losses of the compressed plasma. With total densities of the order of nearly 10^12 cm-3 and horizontal fields of order 10 G, energy and force balance yield vertical velocities of about 10 km/s and temperatures of 7000-8000 K. The threads are nourished by plasma inflow from outside the prominence along largely horizontal fields and sudden onset of gravitational instability. Title: Formation and Dynamics of Multi-thread Arcades of Coronal Loops Authors: Ryutova, M.; Frank, Z.; Berger, T. Bibcode: 2009ASPC..415..291R Altcode: Coronal structures having various forms and dynamics, often bifurcate into a long living, well organized multi-thread loop arcades. To describe this process we use the model of energetically open system, consisting of current carrying magnetic loops that interconnect a high β energy production region with a low β dissipation region through the resistive stresses. The model includes feedback managed by the transition region. Such a system may be driven into various dynamic forms including spontaneous process of self-organization. Title: Observations of Large-Scale Dynamic Bubbles in Prominences Authors: de Toma, G.; Casini, R.; Berger, T. E.; Low, B. C.; de Wijn, A. G.; Burkepile, J. T.; Balasubramaniam, K. S. Bibcode: 2009ASPC..415..163D Altcode: Solar prominences are very dynamic objects, showing continuous motions down to their smallest resolvable spatial and temporal scales. However, as macroscopic magnetic structures, they are remarkably stable during their quiescent phase. We present recent ground-based and Hinode observations of large-scale bubble-like, dynamic sub-structures that form within and rise through quiescent prominences without disrupting them. We investigate the similarities and differences of the Hinode and ground-based observations and discuss their implications for models of prominences. Title: Sunspot Penumbrae: Formation and Fine Structure Authors: Ryutova, M.; Berger, T.; Title, A. Bibcode: 2009ASPC..415..361R Altcode: Sub-arcsecond observations revealing the fine sub-structure of penumbral filaments and new properties of their dynamics, provide both the basis and constraints for novel models of the penumbra. Even more severe conditions are imposed on models by new data obtained with the SOT instrument on Hinode, showing e.g. direct connection between the dynamic changes in penumbra and appearance of bright transients in the overlying chromosphere. We propose the mechanism that not only explains the observed properties of individual filaments, but is part of the physical process that determines formation of penumbra and its impact on the overlying atmosphere. Title: An Intriguing Chromospheric Jet Observed by Hinode: Fine Structure Kinematics and Evidence of Unwinding Twists Authors: Liu, Wei; Berger, Thomas E.; Title, Alan M.; Tarbell, Theodore D. Bibcode: 2009ApJ...707L..37L Altcode: 2009arXiv0910.5186L We report a chromospheric jet lasting for more than 1 hr observed by the Hinode Solar Optical Telescope in unprecedented detail. The ejection occurred in three episodes separated by 12-14 minutes, with the amount and velocity of material decreasing with time. The upward velocities range from 438 to 33 km\nolimits s\nolimits ^{-1}, while the downward velocities of the material falling back have smaller values (mean: -56 km\nolimits s\nolimits ^{-1}) and a narrower distribution (standard deviation: 14 km\nolimits s\nolimits ^{-1}). The average acceleration inferred from parabolic spacetime tracks is 141 m\nolimits s^{-2}, a fraction of the solar gravitational acceleration. The jet consists of fine threads (0farcs5-2'' wide), which exhibit coherent, oscillatory transverse motions perpendicular to the jet axis and about a common equilibrium position. These motions propagate upward along the jet, with the maximum phase speed of 744 ± 11 km\nolimits s\nolimits ^{-1} at the leading front of the jet. The transverse oscillation velocities range from 151 to 26 km\nolimits s\nolimits ^{-1}, amplitudes from 6.0 to 1.9 Mm\nolimits, and periods from 250 to 536 s\nolimits. The oscillations slow down with time and cease when the material starts to fall back. The falling material travels along almost straight lines in the original direction of ascent, showing no transverse motions. These observations are consistent with the scenario that the jet involves untwisting helical threads, which rotate about the axis of a single large cylinder and shed magnetic helicity into the upper atmosphere. Title: Service-Mode Observations for Ground-Based Solar Physics Authors: Reardon, K. P.; Rimmele, T.; Tritschler, A.; Cauzzi, G.; Wöger, F.; Uitenbroek, H.; Tsuneta, S.; Berger, T. Bibcode: 2009ASPC..415..332R Altcode: 2009arXiv0909.1522R There are significant advantages in combining Hinode observations with ground-based instruments that can observe additional spectral diagnostics at higher data rates and with greater flexibility. However, ground-based observations, because of the random effects of weather and seeing as well as the complexities data analysis due to changing instrumental configurations, have traditionally been less efficient than satellite observations in producing useful datasets. Future large ground-based telescopes will need to find new ways to optimize both their operational efficiency and scientific output.

We have begun experimenting with service-mode or queue-mode observations at the Dunn Solar Telescope using the Interferometric Bidimensional Spectrometer (IBIS) as part of joint Hinode campaigns. We describe our experiences and the advantag es of such an observing mode for solar physics. Title: Helical Shape and Twisting Motion as Intrinsic Properties of Penumbral Filaments Authors: Shine, R. A.; Ryutova, M.; Berger, T. E.; Title, A. M.; Tarbell, T. D.; Ichimoto, K. Bibcode: 2009AGUFMSH23B1541S Altcode: A wealth of high resolution data obtained with advanced ground based telescopes and the SOT instrument on HINODE have led to new findings in the properties of penumbral filaments and controversies in their interpretation. Here we address one such issue, namely the question of whether the apparent twist of filaments is real or is just a viewing effect. We show that the helical shape and twisting motions of penumbral filaments follow from first principles and represent an integral part of penumbra formation and dynamics. As such, these properties link together other observed features of filaments including their magnetic and thermal substructure and their impact on the overlying atmosphere. At all stages of penumbral dynamics, qualitative agreement of theory and observations is supported by quantitative analysis as well. Title: High Resolution Observations of Solar Quiescent Prominences with the Hinode Solar Optical Telescope: an Open Challenge to 21st Century Ground-based Solar Telescopes (Invited) Authors: Berger, T. E. Bibcode: 2009AGUFMSH53B..06B Altcode: The Solar Optical Telescope (SOT) on the Japanese Hinode satellite is a 0.5-meter diameter Gregorian solar telescope in a 600 km Sun-synchronous orbit. The telescope achieves diffraction-limited imaging with no atmospheric seeing in a wavelength range from 380 nm to 660 nm. Using both the Broadband Filter Imager (BFI) Ca II H-line channel at 389.6 nm and the tunable Narrowband Filter Imager (NFI) H-alpha channel at 656.3 nm we have observed many quiescent solar prominences since the satellite launch in September 2006. The excellent optical quality and low scattering of the SOT telescope combined with the lack of atmospheric scattering and seeing enables us to capture multi-hour diffraction-limited movies of quiescent prominences above the limb that achieve 200 km spatial resolution and 15--30 second temporal resolution. These SOT observations have led to the discovery of new flows in the solar outer atmosphere in the form of buoyant small-scale (2--6 Mm) plumes and large-scale (10--50 Mm) "bubbles" or arches that originate below quiescent prominences and rise with speeds of 10--30 km/sec to heights of 10--30+ Mm above the solar limb. In this talk we review the kinematic properties of these new flows in combination with the long-observed filamentary downflows to show that quisecent prominences are not magnetostatic structures "suspended against gravity" but are rather entirely dynamic structures in which mass is continually drained in the downflows while being resupplied largely by condensation from the coronal cavity above and episodic buoyant flows from below. The Hinode/SOT instrument has definitively shown the value of flying high-resolution visible-light solar telescopes in space by acheiving in its first six months what had been a long-standing goal of ground-based solar prominence research for the past 50 years. However many key quiescent prominence characteristics cannot be measured by the limited instrumentation on the Hinode satellite. Primary among these is vector magnetic field in prominences at high spatial and temporal resolution and the thermodynamic and magnetic characteristics of the new plume and bubble flows. It is hoped that the new generation of adaptive-optics ground-based telescopes such as the 1.6-m NST can make progress in these areas while we await the next solar space telescope missions. Title: Role of the Resistive and Thermal Instabilities in Dynamics of Quiescent Prominences Authors: Frank, Z.; Ryutova, M.; Berger, T. E.; Title, A. M.; Tarbell, T. D. Bibcode: 2009AGUFMSH41B1653F Altcode: We present the observations taken with the SOT instrument on Hinode in G-band and Ca H lines. High cadence data compiled in movies show clear evidence for several fundamental plasma instabilities. We combine the observational evidence and theoretical estimates to identify these instabilities. The following can be given as examples. (1) An analogue of the Kelvin-Helmholtz instability develops at the prominence/corona interface that manifests itself in growing ripples during a linear growth phase and may be followed by a nonlinear stage taking the form of an explosive instability corresponding to a CME ejection. This instability also includes the regime of "smoke ring" formation. (2) The appearence of "bubbles and spikes" typical to the Rayleigh-Taylor instability are observed. Their evolution and growth rates are found to be modified by both poloidal and toroidal components of magnetic field. (3) A resistive interchange instability, associated with an "unfavorable" magnetic field curvature relative to the density/temperature gradients, may be responsible for a hot barb formation, its evolution and collapse. Title: Fine Structures and Kinematics of an Intriguing Chromospheric Jet Observed by Hinode Solar Optical Telescope Authors: Liu, W.; Berger, T. E.; Title, A. M.; Tarbell, T. D. Bibcode: 2009AGUFMSH51A1266L Altcode: Transient, small-scale ejections of plasma from the lower atmosphere are common manifestations of solar activity. Hinode, with its superior resolutions, has spurred renewed interest in solar jets since its launch. Here we report a chromospheric jet lasting for more than 1 hr on 2007 February 9 observed by the Hinode Solar Optical Telescope (SOT) in unprecedented detail. SOT Ca II H passband observations at high resolution of 0.2 arcsecond and cadence of 8 s allowed us to investigate the fine structures and kinematics of the jet. The ejection occurred in three episodes, rather than continuously, with the amount and velocity of material decreasing with time. The upward velocities along the jet range from ~440 to ~30 km/s, while the downward velocities of the material falling back have much smaller values (mean: -60 km/s) and a narrower distribution. Some tracks in the space-time plot clearly show parabolic shapes and the inferred acceleration is a fraction of the solar gravitational acceleration. The jet consists of fine threads (0.5-2 arcsecond wide), which exhibit coherent, oscillatory transverse motions perpendicular to the jet axis and about a common equilibrium position. These motions propagate upward, with the maximum phase speed of ~740 km/s found at the leading front of the jet. The transverse oscillation velocities range from 150 to 30 km/s, amplitudes from 6 to 2 Mm, and periods from 250 to 550 s. The oscillations slow down with time and cease when the material starts to fall back. The falling material travels along almost straight lines in the original direction of ascent, showing no transverse motions. These observations are consistent with the models suggested by Shibata & Uchida (1985) and Canfield et al. (1996). In this scenario, the jet involves untwisting helical threads, which rotate about the axis of a single large cylinder and shed magnetic helicity into the upper atmosphere. Implications of this event in the context of multiwavelength data in H-alpha, EUV, and X-rays will be discussed. A chromospheric jet observed by Hinode SOT in the Ca II H passband (T=1-2×10 4 K). Note the helical-like fine threads. Title: Origin of Filamentary Structures and Flows in Quiescent Prominences Authors: Ryutova, M.; Berger, T. E.; Tarbell, T. D.; Frank, Z.; Title, A. M. Bibcode: 2009AGUFMSH23B1540R Altcode: The paradox of fine vertical structure has usually referred to an apparent contradiction met when comparing vertical fine structures of quiescent prominences observed on the limb with the necessary horizontal magnetic field along their long axis. In addition to this fundamental problem, the very formation of fine vertical structures has been a long standing puzzle. Here we address these problems and show that considering the global structure of a prominence as a large scale skewed formation with toroidal and poloidal fields removes the paradox and allows derivation of dynamic stability criteria. This also includes the mechanism of the fine structure formation and peculiarities of downward mass motions. Theoretical estimates of key parameters are compared with the observations taken with the SOT instrument on Hinode. We find results of comparison very encouraging. For the approximate 3D reconstruction of the general shape of prominences, the STEREO A and B images have been used. Title: The Experiment LIFE-SPORES under Development for the Phobos-Grunt Mission Authors: Rettberg, P.; Rabbow, E.; Moller, R.; Wamann, M.; Berger, T.; Horneck, G.; Reitz, G.; Sychev, V.; Betts, B.; Warmflash, D. Bibcode: 2009OLEB...39...83R Altcode: The Russian space agency will launch a sample return mission nicknamed Phobos-Grunt to the Martian moon Phobos. According to plans, the spacecraft will land on Phobos, collect soil and rock samples from its surface, and then return back to Earth. The spacecraft will release a capsule containing all the samples gathered on Phobos, to land on Earth. Attached to the capsule for the entire 34 months of the journey will be a small cylinder containing a collection of terrestrial microorganisms. In its flight, the cylinder will be, in effect, a simulated space rock, subject to the same extreme conditions as a Martian meteorite traveling to Earth. It is the Living Interplanetary Flight Experiment (LIFE) experiment of The Planetary Society (http://www.planetary.org/programs/projects/life/). The panspermia theory hypothesises that living organisms could be transported through the solar system and then take hold on other planets. In one component of the LIFE experiment called LIFE-SPORES, the ability of spores from the bacterium Bacillus subtilis to survive an interplanetary travel from Earth to Mars moon Phobos and back will be tested. In addition to the well-characterized and already sequenced wildtype strain Bacillus subtilis 168 a newly developed strain, MW01, whose cells are about 3 to 4 times more UV and ionising radiation resistant than 168, will be used as test object. For dosimetry of ionsing radiation during the mission TLDs (thermoluminescence detectors) will be used and analyzed post-flight. Both bacterial strains are now part of an ongoing experiment on the ISS, ADAPT, on EXPOSE-E mounted on the Eutef platform of Columbus which will be exposed to the space conditions in LEO for about 18 months. Title: Temporal and spatial evolution of the solar energetic particle event on 20 January 2005 and resulting radiation doses in aviation Authors: Matthiä, D.; Heber, B.; Reitz, G.; Meier, M.; Sihver, L.; Berger, T.; Herbst, K. Bibcode: 2009JGRA..114.8104M Altcode: 2009JGRA..11408104M The solar energetic particle event on 20 January 2005 was one of the largest ground level events ever observed. Neutron monitor stations in the Antarctic recorded count rate increases of several thousand percent caused by secondary energetic particles, and it took more than 36 h to return to background level. Such huge increases in high energetic solar cosmic radiation on the ground are obviously accompanied by considerable changes in the radiation environment at aviation altitudes. Measurements of 28 neutron monitor stations were used in this work to numerically approximate the primary solar proton spectra during the first 12 h of the event by minimizing the differences between measurements and the results of Monte-Carlo calculated count rate increases. The primary spectrum of solar energetic protons was approximated by a power law in rigidity and a linear angular distribution. The incoming direction of the solar energetic particles was determined and compared to the interplanetary magnetic field direction during the event. The effects on the radiation exposure at altitudes of about 12 km during that time were estimated to range from none at low latitudes up to almost 2 mSv/h for a very short time in the Antarctic region and about 0.1 mSv/h at high latitudes on the Northern Hemisphere. After 12 h, dose rates were still increased by 50% at latitudes above 60° whereas no increases at all occurred at latitudes below 40° during the whole event. Title: A New View of Fine Scale Dynamics and Magnetism of Sunspots Revealed by Hinode/SOT Authors: Ichimoto, K.; Suematsu, Y.; Katsukawa, Y.; Tsuneta, S.; Shimojo, M.; Shimizu, T.; Shine, R. A.; Tarbell, T. D.; Berger, T.; Title, A. M.; Lites, B. W.; Kubo, M.; Yokoyama, T.; Nagata, S. Bibcode: 2009ASPC..405..167I Altcode: The Solar Optical Telescope on-board Hinode is providing a new view of the fine scale dynamics in sunspots with its high spatial resolution and unprecedented image stability. We present three features related to the Evershed flow each of which raises a new puzzle in sunspot dynamics; i.e., twisting appearance of penumbral filaments, the source and sink of individual Evershed flow channels, and the net circular polarization in penumbrae with its spatial relation to the Evershed flow channels. Title: Has Hinode Revealed the Missing Turbulent Flux of the Quiet Sun? Authors: Lites, B. W.; Kubo, M.; Socas-Navarro, H.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A. M.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2009ASPC..405..173L Altcode: The Hinode Spectro-Polarimeter has revealed the presence of surprisingly strong horizontal magnetic fields nearly everywhere in the quiet solar atmosphere. These horizontal fields, along with measures of the vertical fields, may be the signature of the ``hidden turbulent flux'' of the quiet Sun. The measured horizontal fields average at least to 55 Gauss: nearly 5 times that of the measured longitudinal apparent flux density. The nature of these fields are reviewed, and discussed in the light of recent magneto-convection numerical simulations of the quiet Sun. Title: First Results from a Novel Magnetograph (SHAZAM) Authors: DeForest, Craig; Rimmele, T.; Berger, T.; Peterson, J. Bibcode: 2009SPD....40.3301D Altcode: The magnetic energy flux through the Sun's surface is dominated by small features at all currently observable spatial scales; hence there is a strong need to improve the spatial resolution of magnetic measurements, which are increasingly photon starved as telescopes improve. The Solar High-speed Zeeman Magnetograph (SHAZAM) is a line-of-sight magnetograph based on the principle of spectral stereoscopy. It is designed to acquire magnetograms quickly enough to beat image fluctuations due to both solar evolution and terrestrial seeing, even on scales under 100 km on the Sun. It is over 100x more photon efficient than existing quantitative magnetographs such as SOHO/MDI. We present first results from an observing run at the National Solar Observatory's Dunn Solar Telescope in May 2009, hopefully including near-diffraction-limited, time resolved magnetogram sequences with better than 150km resolution on the surface of the Sun. Title: Prominence Bubbles and Plumes: Thermo-magnetic Buoyancy in Coronal Cavity Systems Authors: Berger, Thomas; Hurlburt, N. Bibcode: 2009SPD....40.1007B Altcode: The Hinode/Solar Optical Telescope continues to produce high spatial and temporal resolution images of solar prominences in both the Ca II 396.8 nm H-line and the H-alpha 656.3 nm line. Time series of these images show that many quiescent prominences produce large scale (50 Mm) dark "bubbles" that "inflate" into, and sometimes burst through, the prominence material. In addition, small-scale (2--5 Mm) dark plumes are seen rising into many quiescent prominences. We show typical examples of both phenomena and argue that they originate from the same mechanism: concentrated and heated magnetic flux that rises due to thermal and magnetic buoyancy to equilibrium heights in the prominence/coronal-cavity system. More generally, these bubbles and upflows offer a source of both magnetic flux and mass to the overlying coronal cavity, supporting B.C. Low's theory of CME initiation via steadily increasing magnetic buoyancy breaking through the overlying helmut streamer tension forces. Quiescent prominences are thus seen as the lowermost parts of the larger coronal cavity system, revealing through thermal effects both the cooled downflowing "drainage" from the cavity and the heated upflowing magnetic "plasmoids" supplying the cavity. We compare SOT movies to new 3D compressible MHD simulations that reproduce the dark turbulent plume dynamics to establish the magnetic and thermal character of these buoyancy-driven flows into the corona. Title: Prominence Formation Associated with an Emerging Helical Flux Rope Authors: Okamoto, Takenori J.; Tsuneta, Saku; Lites, Bruce W.; Kubo, Masahito; Yokoyama, Takaaki; Berger, Thomas E.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Nagata, Shin'ichi; Shibata, Kazunari; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M. Bibcode: 2009ApJ...697..913O Altcode: 2009arXiv0904.0007O The formation and evolution process and magnetic configuration of solar prominences remain unclear. In order to study the formation process of prominences, we examine continuous observations of a prominence in NOAA AR 10953 with the Solar Optical Telescope on the Hinode satellite. As reported in our previous Letter, we find a signature suggesting that a helical flux rope emerges from below the photosphere under a pre-existing prominence. Here we investigate more detailed properties and photospheric indications of the emerging helical flux rope, and discuss their relationship to the formation of the prominence. Our main conclusions are: (1) a dark region with absence of strong vertical magnetic fields broadens and then narrows in Ca II H-line filtergrams. This phenomenon is consistent with the emergence of the helical flux rope as photospheric counterparts. The size of the flux rope is roughly 30,000 km long and 10,000 km wide. The width is larger than that of the prominence. (2) No shear motion or converging flows are detected, but we find diverging flows such as mesogranules along the polarity inversion line. The presence of mesogranules may be related to the emergence of the helical flux rope. (3) The emerging helical flux rope reconnects with magnetic fields of the pre-existing prominence to stabilize the prominence for the next several days. We thus conjecture that prominence coronal magnetic fields emerge in the form of helical flux ropes that contribute to the formation and maintenance of the prominence. Title: Simulations Of Buoyant Plumes In Solar Prominences Authors: Hurlburt, Neal E.; Berger, T. Bibcode: 2009SPD....40.1009H Altcode: Recent observations of solar prominences have revealed a complex, dynamic flow field within them. The flow field within quiescent prominences is characterized by long ``threads'' and dark ``bubbles'' that fall and rise (respectively) in a thin sheet. The flow field in active prominences display more helical motions that travel along the axis of the prominence. We explore the possible dynamics of both of these with the aid of 2.5D MHD simulations. Our model, compressible plasma possesses density and temperature gradients and resides in magnetic field configurations that mimc those of a solar prominence. The system is the subjected to to localized heating to trigger a variety of modes and instabilities. Title: Mesoscale dynamics on the Sun's surface from HINODE observations Authors: Roudier, Th.; Rieutord, M.; Brito, D.; Rincon, F.; Malherbe, J. M.; Meunier, N.; Berger, T.; Frank, Z. Bibcode: 2009A&A...495..945R Altcode: 2009arXiv0902.2299R Context:
Aims: The interactions of velocity scales on the Sun's surface, from granulation to supergranulation are still not understood, nor are their interaction with magnetic fields. We thus aim at giving a better description of dynamics in the mesoscale range which lies between the two scales mentioned above.
Methods: We analyse a 48 h high-resolution time sequence of the quiet Sun photosphere at the disk center obtained with the Solar Optical Telescope onboard Hinode. The observations, which have a field of view of 100´´ × 100´´, typically contain four supergranules. We monitor in detail the motion and evolution of granules as well as those of the radial magnetic field.
Results: This analysis allows us to better characterize Trees of Fragmenting Granules issued from repeated fragmentation of granules, especially their lifetime statistics. Using floating corks advected by measured velocity fields, we show their crucial role in the advection of the magnetic field and in the build up of the network. Finally, thanks to the long duration of the time series, we estimate that the turbulent diffusion coefficient induced by horizontal motion is approximately 430 km2 s-1.
Conclusions: These results demonstrate that the long living families contribute to the formation of the magnetic network and suggest that supergranulation could be an emergent length scale building up as small magnetic elements are advected and concentrated by TFG flows. Our estimate for the magnetic diffusion associated with this horizontal motion might provide a useful input for mean-field dynamo models. Title: The Solar Chromosphere: Old Challenges, New Frontiers Authors: Ayres, T.; Uitenbroek, H.; Cauzzi, G.; Reardon, K.; Berger, T.; Schrijver, C.; de Pontieu, B.; Judge, P.; McIntosh, S.; White, S.; Solanki, S. Bibcode: 2009astro2010S...9A Altcode: No abstract at ADS Title: On the Penumbral Jetlike Features and Chromospheric Bow Shocks Authors: Ryutova, M.; Berger, T.; Frank, Z.; Title, A. Bibcode: 2008ApJ...686.1404R Altcode: We present observations of sunspot penumbrae obtained during the disk passage of AR 10923 (2006 November 10-20) with the SOT instrument on Hinode in 4305 Å G band and Ca II λ3968 H line. Along with recently discovered jetlike features (Katsukawa et al. 2007), we find other kinds of bright elongated transients abundantly pervading the entire penumbra and drifting as a whole in a direction almost perpendicular to their long axes. Their measured velocities strongly depend on their orientation with respect to the line of sight and range from simeq1 to simeq20 km s-1. We present quantitative analysis of these features and interpret them relative to our recent penumbral model (Ryutova et al. 2008) to show that they are produced by shocks resulting from a slingshot effect associated with the ongoing reconnection processes in neighboring penumbral filaments. Due to sharp stratification of the low atmosphere, postreconnection flux tubes moving upward quickly accelerate. At transonic velocities a bow (detached) shock is formed in front of the flux tube, as usually occurs in cases of blunt bodies moving with supersonic velocities. Observed parameters of transients are in good agreement with calculated parameters of bow shocks. On some, much more rare occasions compared to "drifting" bow-shock-type transients, there appear compact bright transients moving in the radial direction, along their long axis, and having velocities of 20-50 km s-1. We relate these features to a category of true microjets. Title: Hinode, TRACE, SOHO, and Ground-based Observations of a Quiescent Prominence Authors: Heinzel, P.; Schmieder, B.; Fárník, F.; Schwartz, P.; Labrosse, N.; Kotrč, P.; Anzer, U.; Molodij, G.; Berlicki, A.; DeLuca, E. E.; Golub, L.; Watanabe, T.; Berger, T. Bibcode: 2008ApJ...686.1383H Altcode: A quiescent prominence was observed by several instruments on 2007 April 25. The temporal evolution was recorded in Hα by the Hinode SOT, in X-rays by the Hinode XRT, and in the 195 Å channel by TRACE. Moreover, ground-based observatories (GBOs) provided calibrated Hα intensities. Simultaneous extreme-UV (EUV) data were also taken by the Hinode EIS and SOHO SUMER and CDS instruments. Here we have selected the SOT Hα image taken at 13:19 UT, which nicely shows the prominence fine structure. We compare this image with cotemporaneous ones taken by the XRT and TRACE and show the intensity variations along several cuts parallel to the solar limb. EIS spectra were obtained about half an hour later. Dark prominence structure clearly seen in the TRACE and EIS 195 Å images is due to the prominence absorption in H I, He I, and He II resonance continua plus the coronal emissivity blocking due to the prominence void (cavity). The void clearly visible in the XRT images is entirely due to X-ray emissivity blocking. We use TRACE, EIS, and XRT data to estimate the amount of absorption and blocking. The Hα integrated intensities independently provide us with an estimate of the Hα opacity, which is related to the opacity of resonance continua as follows from the non-LTE radiative-transfer modeling. However, spatial averaging of the Hα and EUV data have quite different natures, which must be taken into account when evaluating the true opacities. We demonstrate this important effect here for the first time. Finally, based on this multiwavelength analysis, we discuss the determination of the column densities and the ionization degree of hydrogen in the prominence. Title: Magnetic Fields of the Quiet Sun: A New Quantitative Perspective From Hinode Authors: Lites, B. W.; Kubo, M.; Socas-Navarro, H.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2008ASPC..397...17L Altcode: This article summarizes results of studies presented in two papers already published: Lites et al. (2007a); Lites et al. (2007b). Please see these for further details. Title: On-orbit Performance of the Solar Optical Telescope aboard Hinode Authors: Ichimoto, K.; Katsukawa, Y.; Tarbell, T.; Shine, R. A.; Hoffmann, C.; Berger, T.; Cruz, T.; Suematsu, Y.; Tsuneta, S.; Shimizu, T.; Lites, B. W. Bibcode: 2008ASPC..397....5I Altcode: 2008arXiv0804.3248I On-orbit performance of the Solar Optical Telescope (SOT) aboard Hinode is described with some attention to its unpredicted aspects. In general, SOT reveals an excellent performance and has been providing outstanding data. Some unexpected features exist, however, in behaviours of the focus position, throughput and structural stability. Most of them are recovered by the daily operation i.e., frequent focus adjustment, careful heater setting and corrections in data analysis. The tunable filter contains air bubbles which degrade the data quality significantly. Schemes for tuning the filter without disturbing the bubbles have been developed and tested, and some useful procedures to obtain Dopplergrams and magnetograms are now available. October and March, when the orbit of satellite becomes nearly perpendicular to the direction towards the Sun, provide a favourable condition for continuous runs of the narrow-band filter imager. Title: Hinode Observations of Magnetic Elements in Internetwork Areas Authors: de Wijn, A. G.; Lites, B. W.; Berger, T. E.; Frank, Z. A.; Tarbell, T. D.; Ishikawa, R. Bibcode: 2008ApJ...684.1469D Altcode: 2008arXiv0806.0345D We use sequences of images and magnetograms from Hinode to study magnetic elements in internetwork parts of the quiet solar photosphere. Visual inspection shows the existence of many long-lived (several hours) structures that interact frequently and may migrate over distances of ~7 Mm over a period of a few hours. About a fifth of the elements have an associated bright point in G-band or Ca II H intensity. We apply a hysteresis-based algorithm to identify elements. The algorithm is able to track elements for about 10 minutes on average. Elements intermittently drop below the detection limit, although the associated flux apparently persists and often reappears some time later. We infer proper motions of elements from their successive positions and find that they obey a Gaussian distribution with an rms of 1.57 +/- 0.08 km s-1. The apparent flows indicate a bias of about 0.2 km s-1 toward the network boundary. Elements of negative polarity show a higher bias than elements of positive polarity, perhaps as a result of the dominant positive polarity of the network in the field of view or because of increased mobility due to their smaller size. A preference for motions in X is likely explained by higher supergranular flow in that direction. We search for emerging bipoles by grouping elements of opposite polarity that appear close together in space and time. We find no evidence supporting Joy's law at arcsecond scales. Title: The Small-Scale Field Measured With Hinode/SOT and Feature Tracking: Where is the mixed- polarity flux? Authors: Deforest, C. E.; Lamb, D. A.; Berger, T.; Hagenaar, H.; Parnell, C.; Welsch, B. Bibcode: 2008AGUSMSP51D..01D Altcode: We report on the results of the first feature tracking study of the solar magnetic field with Hinode/SOT. We processed a SOT Na-D line-of-sight magnetogram sequence with five different magnetic tracking codes. The SOT data allow us to probe the evolving magnetic field on the granular scale for hours at a time, something that was not possible with either ground-based observations (which are limited to short periods of good seeing) or prior space-based observations (which are limited to arcsecond spatial scales). We find that the field is much less mixed than previously supposed: while Hinode resolves small-scale structure within features that, to SOHO/MDI, would appear as monolithic flux concentrations, this substructure has but a single sign. Furthermore, the average distance between identifiable flux concentrations of opposite sign remains nearly unchanged at the higher resolution, a result that is quite surprising in light of the common picture of a sea of strong mixed-polarity flux concentrations dotting the inter-granular lanes. We discuss possible mechanisms for this surprising result, and implications for the small-scale dynamo. Title: Emergence of a helical flux rope and prominence formation Authors: Okamoto, T. J.; Tsuneta, S.; Lites, B. W.; Kubo, M.; Yokoyama, T.; Berger, T. E.; Ichimoto, K.; Katsukawa, Y.; Nagata, S.; Shibata, K.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M. Bibcode: 2008AGUSMSP43B..06O Altcode: We report a discovery about emergence of a helical flux rope. The episode may be related to the formation and evolution of an active region prominence. Statistical studies by previous authors indicate that numerous prominences have the inverse-polarity configuration suggesting the helical magnetic configurations. There are two theoretical models about formation of such a coronal helical magnetic field in association with prominences: flux rope model and sheared-arcade model. We have so far no clear observational evidence to support either model. In order to find a clue about the formation of the prominence, we had continuous observations of NOAA AR 10953 with the SOT during 2007 April 28 to May 9. A prominence was located over the polarity inversion line in the south-east of the main sunspot. These observations provided us with a time series of vector magnetic fields on the photosphere under the prominence. We found four new features: (1) The abutting opposite-polarity regions on the two sides along the polarity inversion line first grew laterally in size and then narrowed. (2) These abutting regions contained vertically-weak, but horizontally-strong magnetic fields. (3) The orientations of the horizontal magnetic fields along the polarity inversion line on the photosphere gradually changed with time from a normal- polarity configuration to an inverse-polarity one. (4) The horizontal-magnetic field region was blueshifted. These indicate that helical flux rope emerges from below the photosphere into the corona along the polarity inversion line under the prominence. We suggest that this supply of a helical magnetic flux possibly into the corona is related to formation and maintenance of active-region prominences. Title: Photospheric Signature of Penumbral Microjets Authors: Katsukawa, Y.; Jurcak, J.; Ichimoto, K.; Suemtasu, Y.; Tsuneta, S.; Shimizu, T.; Berger, T. E.; Shine, R. A.; Tarbell, T. D.; Lites, B. W. Bibcode: 2008AGUSMSP53A..03K Altcode: HINODE Solar Optical Telescope (SOT) discovered ubiquitous occurrence of fine-scale jetlike activities in penumbral chromospheres, which are referred to as penumbral microjets. The microjets' small width of 400 km and short duration of less than 1 min make them difficult to identify in existing ground-based observations. The apparent rise velocity is faster than 50km/s and is roughly comparable to the Alfven speed in the sunspot chromosphere. These properties of penumbral microjets suggest that magnetic reconnection in uncombed magnetic field configuration is the most possible cause of penumbral microjets. In order to understand magnetic configuration associated with penumbral microjets and prove the chromospheric magnetic reconnection hypothesis, we investigated relationship between penumbral microjets seen in CaIIH images and photospheric magnetic fields measured by the HINODE spectro-polarimeter. We found the inclination angles of penumbral microjets measured in CaII H images are roughly consistent with inclination angles of relatively vertical magnetic field component in uncombed magnetic field configuration. In addition, strong and transient downflows are observed in the photosphere near the boundary of a horizontal flux tube associated with a penumbral microjet. The size of the downflow region is about 300km, which is close to the width of penumbral microjets seen in CaII H images. The downflow velocity of several km/s might be a result of an outflow of chromospheric magnetic reconnection and suffer deceleration due to the higher density in the photosphere. Title: Evershed Flows as an Integral Part of Penumbral Formation and its Fine Structure Authors: Ryutova, M.; Berger, T.; Lites, B.; Title, A.; Frank, Z. Bibcode: 2008AGUSMSP41B..07R Altcode: Observations of Evershed flows with the Solar Optical Telescope (SOT) on Hinode (Ichimito, Shine, Lites, et al. 2008, PASJ, 59, S593) showed that penumbral flows have small scale structures and much more complex properties than those of a simple outflow of material with unique direction and appearence. We address this problem and show that the flow properties are directly connected to the observed properties of penumbral filaments and are an integral part of penumbral development during sunspot formation. In our recent model (Ryutova, Berger, & Title, 2008, ApJ, 676, April), based on the observations that sunspot has a filamentary structure and consists of a dense conglomerate of non-collinear interlaced flux tubes, the penumbra is formed due to an on-going reconnection processes that leads to branching out of the peripheral flux tubes from the "trunk". As flux tubes have different parameters, branching occurs at different heights and with different inclinations, thus forming an "uncombed" penumbra. Each elemental act of reconnection generates an inevitable twist in the post-reconnection filaments that acquire a screw pinch configuration. This explains the remarkable dynamic stability of penumbral filaments and their observed properties, such as presence of dark cores, wrapping and spinning of filaments around each other, bright footpoints, etc. Here we show that propagation of twist along current carrying helical flux tubes is accompanied by plasma flows that may have diverse properties depending on the location of interacting flux tubes, their inclination and pitch. We apply the model to observations taken with the SOT instrument, which includes spectro-polarimetric data, and perform quantitative analysis. Title: Quiescent Prominence Structure and Dynamics: a new View From the Hinode/SOT Authors: Berger, T.; Okamoto, J.; Slater, G.; Magara, T.; Tarbell, T.; Tsuneta, S.; Hurlburt, N. Bibcode: 2008AGUSMSP53A..01B Altcode: To date the Hinode/Solar Optical Telescope (SOT) has produced over a dozen sub-arcsecond, multi-hour movies of quiescent solar prominences in both the Ca II 396.8~nm H-line and the H-alpha 656.3~nm line. These datasets have revealed new details of the structure and dynamics of quiescent prominences including a new form of mass transport in the form of buoyant plume upflows from the chromosphere. We review the SOT prominence datasets to show that quiescent prominences appear in two major morphological categories: "vertically" and "horizontally" structured. The vertically structured prominences all show ubiquitous downflows in 400--700~km wide "streams" with velocities of approximately 10~km~s-1. Most of the vertically structured prominences also show episodic upflows in the form of dark turbulent plumes with typical velocities of 20~km~s-1. Large-scale oscillations are frequently seen in vertical prominences with periods on the order of 10 min and upward propagation speeds of approximately 10~km~s-1. In addition, "bubble" events in which large voids 10--30~Mm across inflate and then burst are seen in some of the vertical prominences. In contrast, the horizontally structured quiescent prominences exhibit only limited flows along the horizontal filaments. We speculate on the origin of the distinction between the vertically and horizontally structured prominences, taking into account viewing angle and the underlying photospheric magnetic flux density. We also discuss the nature of the mysterious dark plumes and bubble expansions and their implications for prominence mass balance in light of recent models of prominence magnetic structure that find vertical flows along some field lines. Title: Magnetic Fields in the Photosphere: Professor Parker's Contributions to our Understanding of Surface Activity on the Sun Authors: Berger, T. Bibcode: 2008AGUSMSP33A..02B Altcode: Magnetic fields in the photosphere of the Sun span sizes from large sunspot active regions on the order of 50 Mm down to the smallest observable magnetic elements 100 km or less in diameter. The generation of these fields in the convection zone and their subsequent interactions with photospheric flowfields are responsible for the majority of observed solar variability over a large range of time and wavelength scales. Professor Parker's research has encompassed this range and shed light on the origins of large scale active regions, the structure and dynamics of sunspots, and the implications of the highly dynamic interactions of magnetic elements with the convective flowfield. We review the contributions of Prof. Parker to these topics in the light of recent observations from both ground-based and space-based telescopes and point out issues of continuing controversy that require further theoretical and observational exploration. Title: On the Fine Structure and Formation of Sunspot Penumbrae Authors: Ryutova, M.; Berger, T.; Title, A. Bibcode: 2008ApJ...676.1356R Altcode: Recent high-resolution observations with the 1 m Swedish Solar Telescope (SST) on La Palma reveal the fine substructure of penumbral filaments and new properties of their dynamics. These findings provide both the basis and constraints for novel models of the penumbra. We present new observations of a large isolated sunspot near Sun center obtained with the SST in 2006. Our data, taken simultaneously in the 4305 Å G-band and 4364 Å continuum bandpasses and compiled in high-cadence movies, confirm the previous results and reveal new features of penumbral filament dynamics. We find that individual filaments are cylindrical helices with the apparent properties of vortex tubes exhibiting flow patterns similar to kinked flux tubes. Measured pitch/radius ratios of helical filaments indicate their dynamic stability. We propose a mechanism that explains the fine structure of penumbral filaments, their observed dynamics, and their formation process in association with sunspot properties. The mechanism assumes that the umbra itself is a dense conglomerate of twisted, interlaced flux tubes with peripheral filaments branching out from the "trunk" at different heights due to ongoing reconnection processes and arcing downward to the photosphere. The twist of individual filaments, and the resulting distribution of magnetic fields and temperature, is due to the onset of the well-known screw pinch instability, the parameters of which can be measured from our data. Title: Formation of Solar Magnetic Flux Tubes with Kilogauss Field Strength Induced by Convective Instability Authors: Nagata, Shin'ichi; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Katsukawa, Yukio; Shimizu, Toshifumi; Yokoyama, Takaaki; Tarbell, Theodore D.; Lites, Bruce W.; Shine, Richard A.; Berger, Thomas E.; Title, Alan M.; Bellot Rubio, Luis R.; Orozco Suárez, David Bibcode: 2008ApJ...677L.145N Altcode: Convective instability has been a mechanism used to explain the formation of solar photospheric flux tubes with kG field strength. However, the turbulence of the Earth's atmosphere has prevented ground-based observers from examining the hypothesis with precise polarimetric measurement on the subarcsecond scale flux tubes. Here we discuss observational evidence of this scenario based on observations with the Solar Optical Telescope (SOT) aboard Hinode. The cooling of an equipartition field strength flux tube precedes a transient downflow reaching 6 km s-1 and the intensification of the field strength to 2 kG. These observations agree very well with the theoretical predictions. Title: Hinode SOT Observations of Solar Quiescent Prominence Dynamics Authors: Berger, Thomas E.; Shine, Richard A.; Slater, Gregory L.; Tarbell, Theodore D.; Title, Alan M.; Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Suematsu, Yoshinori; Tsuneta, Saku; Lites, Bruce W.; Shimizu, Toshifumi Bibcode: 2008ApJ...676L..89B Altcode: We report findings from multihour 0.2'' resolution movies of solar quiescent prominences (QPs) observed with the Solar Optical Telescope (SOT) on the Hinode satellite. The observations verify previous findings of filamentary downflows and vortices in QPs. SOT observations also verify large-scale transverse oscillations in QPs, with periods of 20-40 minutes and amplitudes of 2-5 Mm. The upward propagation speed of several waves is found to be ~10 km s-1, comparable to the sound speed of a 10,000 K plasma, implying that the waves are magnetoacoustic in origin. Most significantly, Hinode SOT observations reveal that dark, episodic upflows are common in QPs. The upflows are 170-700 km in width, exhibit turbulent flow, and rise with approximately constant speeds of ~20 km s-1 from the base of the prominence to heights of ~10-20 Mm. The upflows are visible in both the Ca II H-line and Hα bandpasses of SOT. The new flows are seen in about half of the QPs observed by SOT to date. The dark upflows resemble buoyant starting plumes in both their velocity profile and flow structure. We discuss thermal and magnetic mechanisms as possible causes of the plumes. Title: Emergence of a Helical Flux Rope under an Active Region Prominence Authors: Okamoto, Takenori J.; Tsuneta, Saku; Lites, Bruce W.; Kubo, Masahito; Yokoyama, Takaaki; Berger, Thomas E.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Nagata, Shin'ichi; Shibata, Kazunari; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M. Bibcode: 2008ApJ...673L.215O Altcode: 2008arXiv0801.1956O Continuous observations were obtained of NOAA AR 10953 with the Solar Optical Telescope (SOT) on board the Hinode satellite from 2007 April 28 to May 9. A prominence was located over the polarity inversion line (PIL) to the southeast of the main sunspot. These observations provided us with a time series of vector magnetic fields on the photosphere under the prominence. We found four features: (1) The abutting opposite-polarity regions on the two sides along the PIL first grew laterally in size and then narrowed. (2) These abutting regions contained vertically weak but horizontally strong magnetic fields. (3) The orientations of the horizontal magnetic fields along the PIL on the photosphere gradually changed with time from a normal-polarity configuration to an inverse-polarity one. (4) The horizontal magnetic field region was blueshifted. These indicate that helical flux rope was emerging from below the photosphere into the corona along the PIL under the preexisting prominence. We suggest that this supply of a helical magnetic flux to the corona is associated with evolution and maintenance of active region prominences. Title: The Altcriss project on board the International Space Station Authors: Casolino, M.; Minori, M.; Picozza, P.; Fuglesang, C.; Galper, A.; Popov, A.; Benghin, V.; Petrov, V. M.; Nagamatsu, A.; Berger, T.; Reitz, G.; Durante, M.; Pugliese, M.; Roca, V.; Sihver, L.; Cucinotta, F.; Semones, E.; Shavers, M.; Guarnieri, V.; Lobascio, C.; Castagnolo, D.; Fortezza, R. Bibcode: 2008ICRC....1..489C Altcode: 2008ICRC...30a.489C The Altcriss project aims perform long term measurement of the radiation environment in different points of the International Space Station. To achieve this goal, it employs an active silicon detector, Sileye-3/Alteino, to monitor nuclei up to Iron in the energy range above 40 MeV/n. Both long term modulation of galactic cosmic rays going toward solar minimum and solar particles events will be observed. A number of different dosimeters are being employed to measure the dose and compare it with the silicon detector data. Another aim of the project is to monitor the effectiveness of shielding materials in orbit: a set of polyethylene tiles is placed in the detector acceptance window and particle flux and composition is compared with measurements in the same locations without shielding. Dosimeters are thus placed behind the shielding material and in an unshielded location to cross-correlate this information. The observation campaign begun in December 2005 and is running continuously ever since. Active and passive data have been retreived at the end of expedition 13, 14 and Astrolab mission. In this work we will describe the experiment and the preliminary results. Title: The Horizontal Magnetic Flux of the Quiet-Sun Internetwork as Observed with the Hinode Spectro-Polarimeter Authors: Lites, B. W.; Kubo, M.; Socas-Navarro, H.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2008ApJ...672.1237L Altcode: Observations of very quiet Sun using the Solar Optical Telescope/Spectro-Polarimeter (SOT/SP) aboard the Hinode spacecraft reveal that the quiet internetwork regions are pervaded by horizontal magnetic flux. The spatial average horizontal apparent flux density derived from wavelength-integrated measures of Zeeman-induced linear polarization is BTapp = 55 Mx cm -2, as compared to the corresponding average vertical apparent flux density of | BLapp| = 11 Mx cm -2. Distributions of apparent flux density are presented. Magnetic fields are organized on mesogranular scales, with both horizontal and vertical fields showing "voids" of reduced flux density of a few granules spatial extent. The vertical fields are concentrated in the intergranular lanes, whereas the stronger horizontal fields are somewhat separated spatially from the vertical fields and occur most commonly at the edges of the bright granules. High-S/N observations from disk center to the limb help to constrain possible causes of the apparent imbalance between | BLapp| and BTapp, with unresolved structures of linear dimension on the surface smaller by at least a factor of 2 relative to the SOT/SP angular resolution being one likely cause of this discrepancy. Other scenarios for explaining this imbalance are discussed. The horizontal fields are likely the source of the "seething" fields of the quiet Sun discovered by Harvey et al. The horizontal fields may also contribute to the "hidden" turbulent flux suggested by studies involving Hanle effect depolarization of scattered radiation. Title: Depth dose distributions measured with thermoluminescence detectors inside the anthropomorphic torso of the MATROSHKA experiment inside and outside the ISS Authors: Berger, Thomas; Reitz, Guenther; Hajek, Michael; Bergmann, Robert; Bilski, Pawel; Puchalska, Msc. Monika Bibcode: 2008cosp...37..257B Altcode: 2008cosp.meet..257B The ESA MATROSHKA (MTR) facility was realized through the German Aerospace Center, DLR, Cologne, as main contractor, aiming for the determination of skin and organ doses within a simulated human upper torso. MTR simulates, by applying an anthropomorphic upper torso, as exact as possible an astronaut performing either an extravehicular activity (EVA) (MTR Phase 1) or an astronaut working inside the International Space Station (MTR Phase 2A). It consists of a human phantom, a Base Structure and a Carbon fibre container - simulating the astronaut‘s space suit. The phantom itself is made up of 33 slices composed of natural bones, embedded in tissue equivalent plastic of different density for tissue and lung. The Phantom slices are equipped with channels and cut-outs to allow the accommodation of active and passive dosemeters, temperature and pressure sensors. Over 4800 passive detectors (thermoluminescence detectors (TLDs) and plastic nuclear track detectors) constitute the radiation experiments which are beside inside the phantom also located on top the head of the phantom, in front of the belly and around the body as part of a Poncho and a Hood. In its 1st exposure phase (MTR 1: 2004 - 2005) MTR measured the depth dose distribution of an astronaut performing an EVA - mounted outside the Zvezda Module. In its 2nd exposure phase the phantom was positioned inside the ISS to monitor the radiation environment and measure the depth dose distribution in dependence on the inside shielding configurations. The majority of the TLDs provided for the determination of the depth dose distribution was provided by IFJ-PAN, ATI and DLR. Data of "combined" depth dose distribution of the three different groups will be shown for the MTR-1 exposure (outside the ISS) and the MTR-2A (inside the ISS). The discussion will focus on the difference in depth dose as well as skin dose distribution based on the different shielding thickness provided by the two experimental phases. Title: Vertical plasma motions in prominence sheets observed by Hinode Authors: Panasenco, Olga; Velli, Marco; Berger, Thomas Bibcode: 2008cosp...37.2337P Altcode: 2008cosp.meet.2337P We analyze the approximately vertical motions inside prominence plasma observed by Hinode on 25 April 2007 in Hα line and 30 November 2006 in CaH line. Well-established observational facts are that all filaments (prominences on the limb) are composed of fine threads of similar dimensions, rooted in the photosphere and presumably tracing magnetic field lines, and that continuous counter-streaming motions occur along threads. We take into account the geometry of the prominence sheet and the viewing angle to reduce possible projection effect and more correctly interpret the nature of observational downward flows of denser and cooler plasma as well as the upward flow of hotter plasma which appears dark in the Hα and CaH spectral lines. The dark upflows exhibit turbulent flow properties such as vortex formation and shedding that are consistent with the properties of thermal starting plumes. Sometimes an illusion of dark upward motion is generated by rarefactions in the plasma sheet caused by the cooler denser downward flows. On both dates, we suspect there is probably more filament mass in the prominence that is visible in either the Hα or CaH lines. The source of the downward moving plasma may be located either higher above the visible upper edge of the prominence or on the far end of the prominence spine. The bright downward motions of the more cool and dense plasma may be partly due to the counter-streaming motion along the magnetic fields lines, or it may be due to the presence of rayleigh-taylor type or ballooning/interchange instabilities in the upper regions of the prominence, which are then stabilized lower down where the magnetic field is stronger and the plasma beta lower. Title: Small-Scale Jetlike Features in Penumbral Chromospheres Authors: Katsukawa, Y.; Berger, T. E.; Ichimoto, K.; Lites, B. W.; Nagata, S.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M.; Tsuneta, S. Bibcode: 2007Sci...318.1594K Altcode: We observed fine-scale jetlike features, referred to as penumbral microjets, in chromospheres of sunspot penumbrae. The microjets were identified in image sequences of a sunspot taken through a Ca II H-line filter on the Solar Optical Telescope on board the Japanese solar physics satellite Hinode. The microjets’ small width of 400 kilometers and short duration of less than 1 minute make them difficult to identify in existing observations. The microjets are possibly caused by magnetic reconnection in the complex magnetic configuration in penumbrae and have the potential to heat the corona above a sunspot. Title: Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection Authors: Shibata, Kazunari; Nakamura, Tahei; Matsumoto, Takuma; Otsuji, Kenichi; Okamoto, Takenori J.; Nishizuka, Naoto; Kawate, Tomoko; Watanabe, Hiroko; Nagata, Shin'ichi; UeNo, Satoru; Kitai, Reizaburo; Nozawa, Satoshi; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Tarbell, Theodore D.; Berger, Thomas E.; Lites, Bruce W.; Shine, Richard A.; Title, Alan M. Bibcode: 2007Sci...318.1591S Altcode: 2008arXiv0810.3974S The heating of the solar chromosphere and corona is a long-standing puzzle in solar physics. Hinode observations show the ubiquitous presence of chromospheric anemone jets outside sunspots in active regions. They are typically 3 to 7 arc seconds = 2000 to 5000 kilometers long and 0.2 to 0.4 arc second = 150 to 300 kilometers wide, and their velocity is 10 to 20 kilometers per second. These small jets have an inverted Y-shape, similar to the shape of x-ray anemone jets in the corona. These features imply that magnetic reconnection similar to that in the corona is occurring at a much smaller spatial scale throughout the chromosphere and suggest that the heating of the solar chromosphere and corona may be related to small-scale ubiquitous reconnection. Title: Hinode SOT observations of plume upflows and cascading downflows in quiescent solar prominences Authors: Berger, T.; Shine, R.; Slater, G.; Tarbell, T.; Title, A.; Lites, B.; Tsuneta, S.; Okamoto, T. J.; Ichimoto, K.; Katsukawa, Y.; Sekii, T.; Suematsu, Y.; Shimizu, T. Bibcode: 2007AGUFMSH53A1065B Altcode: We present several Hinode SOT filtergram movies of quiescent solar prominences that show newly discovered "plume-like" upflows and cascading "waterfall-like" downflows that persist for the entire multi-hour duration of the observations. The flow speeds are on the order of 10 km/sec with typical widths of 400-700 km. Preliminary calculations show that if the upflows are buoyancy driven, the associated thermal perturbation is on the order of 10,000 K, sufficient to explain the dark appearance of the upflows in the interference filter passbands. In addition we observe rotational vortices and body oscillations within the prominences. These new observations challenge current magnetostatic models of solar prominences by showing that prominence plasmas are in constant motion, often in directions perpendicular to the magnetic field lines proposed by the models. TRACE, Hinode/EIS, and Hinode/XRT observations are used to investigate the differential topology of the flows across temperature regimes. Title: On the Chromospheric Micro-jets Associated with the Penumbral Filaments Authors: Ryutova, M.; Berger, T.; Tarbell, T.; Frank, Z.; Title, A. Bibcode: 2007AGUFMSH22A0843R Altcode: We present observations of sunspot penumbrae obtained during the disk passage of AR 10923 (November 10--20, 2006) with the Solar Optical Telescope (SOT) on the Hinode satellite. Co-aligned multi-hour movies taken simultaneously in several wavelengths show fine-scale dynamics at the sub-arcsecond level. The dynamics include helical flows along penumbral filaments, branching of filaments, and penumbral "micro-jets" recently described by Katsukawa et al. (AAS 210, 94.13). We present quantitative analyzes of the penumbral jets and interpret them relative to our recent model of penumbral filaments (Ryutova, Berger and Title, 2007, in "Collective phenomena in macroscopic systems", Ed. G. Bertin, et al., World Scientific) to show that the jets are the result of magnetic reconnection of the helical field lines in neighboring non-collinear filaments. Title: Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence Authors: Okamoto, T. J.; Tsuneta, S.; Berger, T. E.; Ichimoto, K.; Katsukawa, Y.; Lites, B. W.; Nagata, S.; Shibata, K.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M. Bibcode: 2007Sci...318.1577O Altcode: 2008arXiv0801.1958O Solar prominences are cool 104 kelvin plasma clouds supported in the surrounding 106 kelvin coronal plasma by as-yet-undetermined mechanisms. Observations from Hinode show fine-scale threadlike structures oscillating in the plane of the sky with periods of several minutes. We suggest that these represent Alfvén waves propagating on coronal magnetic field lines and that these may play a role in heating the corona. Title: Initial Helioseismic Observations by Hinode/SOT Authors: Sekii, Takashi; Kosovichev, Alexander G.; Zhao, Junwei; Tsuneta, Saku; Shibahashi, Hiromoto; Berger, Thomas E.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Lites, Bruce; Nagata, Shin'ichi; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M. Bibcode: 2007PASJ...59S.637S Altcode: 2007arXiv0709.1806S Results from initial helioseismic observations by the Solar Optical Telescope on-board Hinode are reported. It has been demonstrated that intensity oscillation data from the Broadband Filter Imager can be used for various helioseismic analyses. The k - ω power spectra, as well as the corresponding time-distance cross-correlation function, which promise high-resolution time-distance analysis below the 6-Mm travelling distance, were obtained for G-band and CaII-H data. Subsurface supergranular patterns were observed from our first time-distance analysis. The results show that the solar oscillation spectrum is extended to much higher frequencies and wavenumbers, and the time-distance diagram is extended to much shorter travel distances and times than were observed before, thus revealing great potential for high-resolution helioseismic observations from Hinode. Title: Hinode Observations of Horizontal Quiet Sun Magnetic Flux and the ``Hidden Turbulent Magnetic Flux'' Authors: Lites, Bruce; Socas-Navarro, Hector; Kubo, Masahito; Berger, Thomas; Frank, Zoe; Shine, Richard A.; Tarbell, Theodore D.; Title, Alan M.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Tsuneta, Saku; Suematsu, Yoshinori; Shimizu, Toshifumi Bibcode: 2007PASJ...59S.571L Altcode: We present observations of magnetic fields of the very quiet Sun near disk center using the Spectro-Polarimeter of the Solar Optical Telescope aboard the Hinode satellite. These observations reveal for the first time the ubiquitous presence of horizontal magnetic fields in the internetwork regions. The horizontal fields are spatially distinct from the vertical fields, demonstrating that they are not arising mainly from buffeting of vertical flux tubes by the granular convection. The horizontal component has an average ``apparent flux density'' of 55Mxcm-2 (assuming the horizontal field structures are spatially resolved), in contrast to the average apparent vertical flux density of 11Mxcm-2. The vertical fields reside mainly in the intergranular lanes, whereas the horizontal fields occur mainly over the bright granules, with a preference to be near the outside edge of the bright granules. The large apparent imbalance of vertical and horizontal flux densities is discussed, and several scenarios are presented to explain this imbalance. Title: Penumbral Dynamics and its Manifestation in the Overlying Chromosphere Authors: Ryutova, Margarita; Berger, Thomas; Tarbell, Theodor; Frank, Zoe; Title, Alan Bibcode: 2007APS..DPPYP8056R Altcode: Mature sunspots are usually surrounded by penumbra - a dense conglomerate of a random interlaced flux tubes with varying inclinations. High resolution observations show a fine sub-structure of penumbral filaments and new regularities in their dynamics. These regularities fit well our recent model of penumbra based on cascading reconnection events occurring in the system of non-collinear flux tubes. Each act of reconnection generates twist in the reconnected filaments and facilitates the onset of a screw pinch instability, consistent with the observations showing that individual filaments are cylindrical helices with a pitch/radius ratio providing their stability. In addition, the post-reconnection products produce a sling-shot effect that generates oblique shocks and leads to appearence of a lateral jets. Here we report high resolution (120-180 km) high cadence (15-30 sec) observations taken with the Solar Optical Telescope (SOT) on the Hinode satellite. Co-aligned multi-hour movies taken simultaneously in several wavelengths show detailed behavior of penumbra filaments and their effect on the overlying chromosphere. We confirm the ubiquitous nature of penumbral micro-jets recently discovered by SOT instrument (Katsukawa et al. 2007, AAS 210, 94.13), and present quantitative analysis of chromospheric jets based on our recent model of penumbra. Title: Flare Ribbons Observed with G-band and FeI 6302Å, Filters of the Solar Optical Telescope on Board Hinode Authors: Isobe, Hiroaki; Kubo, Masahito; Minoshima, Takashi; Ichimoto, Kiyoshi; Katsukawa, Yukio; Tarbell, Theodore D.; Tsuneta, Saku; Berger, Thomas E.; Lites, Bruce; Nagata, Shin'ichi; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Title, Alan M. Bibcode: 2007PASJ...59S.807I Altcode: 2007arXiv0711.3946I The Solar Optical Telescope (SOT) on board the Hinode satellite observed an X3.4 class flare on 2006 December 13. A typical two-ribbon structure was observed, not only in the chromospheric CaII H line, but also in the G-band and FeI 6302Å line. The high-resolution, seeing-free images achieved by SOT revealed, for the first time, sub-arcsec fine structures of the ``white light'' flare. The G-band flare ribbons on sunspot umbrae showed a sharp leading edge, followed by a diffuse inside, as well as a previously known core-halo structure. The underlying structures, such as umbral dots, penumbral filaments, and granules, were visible in the flare ribbons. Assuming that the sharp leading edge was directly heated by a particle beam and the diffuse parts were heated by radiative back-warming, we estimated the depth of the diffuse flare emission using an intensity profile of the flare ribbon. We found that the depth of the diffuse emission was about 100km or less from the height of the source of radiative back-warming. The flare ribbons were also visible in the Stokes-V images of FeI 6302Å, as a transient polarity reversal. This is probably related to a ``magnetic transient'' reported in the literature. The intensity increase in Stokes-I images indicates that the FeI 6302Å line was significantly deformed by the flare, which may cause such a magnetic transient. Title: Formation Process of a Light Bridge Revealed with the Hinode Solar Optical Telescope Authors: Katsukawa, Yukio; Yokoyama, Takaaki; Berger, Thomas E.; Ichimoto, Kiyoshi; Kubo, Masahito; Lites, Bruce; Nagata, Shin'ichi; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M.; Tsuneta, Saku Bibcode: 2007PASJ...59S.577K Altcode: 2007arXiv0709.2527K The Solar Optical Telescope (SOT) on-board Hinode successfully and continuously observed the formation process of a light bridge in a matured sunspot of the NOAA active region 10923 for several days with high spatial resolution. During its formation, many umbral dots were observed to be emerging from the leading edges of penumbral filaments, and rapidly intruding into the umbra. The precursor of the light bridge formation was also identified as a relatively slow inward motion of the umbral dots, which emerged not near the penumbra, but inside the umbra. The spectro-polarimeter on SOT provided physical conditions in the photosphere around the umbral dots and the light bridges. We found that the light bridges and the umbral dots had significantly weaker magnetic fields associated with upflows relative to the core of the umbra, which implies that there was hot gas with weak field strength penetrating from the subphotosphere to near the visible surface inside those structures. There needs to be a mechanism to drive the inward motion of the hot gas along the light bridges. We suggest that the emergence and the inward motion are triggered by a buoyant penumbral flux tube as well as subphotospheric flow crossing the sunspot. Title: Hinode Observations of the Onset Stage of a Solar Filament Eruption Authors: Sterling, Alphonse C.; Moore, Ronald L.; Berger, Thomas E.; Bobra, Monica; Davis, John M.; Jibben, Patricia; Kano, Ryohei; Lundquist, Loraine L.; Myers, D.; Narukage, Noriyuki; Sakao, Taro; Shibasaki, Kiyoto; Shine, Richard A.; Tarbell, Theodore D.; Weber, Mark Bibcode: 2007PASJ...59S.823S Altcode: We used Hinode X-Ray Telescope (XRT) and Solar Optical Telescope (SOT) filtergraph (FG) Stokes-V magnetogram observations, to study the early onset of a solar eruption that includes an erupting filament that we observe in TRACE EUV images. The filament undergoes a slow rise for at least 20min prior to its fast eruption and strong soft X-ray (SXR) flaring; such slow rises have been previously reported, and the new Hinode data elucidate the physical processes occurring during this period. XRT images show that during the slow-rise phase, an SXR sigmoid forms from apparent reconnection low in the sheared core field traced by the filament, and there is a low-level intensity peak in both EUV and SXRs during the slow rise. MDI and SOT FG Stokes-V magnetograms show that the pre-eruption filament is along a neutral line between opposing-polarity enhanced network cells, and the SOT magnetograms show that these opposing fields are flowing together and canceling for at least six hours prior to eruption. From the MDI data we measured the canceling network fields to be ∼ 40G, and we estimated that ∼ 1019 Mx of flux canceled during the five hours prior to eruption; this is only ∼ 5% of the total flux spanned by the eruption and flare, but apparently its tether-cutting cancellation was enough to destabilize the sigmoid field holding the filament and resulted in that field's eruption. Title: What are 'Faculae'? Authors: Berger, T. E.; Title, A. M.; Tarbell, T.; Rouppe van der Voort, L.; Löfdahl, M. G.; Scharmer, G. B. Bibcode: 2007ASPC..369..103B Altcode: We present very high resolution filtergram and magnetogram observations of solar faculae taken at the Swedish 1-meter Solar Telescope (SST) on La Palma. Three datasets with average line-of-sight angles of 16, 34, and 53 degrees are analyzed. The average radial extent of faculae is at least 400~km. In addition we find that contrast versus magnetic flux density is nearly constant for faculae at a given disk position. These facts and the high resolution images and movies reveal that faculae are not the interiors of small flux tubes - they are granules seen through the transparency caused by groups of magnetic elements or micropores ``in front of'' the granules. Previous results which show a strong dependency of facular contrast on magnetic flux density were caused by bin-averaging of lower resolution data leading to a mixture of the signal from bright facular walls and the associated intergranular lanes and micropores. The findings are relevant to studies of total solar irradiance (TSI) that use facular contrast as a function of disk position and magnetic field in order to model the increase in TSI with increasing sunspot activity. Title: Estimate on SOT Light Level in Flight with Throughput Measurements in SOT Sun Tests Authors: Shimizu, T.; Kubo, M.; Tarbell, T. D.; Berger, T. E.; Suematsu, Y.; Ichimoto, K.; Katsukawa, Y.; Miyashita, M.; Noguchi, M.; Nakagiri, M.; Tsuneta, S.; Elmore, D. F.; Lites, B. W. Bibcode: 2007ASPC..369...51S Altcode: The SOT (Solar Optical Telescope, e.g., Shimizu 2004) optical system consists of 50cm-aperture optical telescope (OTA) and focal plane instrument (FPP). The solar light into the telescope penetrates through many optical elements located in OTA and FPP before illuminating CCDs. Natural solar light was fed to the integrated SOT in sun tests for verifying various optical aspects including the confirmation of photon throughput. CCD exposures provide the number of photons accumulated in an exposure duration with a clean-room test condition. To estimate the absolute intensity of the solar light at the telescope entrance in the clean-room test condition, we developed a pinhole-PSD sensor for simultaneous monitoring the solar light outside the clean room and measured the transmission of light through two flat mirrors of the heliostat and clean-room entrance window glass as a function of wavelength. The PSD sensor was pre-calibrated with continuous monitoring the solar light in a day long under a clear constant sky condition, determining the earth atmospheric attenuation and the PSD output for the solar light on orbit. These throughput measurements have provided an estimate on photon throughput for the SOT flight model. The results confirm suitable number of photons without saturation for proper CCD exposures in flight. Title: Contrast Analysis of Solar Faculae and Magnetic Bright Points Authors: Berger, T. E.; Rouppe van der Voort, L.; Löfdahl, M. Bibcode: 2007ApJ...661.1272B Altcode: The morphology and contrast of small-scale solar magnetic elements at four disk positions is analyzed. The data were obtained at the Swedish 1 m Solar Telescope (SST) over 3 yr (2003-2005). Two of the data sets have disk positions near disk center (average μ=cosθ>0.8) and show numerous ``magnetic bright points'' (MBPs), and two are sufficiently limbward to show prominent ``faculae'' (average μ<=0.6). The filtergrams are obtained in the 430.5 nm G band and 436.4 nm ``continuum'' bandpasses; the magnetograms are Fe I 630.25 nm Stokes V images taken with the Solar Optical Universal Polarimeter (SOUP) tunable filter. In all images we achieve nearly diffraction-limited resolution (~100 km in the G band). Analysis shows that MBPs and faculae are distinct radiative signatures of the magnetic field: MBPs have a constant or slightly decreasing contrast with increasing magnetogram signal, while facular contrast increases linearly with magnetogram signal. Faculae are much larger than MBPs, with an average radial width of 400 km. The observations support recent modeling showing that faculae are granules seen through the opacity reduction provided by magnetic elements (or groups thereof), while MBPs are caused by lateral radiation leakage scattering from deeper layers of the magnetic element. Title: Chromospheric Micro-jets Discovered Above Sunspot Penumbrae Authors: Katsukawa, Yukio; Tsuneta, S.; Suematsu, Y.; Ichimoto, K.; Shimizu, T.; Kubo, M.; Nagata, S.; Berger, T.; Tarbell, T.; Shine, R.; Title, A. Bibcode: 2007AAS...210.9413K Altcode: 2007BAAS...39..219K The Solar Optical Telescope (SOT) aboard HINODE allows us to observe dynamical activities in the solar photosphere and the chromosphere with high and stable image quality of 0.2 arcseconds. This superior performance of SOT provides new findings of fine-scale transient activities occurring in the chromosphere. In this paper, we report discovery of fine-scale jet-like phenomena ubiquitously observed above sunspot penumbrae. The jets are identified in image sequences of a sunspot taken through a Ca II H line filter at 3968A. The Ca II H line is sensitive to about 10^4 K plasma in the chromosphere.

Their length is typically between 3000 and 10000km, and their width is smaller than 500km. It is notable that their lifetime is shorter than 1 minute. Those small spatial and temporal scale possibly makes it difficult to identify the phenomena in existing ground-based observations. The jets are easily identified when a sunspot is located far from the disk center, and motion of the bright features suggests that mass is erupted from lower chromosphere to upper atmosphere. Velocities of the motion are estimated to be 50 to 100 km/s from their lateral motion of intensity patterns. The velocities are much faster than sound speeds in the chromosphere. A possible cause of such high-speed jets is magnetic reconnection at the lower chromosphere resulted from fluted magnetic configuration in penumbrae which is suggested by vector magnetic field measurements in the photosphere. Title: Magnetic Patches in Internetwork Quiet Sun Authors: De Wijn, Alfred; Lites, B.; Berger, T.; Shine, R.; Title, A.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Hinode Team Bibcode: 2007AAS...210.9412D Altcode: 2007BAAS...39Q.219D We study strong flux elements in the quiet sun in the context of the nature of quiet-sun magnetism, its coupling to chromospheric, transition-region and coronal fields, and the nature of a local turbulent dynamo. Strong, kilogauss flux elements show up intermittently as small bright points in G-band and Ca II H images. Although bright points have been extensively studied in the magnetic network, internetwork magnetism has only come under scrutiny in recent years. A full spectrum of field strengths seems to be ubiquitously present in the internetwork at small spatial scales, with the stronger elements residing in intergranular lanes. De Wijn et al. (2005) found that bright points in quiet sun internetwork areas appear recurrently with varying intensity and horizontal motion within long-lived patches that outline cell patterns on mesogranular scales. They estimate that the "magnetic patches" have a mean lifetime of nine hours, much longer than granular timescales. We use multi-hour sequences of G-band and Ca II H images as well as magnetograms recorded by the Hinode satellite to follow up on their results. The larger field of view, the longer sequences, the addition of magnetograms, and the absence of atmospheric seeing allows us to better constrain the patch lifetime, to provide much improved statistics on IBP lifetime, to compare IBPs to network bright points, and to study field polarity of IBPs in patches and between nearby patches.

Hinode is an international project supported by JAXA, NASA, PPARC and ESA. We are grateful to the Hinode team for all their efforts in the design, build and operation of the mission. Title: Hinode/SOT Observations Of Apparent "Thermal Plume" Motions In A Solar Prominence Authors: Berger, Thomas; Tarbell, T.; Slater, G.; Tsuneta, S.; Suematsu, Y.; Ichimoto, K.; Katsukawa, Y.; Shimizu, T.; Kubo, M.; Nagata, S. Bibcode: 2007AAS...210.9433B Altcode: 2007BAAS...39..222B We present 396.8 nm Ca II H-line observations of a large hedgerow, or "sheet", prominence seen on the solar western limb on 30-November-2006. The 16 second cadence observations show dark channels rising vertically at speeds of approximately 10 km/sec to heights of about 15 Mm above the limb. Many of the motions end in vortical overturning near the top of the sheet . Bright downflows of similar speed are also seen within the sheet, often in association with a dark channel that has risen to the top of the sheet. The dark channels are suggestive of hot material rising in thermal plumes within the prominence sheet. Similarly, the bright material motions appear to be density enhanced regions of turbulent downflow. Current models of sheet prominences do not include the observed dynamics. In these models, the prominence plasma is in a low-beta state and is constrained to move only along magnetic field lines. However the motions observed here are extremely complex, implying either that the magnetic field lines are undergoing turbulent motion, thus tangling and reconnecting constantly, or that the plasma is not constrained by the field and is in a high-beta convective state. We measure the motion of several representative "plumes" and downflows, estimate the density and temperature of the prominence plasma, and suggest several avenues for further investigation.

This work was supported by NASA under the Hinode/SOT contract NNM07AA01C. Title: Hinode Observations of Umbral Dots Authors: Hurlburt, Neal E.; Berger, T.; Ichimoto, K.; SOT Team Bibcode: 2007AAS...210.9409H Altcode: 2007BAAS...39..218H We analyze observations of sunspot umbra taken by the Solar Optical Telescope (SOT) on Hinode to ascertain the properties of umbral dots. The observations consist of coordinated, multi-wavelength observing sequences spanning several hours for each spot considered. Typically these multi-wavelength observations include longitudinal magnetograms in 6302, and filtergrams in Calcium II H, G-band and blue continuum. We report on the spatial and temporal properties of the umbral dots and their relation to the umbral field and overlying chromosphere.

This work was supported in part by NASA in part under the Hinode/SOT contract NNM07AA01C. Title: Ubiquitous Horizontal Magnetic Fields in the Quiet Solar Photosphere as Revealed by HINODE Meaurements Authors: Lites, Bruce W.; Socas Navarro, H.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Kubo, M.; Shimizu, T.; Nagata, S.; Hinode Team Bibcode: 2007AAS...210.6303L Altcode: 2007BAAS...39..171L Measurements with the HINODE Spectro-Polarimeter (SP) of the quiet Sun allow characterization of the weak, mixed-polarity magnetic flux at the highest angular resolution to date (0.3"), and with good polarimetric sensitivity(0.025% relative to the continuum). The image stabilization of the HINODE spacecraft allows long integrations with degradation of the image quality only by the evolution of the solar granulation. From the Stokes V profile measurements we find an average solar "Apparent Flux Density" of 14 Mx cm-2, with significant Stokes V signals at every position on the disk at all times. However, there are patches of meso-granular size (5-15") where the flux is very weak. At this high sensitivity, transverse fields produce measurable Stokes Q,U linear polarization signals over a majority of the area, with apparent transverse flux densities in the internetwork significantly larger than the corresponding longitudinal flux densities. When viewed at the center of the solar disk, the Stokes V signals (longitudinal fields) show a preference for occurrence in the intergranular lanes, and the Q,U signals occur preferably over the granule interiors, but neither association is exclusive.

Hinode is an international project supported by JAXA, NASA, PPARC and ESA. We are grateful to the Hinode team for all their efforts in the design, build and operation of the mission. Title: Discovery Of Cool Cloud-like Structures In The Corona With Hinode Solar Optical Telescope Authors: Okamoto, Takenori; Tsuneta, S.; Katsukawa, Y.; Ichimoto, K.; Suematsu, Y.; Shimizu, T.; Nagata, S.; Shibata, K.; Tarbell, T.; Shine, R.; Berger, T.; Lites, B.; Myers, D. Bibcode: 2007AAS...210.9426O Altcode: 2007BAAS...39..221O A solar observation satellite Hinode (Japanese for sun rise) was launched in September 2006.Hinode carried 3 advanced solar telescopes, visible light telescope, EUV imaging spectrometer, and X-ray telescope to simultaneously observe the photosphere, chromosphere, transition region, and corona. In the performance verification phase of the Hinode spacecraft with its telescopes, we observed an active region AR10921 near the west limb of the solar disk on November 9 2006. At this point, we planned to observe spicules on the limb with a broadband filter dedicated to Ca II H line (3968A). Ca II-H emission line (3968A) comes from plasma with temperature of approx. 10(4) K, which is much lower than the coronal temperature of 10(6-7) K. In addition to spectacular spicules, we find a large cloud-like structure located 10,000-20,000 km above the limb. The cloud has a very complex fine structure with dominant horizontal thread-like structure. Some features are moving horizontally and also have clear vertical oscillatory motions. The periods and amplitudes of these oscillations are 130-250 seconds and 200-850 km, respectively. The vertical oscillatory motion sometimes has a coherence length as long as 16,000 km. We conclude that from various observational features this vertical oscillation is a signature of Alfven waves propagating along the horizontal magnetic fields. We will discuss their origin and implications. Title: An Hα Surge Provoked by Moving Magnetic Features near an Emerging Flux Region Authors: Brooks, D. H.; Kurokawa, H.; Berger, T. E. Bibcode: 2007ApJ...656.1197B Altcode: We present a detailed study of Hα surges from cotemporal high-resolution multiwavelength images of NOAA AR 8227 obtained by the 50 cm Swedish Vacuum Solar Telescope (formerly situated on La Palma, Spain) and TRACE. We find that two kinds of collisions between opposite polarity magnetic flux produce the surges. First, one edge of an emerging flux region (EFR) collides with the preexisting magnetic field and causes continual surge activities, which have already been named EFR surges by previous authors. Secondly, moving magnetic features (MMFs), which emerge near the sunspot penumbra, pass through the ambient plasma and eventually collide with the opposite polarity magnetic field of the EFR. During their passage from the sunspot penumbra to the EFR, the MMFs constantly interacted with other magnetic elements and had a close relationship and showed similar flow patterns to Ca II K bright points. These brightenings were located at the leading edges of the MMFs. Cancellation of opposite polarity magnetic flux at the surge footpoint is observed, accompanied by chromospheric and coronal brightenings. We explain the evolutionary and morphological characteristics of the multiwavelength features associated with the Hα surges in both cases by the extension of previous 2D schematic models of reconnection in surges. Furthermore, by measuring the expansion velocity and photospheric magnetic field around the surge footpoint, we estimate a dimensionless reconnection rate of 0.04 (ratio of inflow velocity to Alfvén velocity). This is sufficient to produce a significant surge that heats the chromospheric plasma to coronal temperatures. Title: The Altcriss project on board the International Space Station Authors: Casolino, M.; Altamura, F.; Minori, M.; Picozza, P.; Fuglesang, C.; Galper, A.; Popov, A.; Benghin, V.; Petrov, V. M.; Nagamatsu, A.; Berger, T.; Reitz, G.; Durante, M.; Pugliese, M.; Roca, V.; Sihver, L.; Cucinotta, F.; Semones, E.; Shavers, M.; Guarnieri, V.; Lobascio, C.; Castagnolo, D.; Fortezza, R. Bibcode: 2007AdSpR..40.1746C Altcode: 2007arXiv0708.2586C The Altcriss project aims to perform a long term survey of the radiation environment on board the International Space Station. Measurements are being performed with active and passive devices in different locations and orientations of the Russian segment of the station. The goal is to perform a detailed evaluation of the differences in particle fluence and nuclear composition due to different shielding material and attitude of the station. The Sileye-3/Alteino detector is used to identify nuclei up to Iron in the energy range above ≃60 MeV/ n. Several passive dosimeters (TLDs, CR39) are also placed in the same location of Sileye-3 detector. Polyethylene shielding is periodically interposed in front of the detectors to evaluate the effectiveness of shielding on the nuclear component of the cosmic radiation. The project was submitted to ESA in reply to the AO in the Life and Physical Science of 2004 and data taking began in December 2005. Dosimeters and data cards are rotated every 6 months: up to now three launches of dosimeters and data cards have been performed and have been returned with the end of expedition 12 and 13. Title: Continuum Contrast as a function of Magnetic Flux Density and Disk Position: Results from a full Solar Cycle of SOHO/MDI data Authors: Soto, K.; Basri, G.; Ramos-Stierle, F.; Lewis, T.; Reiners, A.; Berger, T. Bibcode: 2006AGUFMSH11A0373S Altcode: The key to understanding total solar irradiance variability is to understand the mechanisms by continuum contrast is effected by the distribution of magnetic flux across the surface of the Sun. The Michelson Doppler Imager (MDI) instrument on the Solar and Heliospheric Observatory (SOHO) satellite has measured full-disk Stokes-V magnetograms along with cotemporal continuum images throughout Solar Cycle 23. We present the results of an examination of the relationship between corrected MDI continuum images with their cotemporal corrected MDI magnetograms. By separating the series of images into bins of Magnetic Flux Density (MFD) and limb angle, we perform a non-linear least squares fit to the data to produce a 3rd-order polynomial function of continuum contrast vs. MFD and disk position. Using the obtained function we can accurately predict continuum contrast at any given disk position as a function of MFD measured in a given magnetogram. The resulting predictions can be used to make simulated continuum images suitable for bolometric correction and input into total irradiance models. This research was partially supported by LWS TR&T Grant NNG05GK46G Title: Sunspot Contrast Measurements from MDI Full-Disk Images: Variations with Disk Position and Solar Cycle Phase Authors: Lewis, T.; Soto, K.; Basri, G.; Ramos-Stierle, F.; Reiners, A.; Berger, T. Bibcode: 2006AGUFMSH11A0374L Altcode: We report measurements of sunspot umbral and penumbral contrast as a function of Magnetic Flux Density (MFD), disk position, and time over Solar Cycle 23 from full-disk magnetogram and continuum images of the SOHO/MDI instrument. Using a technique of image segmentation which utilizes region labeling of entire MDI intensity images in order to segment prospective sunspots and then the application of radial derivatives from the centers of the spots we successfully identify the umbral-penumbral interface of large sunspots in the MDI database. The extracted penumbral and umbral pixels of these images are binned according to MFD and disk position to study the behavior of sunspot contrast. We report measurements of sunspot umbral and penumbral contrast as a function of Magnetic Flux Density (MFD), disk position, and time over Solar Cycle 23 from full- disk magnetogram and continuum images of the SOHO/MDI instrument. This research was partially supported by LWS TR&T Grant NNG05 GK48G. Title: Correction of MDI Full-Disk Magnetograms for Limb Angle Effects by the Assumption of Average Magnetic Uniformity Authors: Ramos-Stierle, F.; Soto, K.; Basri, G.; Lewis, T.; Reiners, A.; Berger, T. Bibcode: 2006AGUFMSH11A0375R Altcode: Analysis of magnetic fields on the sun is crucial to understanding the generation of solar active regions, plage, and the supergranular network and their contributions to Total Solar Irradiance (TSI) variation. The Michelson Doppler Imager (MDI) instrument on the Solar and Heliospheric Observatory (SOHO) satellite has measured full-disk Stokes-V magnetograms along with cotemporal continuum images throughout Solar Cycle 23. These pairs of images can be used to study continuum irradiance changes correlated to magnetogram signal over the entire disk and over most of Cycle 23. However the MDI magnetogram signal must be corrected for line-of-sight angle variations. Typically a 1/mu correction factor (where mu is the cosine of the line-of-sight angle to the surface normal) is applied across the entire disk. However near-limb measurements where mu approaches zero are siginificantly over-corrected by a simple 1/mu factor. We demonstrate a newly developed geometric correction function for MDI magnetograms based on the assumption that the distribution of Magnetic Flux Density (MFD) in the active latitudes should exhibit the same behavior no matter what angle it is viewed from. We examine a series of 106 magnetograms in the time period from 01-January-2001 to 30-April-2001. This method was successful in correcting MDI magnetograms to reasonable MFD in the limbs, with a minimal number of overcorrected points in the extreme limb, an improvement upon the typical approach of 1/mu. The resulting distributions of MFD were more uniform over 50 bins of mu and can be more successfully used to study continuum irradiance variations as a function of MFD across the entire disk. This research was partially supported by LWS TR&T Grant NNG05GK46G. Title: The visible-light broad-band imager for ATST: preliminary design Authors: Uitenbroek, Han; Tritschler, Alexandra; An, Hyun Kyoung; Berger, Thomas Bibcode: 2006SPIE.6269E..61U Altcode: 2006SPIE.6269E.193U This poster outlines the conceptual design of the Visible-light Broad-band Imager (VBI) instrument for the Advanced Technology Solar Telescope (ATST) as it follows from scientific requirements. The VBI is scheduled to be the first-light instrument of the ATST, highlighting the telescope's high spatial resolution capabilities. Title: Horizontal and Vertical Flow Structure in Emerging Flux Regions Authors: Kozu, Hiromichi; Kitai, Reizaburo; Brooks, David H.; Kurokawa, Hiroki; Yoshimura, Keiji; Berger, Thomas E. Bibcode: 2006PASJ...58..407K Altcode: In order to obtain an overall view of the flow structure of convective gas in emerging flux regions (EFRs), we studied three EFRs in two solar active regions, NOAA 8218 and NOAA 10774. Using the Local Correlation Tracking method, we found several horizontally divergent flow structures, which were stable over a period of 1 hour, in 2 EFRs in NOAA 8218. The horizontal flow velocities and the sizes of the structures were around 500m s-1 and about 4Mm in radius, respectively. We analyzed another dataset of NOAA 10774 using spectroscopic methods and found temporarily stable up-ward gas flows in the central part of the EFR. The line-of-sight velocities were around 150m s-1 and the size of the flow patch was 2 to 5Mm in radius. These results support our previous findings that convective-cell-like flow appears in the central part of an EFR. We estimated from these results that the depth of the flow cell in EFRs is about 600km, and the turn-over time of the cell is about 2 hours. Title: BRADOS Dose determination in the Russian Segment of the International Space Station Authors: Hajek, M.; Berger, T.; Fugger, M.; Fuerstner, M.; Vana, N.; Akatov, Y.; Shurshakov, V.; Arkhangelsky, V. Bibcode: 2006AdSpR..37.1664H Altcode: In the frame of the joint experiment BRADOS-1, absorbed dose and average linear energy transfer were assessed by means of 7LiF:Mg,Ti (TLD-700) thermoluminescence detectors for different panels onboard the Russian Segment of the International Space Station in the timeframe between February and October 2001 (248 days). A technique is presented to correct the measured absorbed dose values for thermoluminescent efficiency in the radiation climate onboard the spacecraft. Average linear energy transfer is determined from the high-temperature thermoluminescence emission in the TLD-700 glowcurve and used as a parameter in the thermoluminescent-efficiency correction. Depending on the shielding distribution, the efficiency-corrected absorbed dose varies between 168(2) μGy/d in panel No. 318 (core block ceiling) and 249(4) μGy/d in panel No. 443 (starboard-side commander cabin). The experimental data are compared with model calculations using detailed shielding distributions and orbit parameters as input. Title: Comparison of various techniques for the exact determination of absorbed dose in heavy ion fields using passive detectors Authors: Berger, T.; Reitz, G.; Hajek, M.; Vana, N. Bibcode: 2006AdSpR..37.1716B Altcode: Passive thermoluminescent detectors (TLDs) are commonly applied for the determination of absorbed dose in routine radiation protection. The usage of TLDs in heavy ion fields, e.g., in space dosimetry or for treatment planing in radiotherapy, requires the detailed knowledge of the efficiency of these detectors to the ion under study in dependence on the LET of the ion. This is due to the fact, that the detection efficiency of TLDs changes with increasing LET. If the changing efficiency of the TL-material is not taken into account, this would lead to a deviation of the measured absorbed dose. In the framework of the ICCHIBAN project - which was started as an intercomparison of passive and active detector systems used for dose determination in space - "BLIND" exposures were carried out. No information about dose and ion species was given to the investigators. Three different methods were used for the efficiency correction of TLDs after the BLIND exposures. The first method used the different LET efficiency of the TL-materials LiF:Mg, Ti and LiF:Mg, Cu, P to determine the LET and from this LET the efficiency of the LiF:Mg, Ti dosemeters. The second method used the high temperature emissions in LiF:Mg, Ti for the efficiency correction. The third method used a combination of TLDs and CR-39 track etch detectors to determine the total absorbed dose during the BLIND exposures. The paper will discuss the three methods, and focus on their applicability to precise dose determination and recalculation in space dosimetry. Title: Status of NSRL-ICCHIBAN, ICCHIBAN-7 and -8 and future ICCHIBAN experiments Authors: Uchihori, Y.; Benton, E. R.; Yasuda, N.; Kitamura, H.; Hajek, M.; Berger, T.; Zeitlin, C.; Miller, J. Bibcode: 2006cosp...36.3567U Altcode: 2006cosp.meet.3567U The ICCHIBAN InterComparison for Cosmic-rays with Heavy Ion Beams At NIRS project is an international collaboration established in order to intercompare detector response and intercalibrate space radiation instruments used for astronaut and cosmonaut dosimetry Over the past four years 20 laboratories in 12 nations have participated in eight ICCHIBAN experiments at the NIRS HIMAC in Japan and two ICCHIBAN experiments at accelerator facilities in the USA Results from the ICCHIBAN experiments have improved the calibration of space flight radiation instruments have proved useful in resolving discrepancies between measurements made by different instruments during space flight and have aided in analyzing and interpreting data obtained by both active and passive detectors exposed in low-Earth orbit We present here the current status of the ICCHIBAN project including the status of the ICCHIBAN-7 and ICCHIBAN-8 experiments carried out at HIMAC in Sept 2005 together with plans for future ICCHIBAN experiments Title: The MATROSHKA Facility - History and science overview Authors: Reitz, G.; Berger, T. Bibcode: 2006cosp...36.2259R Altcode: 2006cosp.meet.2259R The ESA MATROSHKA facility was realized through the German Aerospace Center DLR Cologne as main contractor On the 29th of January 2004 the facility was launched with a Russian PROGRESS vehicle to the International Space Station It was installed outside the Russian segment Zvezda on the 26th February 2004 and remained there until August 2005 and simulates as exact as possible an astronaut during an extravehicular activity EVA The MATROSHKA facility basically consists of a human phantom a Base Structure and a Container The container as well as the phantom is mounted to the base structure which serves as a footprint for the human phantom The container is a Carbon Fiber structure and forms with the Base Structure a closed volume that contains a dry oxygen atmosphere and protects the phantom against e g space vacuum space debris solar UV and material off-gassing It acts also as a simulation of the space suit The phantom body is made of commercial phantom parts well introduced in the field of radiotherapy It consists of 33 slices composed of natural bones embedded in tissue equivalent plastic of different density for tissue and lung The Phantom slices are equipped with channels and cut-outs to allow the accommodation of active and passive dosemeters temperature and pressure sensors The radiation experiments accommodated in the facility are performed under leadership of DLR in a cooperation of more than 15 research institutes from all over the world The MATROSHKA experiments represent therefore the currently biggest international Title: Dose distribution in a human phantom onboard aircraft Authors: Berger, T.; Meier, M.; Reitz, G.; Schridde, M. Bibcode: 2006cosp...36.2257B Altcode: 2006cosp.meet.2257B The exposure of aircrew personnel to cosmic radiation has been considered as occupational exposure in the European Union since the European Council Directive 96 29 EURATOM became effective on May 13 1996 In Germany the corresponding safety standards for aircrew which include dose assessment among other things are regulated by the German Radiation Protection Ordinance which implemented the European law and was amended in 2001 The radiation exposure of most German aircrew is calculated by the DLR Institute of Aerospace Medicine in Cologne applying the calculation program EPCARD in the framework of the aircrew dose determination system CALVADOS underline CAL culated and underline V erified underline A viation underline DOS imetry Beside the operational dose calculations DLR performs measuring flights applying active e g TEPC DOSTEL etc and passive TLDs bubble detectors radiation detectors to verify the calculation codes Within these activities the project BODO underline BO dy underline DO simetry comprised a long term exposure of a RANDO copyright anthropomorphic phantom to measure for the first time the skin and the depth dose distribution inside a simulated human torso at aviation altitudes The torso was flown for three months from mid of July to mid of October 2004 onboard a Lufthansa Cargo aircraft This torso made up of 27 polyurethane slices with different densities -- simulating tissue and organs -- was equipped with passive thermoluminescence detectors TLDs of different types namely TLD 600 6 LiF Mg Title: Performance of novel polymer shields aboard the ESA Biopan-5 mission Authors: Hajek, M.; Berger, T.; Fugger, M.; Vana, N. Bibcode: 2006cosp...36.2292H Altcode: 2006cosp.meet.2292H Radiation exposure of astronaut crew has been identified as a key issue in human spaceflight The reduction of dose by appropriate shielding measures is thus donated an essential role for the future development of space exploration particularly with regard to long-term interplanetary missions Optimization of shielding strategies and design may involve polymeric materials with enhanced hydrogen content specifically developed to attenuate high charge-and-energy HZE particles such as those encountered in galactic cosmic rays GCR The projectile energy loss is proportional to rho cdot Z A and reaches a maximum for hydrogen targets Light elements are also expected to minimize target fragmentation particularly the production of secondary neutrons The LETVAR experiment flow aboard the European Space Agency ESA Biopan-5 mission as part of a 27 kg payload attached to the external surface of the Foton-M2 descent capsule was dedicated to studying the shielding performance of three different polymers in reference to aluminium when exposed to the unshielded space environment in low-earth orbit LEO The mission was launched successfully on May 31 2005 from the Baikonur Cosmodrome Kazakhstan and spent 15 6 days at an orbital altitude between 262 and 304 km inclined by 63 r to the equatorial plane After recovery absorbed dose and average linear energy transfer LET were determined in front and behind the material slabs To support data interpretation material samples equivalent to those flown in space were exposed---to the extent possible Title: Inclination of magnetic fields and flows in sunspot penumbrae Authors: Langhans, K.; Scharmer, G. B.; Kiselman, D.; Löfdahl, M. G.; Berger, T. E. Bibcode: 2005A&A...436.1087L Altcode: An observational study of the inclination of magnetic fields and flows in sunspot penumbrae at a spatial resolution of 0.2 arcsec is presented. The analysis is based on longitudinal magnetograms and Dopplergrams obtained with the Swedish 1-m Solar Telescope on La Palma using the Lockheed Solar Optical Universal Polarimeter birefringent filter. Data from two sunspots observed at several heliocentric angles between 12 ° and 39 ° were analyzed. We find that the magnetic field at the level of the formation of the Fe i-line wing (630.25 nm) is in the form of coherent structures that extend radially over nearly the entire penumbra giving the impression of vertical sheet-like structures. The inclination of the field varies up to 45 ° over azimuthal distances close to the resolution limit of the magnetograms. Dark penumbral cores, and their extensions into the outer penumbra, are prominent features associated with the more horizontal component of the magnetic field. The inclination of this dark penumbral component - designated B - increases outwards from approximately 40 ° in the inner penumbra such that the field lines are nearly horizontal or even return to the solar surface already in the middle penumbra. The bright component of filaments - designated A - is associated with the more vertical component of the magnetic field and has an inclination with respect to the normal of about 35 ° in the inner penumbra, increasing to about 60 ° towards the outer boundary. The magnetogram signal is lower in the dark component B regions than in the bright component A regions of the penumbral filaments. The measured rapid azimuthal variation of the magnetogram signal is interpreted as being caused by combined fluctuations of inclination and magnetic field strength. The Dopplergrams show that the velocity field associated with penumbral component B is roughly aligned with the magnetic field while component A flows are more horizontal than the magnetic field. The observations give general support to fluted and uncombed models of the penumbra. The long-lived nature of the dark-cored filaments makes it difficult to interpret these as evidence for convective exchange of flux tubes. Our observations are in broad agreement with the two component model of Bellot Rubi et al. (2003), but do not rule out the embedded flux tube model of Solanki & Montavon (1993). Title: Magnetic Topology and Wave Propagation in the Solar Atmosphere Authors: Lawrence, J. K.; Cadavid, A. C.; McIntosh, S. W.; Berger, T. E. Bibcode: 2005AGUSMSH13C..01L Altcode: We analyze a 9 hr sequence of simultaneous, high resolution, 21 s cadence SVST G-band and K-line solar filtergrams plus magnetograms of lower cadence and resolution. The data include both network and internetwork areas (Berger and Title 2001, Cadavid, et al. 2003, Lawrence, et al. 2003). Time series of the G-band and K-line data are compared after filtering by a Morlet wavelet transform of period 2.5 min. On the average, the K-line signal is delayed by several seconds after the G-band signal Δ T = 8.6 ± 0.1 s for weak (|BZ| < 50 G) magnetic field in internetwork but Δ T = 7.2 ± 0.1 s for weak field in an area including network. The internetwork has no strong fields, but in network (|BZ| > 80 G) the mean delay time drops to Δ T = 3.4 ± 0.3 s. This is consistent with results by McIntosh, Fleck and Tarbell (2004) using TRACE 1600Å and 1700Å UV image series. Our principal result is that the time delay is greater in the internetwork than in the network by 1.4 ± 0.1 s, even for the same local magnetic field strength. This suggests that the difference must be an effect of the field topology. Spatial maps of time delays, in comparison to maps of such topological quantities as the height in the solar atmosphere at which the plasma β = 1, offer additional details of the relationship between wave propagation and the magnetic fields in the solar atmosphere. This work was supported in part by grants NSF-ATM 9987305 and NASA-NAG5-10880. The SVST is operated by the Swedish Royal Academy of Sciences at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Berger, T.E. and Title, A.M. 2001, ApJ, 553, 449. Cadavid, A.C., et al. 2003, ApJ, 586, 1409. Lawrence, J.K., et al. 2003, ApJ, 597, 1178. McIntosh, S.W., Fleck, B. and Tarbell, T.D. 2004, ApJ, 609, L95. Title: High resolution magnetogram measurements of solar faculae Authors: Berger, T. E.; Rouppe van der Voort, L.; Lofdahl, M. G. Bibcode: 2005AGUSMSP31A..02B Altcode: We present new images of magnetic elements near the solar limb ("faculae") along with magnetogram measurements and contrast profiles. Imaging magnetogram observations were made of AR 10377 at μ = cosθ = 0.6 on 06-June-2003 using the Swedish 1-m Solar Telescope; the data are the highest spatial resolution magnetogram measurements of faculae to date. Contrary to previous lower resolution measurements, we find no correlation between facular contrast and magnetic flux density at a given disk position. Increasing magnetic flux density in a region implies an increasing prevalence of micropores. Previous observations which lacked sufficient spatial resolution to discern dark micropore "floors" from bright facular walls find a strong non-linear dependence of facular contrast on magnetic flux density, with decreasing contrast beyond a certain flux density. We show instead that the observed contrast of bright facular walls is independent of magnetic flux density when properly segmented from dark micropores. The observations are useful for examining the detailed structure of faculae including the dark lanes found on the disk-center side of many faculae (explained by several recent 3D MHD numerical simulations). The average radial profile for 678 faculae segmented from the dataset is very nearly gaussian with a FWHM radial extent of 265 km and an extended tail on the limbward side, as predicted by current MHD simulations. Title: First-Light Instrumentation for the Advanced Technology Solar Telescope Authors: Rimmele, T.; Balasubramaniam, K.; Berger, T.; Elmore, D.; Gary, A.; Keller, C.; Kuhn, J.; Lin, H.; Mickey, D.; Pevtsov, A.; Robinson, B.; Sigwarth, M.; Soccas-Navarro, H. Bibcode: 2005AGUSMSP34A..03R Altcode: The 4m Advanced Technology Solar Telescope (ATST) is the next generation ground based solar telescope. In this paper we provide an overview of the ATST post-focus instrumentation. The majority of ATST instrumentation is located in an instrument Coude lab facility, where a rotating platform provides image de-rotation. A high order adaptive optics system delivers a corrected beam to the Coude lab facility. Alternatively, instruments can be mounted at the Nasmyth focus. For example, instruments for observing the faint corona preferably will be mounted at Nasmyth where maximum throughput is achieved. In addition, the Nasmyth focus has minimum telescope polarization and minimum stray light. We give an overview of the initial set of first generation instruments: the Visible-Light Broadband Imager (VLBI), the Visible Spectro-Polarimeter (ViSP), the Near-IR Spectro-Polarimeter (NIRSP), which includes a coronal module, and the Visible Tunable Filter. We also discuss the unique and efficient approach to the ATST instrumentation, which builds on the use of common components such as detector systems, polarimetry packages and various opto-mechanical components. For example, the science requirement for polarimetric sensitivity (10-5 relative to intensity) and accuracy (5'10-4 relative to intensity) place strong constraints on the polarization analysis and calibration units. Consequently, these systems are provided at the facility level, rather than making it part of the requirement for each instrument. Title: Solar Magnetic Flux as a Function of Disk Position over the Solar Cycle Authors: Berger, T. Bibcode: 2005AGUSMSP41B..07B Altcode: A novel analysis of a SOHO/MDI full-disk magnetogram time series from March 1996 to November 2004 is presented. Each of the 26,052 magnetograms in the series are segmented into sectors of constant μ = cos θ, each sector having a width of Δμ = 0.05. Within each sector, a histogram of signed magnetic flux density, corrected for the line-of-sight angle θ, is compiled. For each magnetogram we thus obtain a distribution of signed magnetic flux density as a function of μ. Summing the signed flux in each μ bin gives the total signed flux as a function of μ. Plotting these totals for each μ-sector as a function of time over the course of Solar Cycle 22 reveals that cycle minimum and maximum are differentiated only by the magnitude of the flux distributions. In other words, in contrast to analogous plots of flux versus heliocentric latitude, there is no discernible pattern, or "Butterfly Diagram", of flux seen on the solar disk from Earth. The finding is relevant to investigations of total solar irradiance (TSI) since it is known that the primary cause of the ~ 0.1% TSI variation over the solar cycle is the distribution of non-sunspot magnetic flux at smaller μ-values (so-called "faculae"). Title: Solar magnetic elements at 0.1 arcsec resolution. II. Dynamical evolution Authors: Rouppe van der Voort, L. H. M.; Hansteen, V. H.; Carlsson, M.; Fossum, A.; Marthinussen, E.; van Noort, M. J.; Berger, T. E. Bibcode: 2005A&A...435..327R Altcode: Small magnetic structures can be seen in G-band filtergrams as isolated bright points, strings of bright points and dark micro-pores. At a resolution of 0.1 arcsec, new forms of magnetic structures are found in strong field areas: elongated “ribbons” and more circular “flowers”. In this paper we study the temporal evolution of these small scale magnetic structures. In strong-field regions the time-evolution is more that of a magnetic fluid than that of collections of flux-tubes that keep their identity. We find that the granular flow concentrates the magnetic field into flux sheets that are visible as thin bright features in the filtergrams. Weak upflows are found in the flux sheets and downflows in the immediate surroundings. The flux sheets often become unstable to a fluting instability and the edges buckle. The sheets tend to break up into strings of bright points, still with weak upflows in the magnetic elements and zero velocity or downflows between them. Where there are larger flux concentrations we find ribbons, flowers and micro-pores. There is a continuous transition between these forms and they evolve from one form to another. The appearance is mostly determined by the horizontal size - larger structures are dark (micro-pores), narrower structures are ribbon shaped and the flowers are the smallest in extent. All these structures have darker inner parts and a bright edge. The plasma is found to be at rest in the ribbons, with small concentrations of weak upflow sites. Narrow sheets with downdrafts are found right at the edges of the magnetic field concentrations. Title: Thin Threads of Solar Filaments Authors: Lin, Yong; Engvold, OddbjØrn; der Voort, Luc Rouppe van; Wiik, Jun Elin; Berger, Thomas E. Bibcode: 2005SoPh..226..239L Altcode: High-resolution images obtained in Hα with the new Swedish Solar Telescope at La Palma, Spain, have been used for studies of fine-scale threads in solar filaments. The widths of the thin threads are ≤0.3 arcsec. The fact that the width of the thinnest threads is comparable to the diffraction limit of the telescope of about 0.14 arcsec, at the wavelength of Hα, suggests that even thinner threads may exist. Assuming that the threads represent thin magnetic strings, we conclude that only a small fraction of these are filled with observable absorbing plasma, at a given time. The absorbing plasma is continuously flowing along the thread structures at velocities 15± 10 kms−1, which suggests that the flows must be field-aligned. In one case where a bundle of thin threads appears to be rooted in the nearby photosphere, we find that the individual threads connects with intergranular, dark lanes in the photosphere. We do not find signs of typical network fields at the `roots' of the fine threads, as normally evidenced by bright points in associated G-band images. It is suggested that filament threads are rooted in relatively weak magnetic fields. Title: Solar magnetic elements at 0.1 arcsec resolution. General appearance and magnetic structure Authors: Berger, T. E.; Rouppe van der Voort, L. H. M.; Löfdahl, M. G.; Carlsson, M.; Fossum, A.; Hansteen, V. H.; Marthinussen, E.; Title, A.; Scharmer, G. Bibcode: 2004A&A...428..613B Altcode: New observations of solar magnetic elements in a remnant active region plage near disk center are presented. The observations were obtained at the recently commissioned Swedish 1-m Solar Telescope on La Palma. We examine a single 430.5 nm G-band filtergram that resolves ∼70 km (0.1 arcsec) structures and find new forms of magnetic structures in this particular region. A cotemporal Ca II H-line image is used to examine the low-chromosphere of network elements. A cotemporal Fe I 630.25 nm magnetogram that resolves structures as small as 120 km (0.18 arcsec) FWHM with a flux sensitivity of approximately 130 Mx cm-2 quantifies the magnetic structure of the region. A Ni I 676.8 nm Dopplergram establishes relative velocity patterns associated with the network features with an accuracy of about 300 m s-1. We find that magnetic flux in this region as seen in both the magnetogram and the G-band image is typically structured into larger, amorphous, ``ribbons'' which are not resolved into individual flux tubes. The measured magnetic flux density in the ribbon structures ranges from 300 to 1500 Mx cm-2, the higher values occurring at localized concentrations embedded within the ribbons. The Dopplergram indicates relative downflows associated with all magnetic elements with some indication that higher downflows occur adjacent to the peak magnetic flux location. The mean absolute magnetic flux density of the remnant plage network is about 130 Mx cm-2; in the lowest flux regions of the field-of-view, the mean absolute flux density is approximately 60 Mx cm-2. Within these quiet regions we do not find evidence of pervasive kilo-gauss strength magnetic elements as seen in recent high resolution internetwork studies. In general, the observations confirm recent 3-dimensional numerical simulations which show that the magnetic field in high-density regions such as plage is concentrated in complex structures that are not generally composed of discrete magnetic flux tubes.

Appendices are only available in electronic form at http://www.edpsciences.org Title: Recent Progress in High-Resolution Observations Authors: Berger, T. E.; Title, A. M. Bibcode: 2004ASPC..325...95B Altcode: We review recent optical observations of the solar photosphere and chromosphere with an emphasis on those observations that attain spatial resolution values below 0.25 arcsec. Results from the Dutch Open Telescope (DOT) on La Palma, the Dunn Solar Telescope (DST) on Sacramento Peak, and the Vacuum Tower Telescope (VTT) on Tenerife are reviewed. Particular emphasis is placed on results from the newly commissioned Swedish 1-meter Solar Telescope (SST) on La Palma following our successful campaigns at this instrument in 2002 and 2003. The SST with adaptive optics can now achieve 0.0 arcsec resolution imaging of the Sun in multiple simultaneous wavelengths. Scientific findings on the structure of sunspot penumbrae and lightbridges, small-scale magnetic elements, and faculae at the limb are reviewed. The Lockheed Solar Optical Universal Polarimeter (SOUP) birefringent tunable filter at the SST produced 0.16 arcsec resolution magnetograms in the summer of 2003 that have shed new light on the structure and dynamics of small-scale magnetic fields in the solar photosphere. Title: Instrumentation for the Advanced Technology Solar Telescope Authors: Rimmele, Thomas R.; Hubbard, Robert P.; Balasubramaniam, K. S.; Berger, Tom; Elmore, David; Gary, G. Allen; Jennings, Don; Keller, Christoph; Kuhn, Jeff; Lin, Haosheng; Mickey, Don; Moretto, Gilberto; Socas-Navarro, Hector; Stenflo, Jan O.; Wang, Haimin Bibcode: 2004SPIE.5492..944R Altcode: The 4-m aperture Advanced Technology Solar Telescope (ATST) is the next generation ground based solar telescope. In this paper we provide an overview of the ATST post-focus instrumentation. The majority of ATST instrumentation is located in an instrument Coude lab facility, where a rotating platform provides image de-rotation. A high order adaptive optics system delivers a corrected beam to the Coude lab facility. Alternatively, instruments can be mounted at Nasmyth or a small Gregorian area. For example, instruments for observing the faint corona preferably will be mounted at Nasmyth focus where maximum throughput is achieved. In addition, the Nasmyth focus has minimum telescope polarization and minimum stray light. We describe the set of first generation instruments, which include a Visible-Light Broadband Imager (VLBI), Visible and Near-Infrared (NIR) Spectropolarimeters, Visible and NIR Tunable Filters, a Thermal-Infrared Polarimeter & Spectrometer and a UV-Polarimeter. We also discuss unique and efficient approaches to the ATST instrumentation, which builds on the use of common components such as detector systems, polarimetry packages and various opto-mechanical components. Title: Three-Dimensional Structure of the Active Region Photosphere as Revealed by High Angular Resolution Authors: Lites, B. W.; Scharmer, G. B.; Berger, T. E.; Title, A. M. Bibcode: 2004SoPh..221...65L Altcode: Blue continuum images of active regions at ∼ 60° from the center of the solar disk obtained with the new Swedish 1-m Solar Telescope reveal heretofore unreported structure of the magnetized solar atmosphere. Perhaps the most striking aspect of these images is that, at an angular resolution of 0.12″, they show clearly the three-dimensional structure of the photosphere. In particular, the Wilson depression of the dark floors of pores is readily apparent. Conversely, the segmented structure of light bridges running through sunspots and pores reveal that light bridges are raised above the dark surroundings. The geometry of light bridges permits estimates of the height of their central (slightly darker) ridge: typically in the range 200-450 km. These images also clearly show that facular brightenings outside of sunspots and pores occur on the disk-center side of those granules just limbward of intergranular lanes that presumably harbor the associated plage magnetic flux. In many cases the brightening extends 0.5″ or more over those granules. Furthermore, a very thin, darker lane is often found just centerward of the facular brightening. We speculate that this feature is the signature of cool down flows that surround flux tubes in dynamical models. These newly recognized observational aspects of photospheric magnetic fields should provide valuable constraints for MHD models of the magnetized photosphere, and examination of those models as viewed from oblique angles is encouraged. Title: Observations of solar magnetic elements with 0.1" resolution Authors: Berger, T. E.; Rouppe van der Voort, L. H. M.; Lofdahl, M. G.; Carlsson, M.; Fossum, A.; Hansteen, V. H.; Marthinussen, E.; Title, A. M.; Scharmer, G. Bibcode: 2004AAS...204.2005B Altcode: 2004BAAS...36..686B New observations of solar magnetic elements in a remnant active region plage near disk center are presented. The observations were taken with the Swedish 1-meter Solar Telescope on La Palma. We examine a single 430.5 nm G-band filtergram that resolves ∼70 km (0.''1) structures and find new forms of magnetic structures in this particular region. A simultaneous Ca II H-line image is used to examine the low-chromosphere of network elements. A simultaneous Fe I 630.25 nm magnetogram that resolves structures as small as 120 km (0.''18) FWHM with a flux sensitivity of approximately 130 Mx cm-2 quantifies the magnetic structure of the region. A Ni I 676.8 nm Dopplergram establishes relative velocity patterns associated with the network features with an accuracy of about 300 m s-1. Magnetic flux in this region as seen in both the magnetogram and the G-band image is typically structured into larger, amorphous, ``ribbons'' with a wide range of flux density values, rather than isolated kilogauss flux tubes. We also present filtergrams and magnetograms of magnetic elements at the solar limb showing that solar faculae are resolved into bright granular walls that appear to project 350 to 500 km above the photosphere. Title: Austrian dose measurements onboard space station MIR and the International Space Station - overview and comparison Authors: Berger, T.; Hajek, M.; Summerer, L.; Vana, N.; Akatov, Y.; Shurshakov, V.; Arkhangelsky, V. Bibcode: 2004AdSpR..34.1414B Altcode: The Atominstitute of the Austrian Universities has conducted various space research missions in the last 12 years in cooperation with the Institute for Biomedical Problems in Moscow. They dealt with the exact determination of the radiation hazards for cosmonauts and the development of precise measurement devices. Special emphasis will be laid on the last experiment on space station MIR the goal of which was the determination of the depth distribution of absorbed dose and dose equivalent in a water filled Phantom. The first results from dose measurements onboard the International Space Station (ISS) will also be discussed. The spherical Phantom with a diameter of 35 cm was developed at the Institute for Biomedical Problems and had 4 channels where dosemeters can be exposed in different depths. The exposure period covered the timeframe from May 1997 to February 1999. Thermoluminescent dosemeters (TLDs) were exposed inside the Phantom, either parallel or perpendicular to the hull of the spacecraft. For the evaluation of the linear energy transfer (LET), the high temperature ratio (HTR) method was applied. Based on this method a mean quality factor and, subsequently, the dose equivalent is calculated according to the Q(LET ) relationship proposed in ICRP 26. An increased contribution of neutrons could be detected inside the Phantom. However the total dose equivalent did not increase over the depth of the Phantom. As the first Austrian measurements on the ISS dosemeter packages were exposed for 248 days, starting in February 2001 at six different locations onboard the ISS. The Austrian dosemeter sets for this first exposure on the ISS contained five different kinds of passive thermoluminescent dosemeters. First results showed a position dependent absorbed dose rate at the ISS. Title: Comparison of various techniques for the exact determination of absorbed dose in heavy ion fields using passive detectors Authors: Berger, T.; Reitz, G.; Hajek, M.; Vana, N. Bibcode: 2004cosp...35.4425B Altcode: 2004cosp.meet.4425B Passive thermoluminescent detectors (TLDs) are commonly applied for the determination of absorbed dose in routine radiation protection. The usage of TLDs in heavy ion fields, e.g. for treatment planing in radiotherapy or in space dosimetry, requires the detailed knowledge of the efficiency of these detectors to the ion under study in dependence on the LET of the ion. This is due to the fact, that the detection efficiency of TLDs changes with increasing LET. This would lead - if the changing efficiency of the TL- material is not taken into account - to a measured deviation of the absorbed dose. In the framework of the ICCHIBAN project - which was started as an intercomparison of passive and active detector systems used for dose determination in space - "Blind" exposures were carried out. No information about dose and ion species was given for the investigators. Three different methods were used for the efficiency correction of TLDs after the BLIND exposures. The first method used the different LET efficiency of the TL-materials LiF: Mg, Ti and LiF:Mg, Cu,P to determine the LET and based on this value the efficiency of the LiF: Mg, Ti dosemeters. The second method used the high temperature emissions in LiF: Mg, Ti for the efficiency correction. The third method applied used a combination of TLDs and CR-39 track etch detectors to determine the total absorbed dose during the BLIND exposures. The paper will discuss the threee methods, and focus on the applicability for the usage of these methods for dose determination and recalculation in space dosimetry. Title: BRADOS - Dose determination in the Russian segment of the International Space Station Authors: Hajek, M.; Berger, T.; Fürstner, M.; Fugger, M.; Vana, N.; Akatov, Y.; Shurshakov, V.; Arkhangelsky, V. Bibcode: 2004cosp...35.1950H Altcode: 2004cosp.meet.1950H Absorbed dose and dose-average linear energy transfer (LET) were assessed by means of LiF: Mg, Ti thermoluminescence (TL) detectors at different locations onboard the Russian segment (RS) of the International Space Station (ISS) in the timeframe between February and November 2001, i.e. for 248 days. Based on calibrations of the employed detectors in a variety of heavy-ion beams, mainly at the Heavy Ion Medical Accelerator (HIMAC) in Chiba, Japan, the measured absorbed dose values could be corrected for the TL dose registration efficiency in the radiation climate onboard the ISS. Various strategies for efficiency correction are discussed. For the specific case the efficiency correction accounted for a reduction by nearly 20 % in dose, implying that without proper consideration of the TL efficiency behaviour the absorbed dose inside the ISS would be overestimated. The dose-average LET was derived from TLD-700 measurements evaluated according to the well-established high-temperature ratio (HTR) method which analyzes the TL emission in the temperature range between 248 and 310 C. According to the shielding distribution, the efficiency-corrected absorbed dose was found to vary between 155 μ Gy/d for panel N 457 (RS-ISS toilet) and 230 μ Gy/d for panel N 443 (RS-ISS starboard cabin). The determined LET indicated a modification of the spectral composition of the onboard radiation field for the different exposure locations. Arrangement of TLD-600 and TLD-700 in pair allowed also some information about the neutron component to be drawn. Experimentally determined absorbed dose values are compared with model calculations by means of a self-developed code, using as input data detailed shielding distributions and proton fluxes from AP-8 and JPL algorithms. Title: A study of the causal relationship between the emergence of a twisted magnetic flux rope and a small Hα two-ribbon flare Authors: Brooks, D. H.; Kurokawa, H.; Yoshimura, K.; Kozu, H.; Berger, T. E. Bibcode: 2003A&A...411..273B Altcode: We present results from an analysis of a small two-ribbon flare which occurred above emerging flux in solar active region NOAA 8218 on 1998, May 13th and which was observed by the Swedish Vacuum Solar Telescope (SVST) on the island of La Palma, Spain. The relatively simple magnetic morphology and small size of the flare together with the high quality of the SVST observations allow us to examine the essential properties of flares in emerging flux regions in greater detail than before.

In this paper we compare and contrast the flaring emerging flux region simultaneously with a non-flaring emerging flux region within the same field of view. Unusual magnetic footpoint motions are observed in the flaring region, coincident with the Hα kernels, which result in a high level of shearing of the magnetic neutral line between opposite polarities. The Hα images show dark filament structures which form an inverted S-like shape immediately prior to the flare and then separate after the energy release disrupts the magnetic field. We interpret the motions and structures as strong evidence for the emergence of a twisted magnetic flux rope which developed a sheared configuration with the overlying magnetic field. In contrast the companion region shows separating footpoints, with apparent arch-like filament connections in the Hα images, consistent with the expected appearance of emerging flux. The observations imply that the attachment of the inverted S-shaped structure may be an observational consequence of the magnetic reconnection or untwisting of the field which triggered the flare. We also find some evidence that the increase in magnetic flux is faster in the flaring region.

Finally, we propose a simple schematic model of the emergence of a twisted magnetic flux rope and attached branch which can account for the observed footpoint motions and Hα structures of the flaring region. Such a model can, in principle, induce partial magnetic reconnection in the overlying coronal field and we found some evidence of coronal loop footpoint brightenings which support our conclusions. Our high resolution study supports the results of previous authors that even a small twisted structure in an emerging flux tube can be important for flare production. Title: Influence of Photospheric Magnetic Fields and Dynamics on Chromospheric K-Line Emission Authors: Lawrence, J. K.; Cadavid, A. C.; Miccolis, D.; Berger, T. E.; Ruzmaikin, A. Bibcode: 2003ApJ...597.1178L Altcode: We analyze a 9 hr sequence of simultaneous, high-resolution, high-cadence G-band and K-line solar filtergrams plus magnetograms of lower cadence and resolution. Images include both network and internetwork. The magnetic and filtergram intensities, their fluctuations, and relative phases change with progressive strengthening of local magnetic field. At increased flux levels, sudden photospheric downflows create long-lived magnetic elements. For weak magnetic fields the K-line and G-band intensities include an oscillatory component with period 4 minutes. For stronger fields, the K-line period shifts to 5 minutes, while the G-band fluctuations fade due to dissociation of their source, the CH radical. These K-line and G-band fluctuations, whose periods are longer than the acoustic cutoff, are coherent and in phase. They also are coherent with fluctuations of the magnetic field. Weak-field magnetic fluctuations lead the intensity fluctuations by a phase shift of 90°. Strong-field magnetic fluctuations trail the intensities by 100°. These are interpreted as standing waves in the photosphere and low chromosphere. Another class of G-band fluctuations, with periods shorter than the acoustic cutoff, is associated both with stronger magnetic fields and with enhanced K-line emission with fluctuations longer than the cutoff period. This suggests waves excited by rapid photospheric perturbations and propagating up along magnetic flux tubes. Title: Future Capabilities for Solar/Stellar Observations Authors: Carpenter, K.; Hassler, D.; Berger, T.; Bastian, T.; Pallavicini, R.; Balachandran, S. Bibcode: 2003csss...12..359C Altcode: This session outlines the potential instrumental capabilities for the observation of cool stars and the Sun. The individual contributions cover space-based solar missions (Hassler), ground-based solar optical/IR instruments (Berger), solar-stellar radio capabilities (Bastian), space-based stellar missions (Carpenter), ground-based optical (Pallavicini) and infrared facilities (Balachandran) for stellar observations. Title: The Observation of Sunspot Light-Bridge Structure and Dynamics Authors: Berger, T. E.; Berdyugina, S. V. Bibcode: 2003ApJ...589L.117B Altcode: We present very high resolution multiwavelength images of a sunspot light bridge in NOAA Active Region 10132 taken at the Swedish 1 m Solar Telescope on La Palma on 2002 September 25. The adaptive optics-corrected images resolve 100 km scale bright grains on either side of an approximately 380 km dark lane in the center of the bridge. Movies of the data show the grains in a steady unidirectional flow with an average speed of 900 m s-1 along the entire length of the bridge. Overturning motions are seen in the larger grains, suggesting a convective origin for these structures. Simultaneous 160 nm ultraviolet images from the Transition Region and Coronal Explorer (TRACE) satellite show a constant brightness enhancement over the light bridge, implying a steady chromospheric heat source. TRACE 160 nm movies do not resolve the unidirectional flow; instead, they suggest that a horizontal oscillatory motion exists in the chromosphere of the light bridge. A C2.0 flare at 16:00 UT, one ribbon of which occurs directly along the light bridge, indicates a high level of magnetic stress and impulsive dissipation associated with the observed light-bridge dynamics. Title: Influence of Photospheric Magnetism and Dynamics on Chromospheric K-line Emission Authors: Lawrence, J. K.; Cadavid, A. C.; Miccolis, D.; Berger, T. E.; Ruzmaikin, A. Bibcode: 2003SPD....34.0704L Altcode: 2003BAAS...35..820L We analyze a unique 9 hr sequence of near simultaneous, high resolution and high cadence G-band and K-line SVST solar filtergrams together with magnetograms of lower cadence and resolution. We focus on a region of the solar surface that includes both internetwork and network. We examine how the (temperature minimum/chromospheric) CaII K-line and (photospheric) G-band intensities, their temporal fluctuations and their coherence and phase relations, with each other and with magnetic fluctuations, change as we progress from weak magnetic fields (internetwork) to intermediate and strong fields (network).

As the background level of flux is increased, sudden photospheric downflow events can create long-lived, compact (i.e. network) magnetic elements. For weak magnetic fields the K-line and G-band intensity signals show an oscillatory component with period centered on 4 min. As we pass to strong fields, the K-line signal shifts to a 5 min period while the G-band signal fades, presumably due to dissociation of the CH radical. The K-line and G-band signals are coherent and nearly in-phase. They are both coherent with fluctuations of the magnetic field. For weak field the magnetic signal leads the intensity signals by 90o in phase. For intermediate and strong fields the magnetic signal trails the intensities by 110o. We interpret this as a transition from acoustic standing waves with weak, passive magnetic field to a slow mode trapped magnetoacoustic wave. For intermediate magnetic field we find, in addition to the coherent waves, that G-band fluctuations at frequencies above the acoustic cutoff (period < 3.5 min) are associated with magnetic fields and with K-line emission at periods > 3.5 min. This suggests the presence of flux tube waves excited by rapid photospheric perturbations.

This work was supported by grants NSF-ATM 9987305 and NASA-NAG5-10880. The SVST is operated by the Swedish Royal Academy of Sciences at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Title: Observations of magnetoconvection in Sunspots with 100 km resolution Authors: Berger, T. E.; Löfdahl, M. G.; Scharmer, G.; Title, A. M. Bibcode: 2003SPD....34.1108B Altcode: 2003BAAS...35..828B We present new observations from the Swedish 1-meter Solar Telescope (SST) on La Palma with ∼0.1 arcsecond ( ∼100 km) resolution: the highest resolution yet achieved in solar observations. We focus on sunspot and active region magnetoconvective phenomena using G-band 4305 Å, 4877 Å continuum, 7507 Å TiO bandhead, and Ca II 3968 Å H-line filtergram movies. The G-band data are post-processed using Joint Phase Diverse Speckle wavefront restoration to create a full diffraction limited time series. Sunspot light-bridges are shown to have dark lanes less than 300 km in width that are coherent along the entire length of the bridge. Similarly, we find elongated dark ``canals'' in plage regions, particularly near pores, that appear to be highly modified intergranular downflow lanes. The canals are less than 200 km in width and are much more coherent than intergranular lanes in non-magnetic regions, often retaining their basic structure for more than one granular turn-over time. Both the light-bridge central lane and the canals appear to be the result of highly constrained flow structure in strong magnetic field regions -- an aspect of solar magnetoconvection that has not previously been observed. This reseach was supported by funding from the Royal Swedish Academy of Sciences, a SOHO Guest Investigator subcontract to California State University Northridge, and the NASA TRACE contract NAS5-38099 at Lockheed Martin. Title: Photospheric Sources of Chromospheric Dynamics in the Internetwork Authors: Cadavid, A. C.; Lawrence, J. K.; Berger, T. E.; Ruzmaikin, A. Bibcode: 2003SPD....34.0703C Altcode: 2003BAAS...35..820C We analyze a unique 9 hr sequence of near simultaneous, high resolution and high cadence G-band and K-line solar filtergrams together with magnetograms of lower cadence and resolution, taken with the SVST. We investigate an internetwork region characterized by magnetic fields with strength < 150 Gauss and focus on the phenomena surrounding discrete photospheric darkening ``events'' in G-band intensities. 72 % of the darkenings are followed after 2 min by K-line brightenings. In the remaining cases the darkenings are instead preceded by K-line brightenings 2 min earlier. In both cases the preceding and following G-band minima are each associated with transient magnetic enhancements, and thus, presumably, photospheric inflows followed by outflows. The magnetic field appears to have no role in coupling the photospheric phenomena to the chromosphere, and acts as a passive tracer of horizontal photospheric flows that converge on the photospheric darkening events and then rebound. The timing and coupling of the photospheric darkenings and chromospheric brightenings appear to be regulated by a pre-existing 4 min oscillation of the solar atmosphere. Other oscillations with periods in the range 1-8 min also are present, and in general the wave power is doubled at the time of an event. At short periods temporal structure is resolved. Our results favor an acoustic source for enhanced amplitudes of K-line intensity oscillations. Title: Weak-Field Magnetogram Calibration using Advanced Stokes Polarimeter Flux Density Maps - II. SOHO/MDI Full-Disk Mode Calibration Authors: Berger, T. E.; Lites, B. W. Bibcode: 2003SoPh..213..213B Altcode: Cotemporal Ni i 676.8 nm full-disk magnetograms from the Michelson Doppler Interferometer (MDI) instrument on SOHO and the Advanced Stokes Polarimeter (ASP) are quantitatively compared using observations of active region AR 8218, a large negative polarity sunspot group observed at S20 W22 on 13 May 1998. MDI produces flux density estimates based on a polarized line center-of-gravity algorithm using moderate spectral resolution filtergrams with approximately 4 arc sec angular resolution. The magnetograms are formed by an on-board image processor and sent to the ground where they are calibrated using an empirical model to produce flux density maps. The ASP uses high spectral resolution Stokes polarimetric observations to produce very high precision vector magnetic field maps at angular resolution values on the order of 1 arc sec in good seeing. We use ASP inversion results to create a reference ASP `longitudinal magnetic flux density map' with which to calibrate the MDI full-disk magnetograms. The magnetograms from each instrument are scaled to a common reference frame and co-aligned with an accuracy of about 1.6 arc sec. Regions of invalid data, poor field-of-view overlap, and sunspots are masked out in order to calibrate MDI predominately on the relatively vertical `weak-field' plage magnetic elements. Pixel-to-pixel statistical comparisons are used to determine an MDI magnetogram linear calibration relative to reference ASP flux density values. We find that the current Level-1.5 MDI full-disk calibration gives flux density values lower on average by a factor of 0.64±0.013 compared to the ASP reference in active region plage. In sunspot regions (penumbra and umbra) the factor is 0.69±0.007. Title: Photospheric Sources and Brightening of the Internetwork Chromosphere Authors: Cadavid, A. C.; Lawrence, J. K.; Berger, T. E.; Ruzmaikin, A. Bibcode: 2003ApJ...586.1409C Altcode: We analyze a unique 9 hr sequence of near-simultaneous, high-resolution and high-cadence G-band and K-line solar filtergrams, together with magnetograms of lower cadence and resolution. Our focus is on the phenomena surrounding discrete photospheric darkening ``events'' in internetwork G-band intensities. 72% of the darkenings are followed after 2 minutes by K-line brightenings. In the remaining cases, the darkenings are instead preceded by K-line brightenings 2 minutes earlier. Equivalent results are found when reference is shifted to K-line brightening events, although these two sets overlap by no more than 15%. The timing and coupling of the photospheric darkenings and chromospheric brightenings appear to be regulated by a preexisting 4 minute oscillation of the solar atmosphere. Other oscillations with periods in the range 1-8 minutes also are present, and in general the wave power is doubled at the time of an event. Our results favor an acoustic source for enhanced amplitudes of K-line intensity oscillations. The magnetic field acts as a passive tracer of horizontal photospheric flows that converge on the photospheric darkening events and then rebound. Title: Intensity tracers of the magnetic field: pitfalls and opportunities Authors: Lites, B. W.; Berger, T. E. Bibcode: 2002ESASP.505...57L Altcode: 2002solm.conf...57L; 2002IAUCo.188...57L Magnetic fields are the main source of structuring of the solar atmosphere. Stokes I images at various wavelengths reflect this structure at the monochromatic heights of formation of the intensity. In the photosphere intensity tracers identify the location and evolution of kiloGauss flux tubes. In the chromosphere and above Stokes I images may be used to identify the direction of the magnetic lines of force, and may be used to establish the connectivity of the field inferred from photospheric vector magnetograms. In some circumstances the intensity diagnostics of the field may be misleading. Some of these "pitfalls" are discussed. Title: Weak-Field Magnetogram Calibration using Advanced Stokes Polarimeter Flux-Density Maps - I. Solar Optical Universal Polarimeter Calibration Authors: Berger, T. E.; Lites, B. W. Bibcode: 2002SoPh..208..181B Altcode: Cotemporal Fe i 630.2 nm magnetograms from the Solar Optical Universal Polarimeter (SOUP) filter and the Advanced Stokes Polarimeter (ASP) are quantitatively compared using observations of active region AR 8218, a large negative polarity sunspot group observed at S20 W22 on 13 May 1998. The SOUP instrument produces Stokes V/I `filter magnetograms' with wide field of view and spatial resolution below 0.5 arc sec in good seeing, but low spectral resolution. In contrast, the ASP uses high spectral resolution to produce very high-precision vector magnetic field maps at spatial resolution values on the order of 1 arc sec in good seeing. We use ASP inversion results to create an ASP `longitudinal magnetic flux-density map' with which to calibrate the less precise SOUP magnetograms. The magnetograms from each instrument are co-aligned with an accuracy of about 1 arc sec. Regions of invalid data, poor field-of-view overlap, and sunspots are masked out in order to calibrate SOUP predominately on the relatively vertical `weak-field' plage magnetic elements. Pixel-to-pixel statistical comparisons are used to determine the SOUP magnetogram linear calibration constant relative to ASP flux-density values. We compare three distinct methods of scaling the ASP and SOUP data to a common reference frame in order to explore filling factor effects. The recommended SOUP calibration constant is 17 000 ± 550 Mx cm−2 per polarization percent in plage regions. We find a distinct polarity asymmetry in SOUP response relative to the ASP, apparently due to a spatial resolution effect in the ASP data: the smaller, less numerous, minority polarity structures in the plage region are preferentially blended with the majority polarity structures. The blending occurs to a lesser degree in the high-resolution SOUP magnetogram thus leading to an apparent increase in SOUP sensitivity to the minority polarity structures relative to the ASP. One implication of this effect is that in mixed polarity regions on the Sun, lower spatial resolution magnetograms may significantly underestimate minority polarity flux levels, thus leading to apparent flux imbalances in the data. Title: Observation and Modelling of Micropore Formation in Active Network Regions Authors: Berger, T. E.; Löfdahl, M. G.; Bercik, D. J. Bibcode: 2002AAS...200.9101B Altcode: 2002BAAS...34Q.953B We present phase-diversity corrected G-band 4305 Å and 4364 Å continuum image time series showing the formation of a micropore in a small active region near disk center. The data were acquired at the Swedish Vacuum Solar Telescope on La Palma in June of 1997 and post-processed using the Phase Diverse Speckle (PDS) algorithm to produce diffraction limited images throughout the majority of both time series. The micropore dataset comprises a 29x29 Mm field of view and spans 5.1 hours with a 38 second cadence. The micropore forms in a strong sink area that can be seen to ``collect" many G-band bright points over the first 2 hours of the observation. During this time there is an occasional darkening at the sink point that may be the first unstable phase of the micropore formation. Once a stable dark pore forms in the flowfield, it grows to a maximum diameter of 1.2 Mm in approximately 1.9 hours. The pore persists for another 35 minutes before apparently being broken up by the intergranular flowfield. The total ``lifetime" of the stable pore phase is 2.5 hours. A separate nearby micropore of 1.5 Mm maximum diameter exists for the entire 5.2 hour data span. We show G-band and continuum movies of the micropore formation, correlation tracking flowfield analyses, G-band bright point tracking results, and area versus time plots for the micropore formation lifetime. The observational data are compared with fully compressible 3D MHD numerical simulations which show the development of a similar micropore structure within the computational domain. This research was supported by NASA SR&T grant NASW-98008, The Royal Swedish Academy of Sciences, NSF and NASA funding at Michigan State University, and Lockheed Martin IRAD funding. Title: Mesogranulation from Principal Component Analysis of SVST Photospheric Continuum Images Authors: Bell, E.; Cadavid, A. C.; Lawrence, J. K.; Berger, T. E. Bibcode: 2002AAS...200.3805B Altcode: 2002BAAS...34Q.699B We analyze a sequence of 279 images of the photosphere made with the Swedish Vacuum Solar Telescope on 1997 June 11. The sequence spans 3 hr with cadence 38 s. The images were taken in continuum near 4364 Å, and underwent phase diversity reconstruction. Resolution is ~ 0.2 Mm and field of view 32 X 32 Mm. We carried out a principal component analysis on sequences of 15 images spaced 6 min apart and covering 1.5 hr. The 15 X 15 correlation matrix of each such set of images was diagonalized, giving 15 eigenimages which are linear combinations of the original 15. The eigenimage corresponding to the largest eigenvalue is the linear combination that best resembles the original set as a whole; those with smaller and smaller eigenvalues resemble the overall set less and less well. Fourier spectra of the eigenimages were calculated separately for several sequences and then averaged together to reduce uncertainties. Fourier analysis of the leading eigenimage reveals structure at two scales: one for λ =1/ν ~ 1.5 Mm corresponding to granulation and another for λ ~ 4.5 Mm. Because of their scale and because the time span of the sets lies between the lifetimes of granules and mesogranules, we interpret the latter as mesogranules. The subsequent eigenimages do not show the larger structure, but show the granular peak at successively smaller scales. This indicates a spatio-temporal scaling of the granulation with shorter lifetimes for smaller features. For comparison purposes, simulated granulation images (Cattaneo, Lenz and Weiss 2001) were similarly analyzed and give similar results. Work supported in part by grants NSF-ATM-9987305, NASA-NAG5-10880 and the NASA CSUN/JPL PAIR Program. F. Cattaneo, D. Lenz and N. Weiss 2001, ApJ, 563, L91. Title: High Resolution Spatio-Temporal Study of Photospheric and Chromospheric Energetics Authors: Cadavid, A. C.; Lawrence, J. K.; Berger, T. E. Bibcode: 2002AAS...200.3809C Altcode: 2002BAAS...34..700C We study the photosphere/chromosphere energetic connection using a nine hour sequence of SVST images obtained May 30, 1998. The data consist of co-spatial, nearly simultaneous filtergrams of G-band (4305 Å ), Ca II K (3934 Å ), two (6563 Å) Hα channels offset by 0.35 Å and 0.7 Å , and Fe I (6302 Å) magnetograms. The cadence of the G-band and Ca K observations is ~ 30 s; that of the other images is ~ 2 min. The pixel scale is 0.06 Mm and field of view 48 X 48 Mm on the Sun. The filtergram resolution is > 0.2 Mm; that of the magnetograms > 0.3 Mm with single magnetogram sensitivity < 150 G. We have co-registered the images to 1 or 2 pixel accuracy. The number distribution of Ca brightenings and of localized changes in magnetic field strength, measured in standard deviations (σ ) from the image means, present three different characteristic regimes; that of the magnetic ``free energy'' (a derived measure based on the local variance of magnetic field) presents two. Ca brightenings below 3σ show a weak but significant correlation with local magnetic field and free energy. At 3σ the strength of the correlation abruptly increases. Above 5σ no correlation is apparent, but large magnetic field values appear. Using a mask to remove the network areas, the weakest brightenings (<1.5 σ ) show anti-correlation with the magnetic field. For 1.5 σ to 4.5 σ there is no correlation. For selected network examples we follow the time evolution in all observed lines. We find cases in which an increase and then relaxation in the magnetic free energy just precedes a local rise in Ca emission followed by a drop to a lower background level than initially. Work supported in part by NSF-ATM-9987305 and NASA-NAG5-10880. Title: Observations of the Structure of small scale photospheric fields Authors: Lawrence, J.; Cadavid, A.; Ruzmaikin, A.; Berger, T. Bibcode: 2002ocnd.confE..26L Altcode: No abstract at ADS Title: Small-scale solar magnetic dynamics Authors: Berger, Thomas Bibcode: 2002ocnd.confE...2B Altcode: No abstract at ADS Title: Austrian radiation dose measurements onboard space station mir and the international space station iss - overview and comparison Authors: Berger, T.; Hajek, M.; Summerer, L.; Vana, N.; Akatov, Y.; Shurshakov, V.; Arkhangelsky, V. Bibcode: 2002cosp...34E2588B Altcode: 2002cosp.meetE2588B The Atominstitut of the Austrian Universities has conducted various space research missions in the last 12 years in cooperation with the Institute for Biomedical Problems in Moscow. They dealt with the exact determination of the radiation hazards for cosmonauts and the development o precise measurement devices.f Special emphasis will be laid on the last experiment on space station MIR the goal of which was the determination of the depth distribution of absorbed dose and dose equivalent in a water filled phantom. The first results from dose measurements onboard the International Space Station will also be discussed.. The phantom with a diameter of 35 cm was developed at the Institute for Biomedical Problems and had 4 channels where dosemeters can be exposed in different depths. The exp osure period covered the timeframe from May 1997 to February 1999. Thermoluminescent dosemeters (TLDs) were exposed inside the phantom, either parallel or perpendicular to the hull of the spacecraft. For the evaluation of the linear energy transfer (LET), the High Temperature Ratio (HTR) - method was applied. Based on this method a mean quality factor and, subsequently, the dose equivalent is calculated according to the Q(LET ) relationship proposed in ICRP 26. An increased contribution of neutrons could be detected inside the phantom. However the total dose equivalent did not increase over the depth of the phantom. As the first Austrian measurements on the ISS dosemeter packages were exposed for 248 days, starting in February 2001 at six different locations onboard the ISS. The Austrian dosemeter sets for this first exposure on the ISS contained 5 different kinds of passive thermoluminescent dosemeters. First results showed a position dependent absorbed dose rate and LET at the ISS. Dose rates ranged from 180 to 280 μGy/d. The differences in dose measurements onboard the 2 space stations will be discussed. Title: Precision spectro-polarimeter for high-resolution observations of solar magnetic fields Authors: Lites, Bruce W.; Elmore, David F.; Streander, Kim V.; Akin, David L.; Berger, Tom; Duncan, Dexter W.; Edwards, Chris G.; Francis, Barbara; Hoffmann, Chris; Katz, Noah; Levay, Michael; Mathur, Dnyanesh; Rosenberg, William A.; Sleight, Ericka; Tarbell, Theodore D.; Title, Alan M.; Torgerson, Darrel Bibcode: 2001SPIE.4498...73L Altcode: As a Japanese National space mission with international collaboration, Solar-B (2005 launch) will carry a spectro- polarimeter (SP) to be operated in visible light to obtain the first high angular resolution, precision measurements of solar vector magnetic fields from space. The SP is part of the Focal Plane Package (FPP) fed by a diffraction-limited 50-cm optical telescope. The SP will be operated exclusively at the photospheric 630 nm Fe I lines. It features a rotating, low-order crystalline quartz retarder for polarization modulation and a reflecting Littrow spectrograph design that is shortened by using diffraction from the 12micrometers wide slit to fill the grating. Polarization analysis is accomplished by a modified Savart plate beam splitter. A custom CCD detector with two active areas, one for each beam from the beam splitter, allows continuous high duty-cycle sampling of polarization. The spectrograph slit will sample a 0.16 x 164 arcsec2 rectangle of the solar image, which may be scanned across the slit by up to +/- 160 arcsec in order to build up vector magnetic field maps of the solar photosphere. Along with simultaneous, co-spatial imaging and polarimetry with the filter imagers of the FPP, the SP will provide a precise view of active and quiet solar magnetic fields that control the structure, dynamics, and energetics of the upper solar atmosphere. Title: Two dual-wavelength sequences of high-resolution solar photospheric images captured over several hours and restored by use of phase diversity Authors: Löfdahl, M. G.; Berger, T. E.; Seldin, J. H. Bibcode: 2001A&A...377.1128L Altcode: The collection, seeing compensation, and temporal filtering of two high-resolution time-sequences of solar photospheric images are described. 44arcsecx80 arcsec image sequences of co-spatial and co-temporal 430.5 nm G band and 436.4 nm continuum filtergrams, were obtained with the 47.5 cm Swedish Vacuum Solar Telescope. One data set covers 5 hours of photospheric evolution; the other covers 8 hours. The field-of-view contains both an enhanced network region, a large pore, and in the longer sequence, a pore forming event. The mean time between frames is <40 s. With a few exceptions, the G band frames are partitioned phase-diverse speckle (PPDS) restorations of three realizations of the atmospheric turbulence acquired rapidly in sequence. Due to strict simultaneity and closely spaced wavelengths, the G band wavefronts, compensated for fixed aberration differences, could also be used for deconvolving the corresponding continuum data. For some of the data, collected during periods of particularly bad seeing, restorations made with a related method, joint phase-diverse speckle, were substituted for the PPDS restorations. Title: Spatiotemporal Scaling of Solar Surface Flows Authors: Lawrence, J. K.; Cadavid, A. C.; Ruzmaikin, A.; Berger, T. E. Bibcode: 2001PhRvL..86.5894L Altcode: 2001astro.ph..1224L The sun provides an excellent natural laboratory for nonlinear phenomena. We use motions of magnetic bright points on the solar surface, at the smallest scales yet observed, to study the small scale dynamics of the photospheric plasma. The paths of the bright points are analyzed within a continuous time random walk framework. Their spatial and temporal scaling suggests that the observed motions are the walks of imperfectly correlated tracers on a turbulent fluid flow in the lanes between granular convection cells. Title: On the Relation of G-Band Bright Points to the Photospheric Magnetic Field Authors: Berger, T. E.; Title, A. M. Bibcode: 2001ApJ...553..449B Altcode: Cotemporal observations in the 4305 Å G-band and Ca II λ3933 K-line, Fe I 6302 Å magnetograms, and 6563 Å Hα images are used to study the relation of G-band bright points (GBPs) to magnetic elements in the photosphere. Angular resolution of 0.2" and 0.3" is achieved in the best G-band and magnetogram images, respectively. Single magnetogram sensitivity of 120-150 gauss (Φmin~1016 Mx) is achieved. Small-scale GBPs appear both in intergranular lanes and on the edges of certain bright, rapidly expanding granules. The latter class of GBPs are nonmagnetic (at the flux limit) and are a source of confusion in magnetic element studies. The large-scale pattern of GBPs and magnetic flux in plage are highly correlated; GBPs occur preferentially on the periphery of extended plage regions, which are primarily demarcated by dark or neutral-contrast regions (e.g., pores or unresolved structures). On subarcsecond scales, GBPs are cospatial (to within an average of 0.24") and comorphous with magnetic elements in intergranular lanes; larger flux concentrations appear more diffuse than the associated GBP groupings. The average peak flux density of GBPs in the data set is ~160 gauss. No significant trend in GBP flux density as a function of either contrast or size is found. Rings of magnetic elements on 5" scales remain very stable for periods on the order of hours. GBPs trace the temporal evolution of magnetic elements closely: there is no indication of a lead or lag (to within the 30-90 s precision of our data) in the appearance of GBPs relative to the appearance of magnetic elements. Pore formation via the accumulation of magnetic elements at a flow-field sink is seen in the data set. Magnetic elements and granules are continually advected into pores by the photospheric flow field. Title: Intercomparison of SOUP, ASP, LPSP, and MDI magnetograms Authors: Berger, T.; Lites, B.; Martinez-Pillet, V.; Tarbell, T.; Title, A. Bibcode: 2001AGUSM..SP51B12B Altcode: We compare simultaneous magnetograms of a solar active region taken by the Advanced Stokes Polarimeter (ASP) and the Solar Optical Universal Polimeter (SOUP) in 1998. In addition we compare magnetograms taken by the La Palma Stokes Polarimeter (LPSP), the Michelson Doppler Imager (MDI) on SOHO, and the SOUP instrument in 2000. The SOUP instrument on the Swedish Vacuum Solar Telescope (SVST) attains the highest spatial resolution but has the least understood calibration; the ASP on the Dunn Solar Telescope (DST) at Sacramento Peak attains the highest magnetic field precision. The goal of the program is to better quantify the SOUP magnetograms and thereby study magnetic element dynamics in the photosphere with higher precision. Title: High Resolution Observations and Modeling of Small-Scale Solar Magnetic Elements Authors: Berger, Thomas E. Bibcode: 2001STIN...0132415B Altcode: This research contract investigating the radiative transfer and dynamic physics of the smallest observable magnetic structures in the solar photosphere. Due to the lack of a high-resolution visible light satellite instrument for solar studies, all data were acquired using ground-based instrumentation. The primary goal of the investigation was to understand the formation and evolution of "G-band bright points" in relation to the associated magnetic elements. G-band bright points are small (on the order of 100 kin or less in diameter) bright signatures associated with magnetic flux elements in the photosphere. They are seen in the A2A-X2 4308 A molecular bandhead of the CH radical ill the solar spectrum and offer the highest spatial resolution and highest contrast "tracers" of small magnetic structure on the Sun. Title: Local-area helioseismology by SOT on-board Solar-B Authors: Sekii, T.; Shibahashi, H.; Kosovichev, A. G.; Duvall, T. L., Jr.; Berger, T. E.; Bush, R.; Scherrer, P. H. Bibcode: 2001ESASP.464..327S Altcode: 2001soho...10..327S Solar-B satellite, a successor to Yohkoh, will be launched in 2005. Placed in a sun-synchronous orbit, it will carry out multi-wavelength observation in optical, EUV and X-ray ranges. One of the instruments on Solar-B, Solar Optical Telescope (SOT), a Japan/US collaboration, aims at measuring the magnetic field and the Doppler velocity field in the solar photosphere. Although it is not specifically designed for helioseismic observations, the high-resolution Dopplergram produced by SOT is potentially a very powerful tool for detailed seismic investigation of subsurface magnetic and thermal structures and associated mass flows. If successful, these measurements will be an important contribution to the main goal of the Solar-B project: understanding the origin and dynamics of the basic magnetic structures and their effects on the solar corona. We discuss the prospect and challenges of local-area helioseismology by SOT. Title: In-flight performance of the Very high Angular resolution ULtraviolet Telescope sounding rocket payload Authors: Korendyke, Clarence M.; Vourlidas, A.; Cook, John W.; Dere, Kenneth P.; Feldman, R.; Howard, Russell A.; Lilley, D. N.; Morrill, Jeff S.; Moses, J. Daniel; Moulton, Norman E.; Moye, Robert W.; Roberts, D. E.; Shepler, E. L.; Smith, J. K.; Socker, Dennis G.; Spears, T. R.; Waymire, R. S.; Brown, Wayne E.; Tarbell, Theodore D.; Berger, Tom; Handy, Brian N. Bibcode: 2000SPIE.4139..340K Altcode: The Very high Angular Resolution ULtraviolet Telescope experiment was successfully launched on May 7, 1999 on a Black Brant sounding rocket vehicle from White Sands Missile Range. The instrument consists of a 30 cm UV diffraction limited telescope followed by a double grating spectroheliograph tuned to isolate the solar Lyman (alpha) emission line. During the flight, the instrument successfully obtained a series of images of the upper chromosphere with a limiting resolution of approximately 0.33 arc-seconds. The resulting observations are the highest resolution images of the solar atmosphere obtained from space to date. The flight demonstrated that subarc-second ultraviolet images of the solar atmosphere are achievable with a high quality, moderate aperture space telescope and associated optics. Herein, we describe the payload and its in- flight performance. Title: On the Nature of the ``Moss'' Observed by TRACE Authors: Martens, P. C. H.; Kankelborg, C. C.; Berger, T. E. Bibcode: 2000ApJ...537..471M Altcode: ``Moss'' is the name given to low-lying (~3000 km), hot (~1 MK) solar coronal plasma that has been observed recently by the Transition Region and Coronal Explorer (TRACE). This paper investigates two hypotheses regarding the nature of the moss: (1) emission from small, million degree loops; (2) emission from the legs of 3-10 million degree loops. We update the coronal radiative loss curve, using the most recent results for coronal abundances, and use an analytical loop model to find that the first hypothesis requires a filling factor close to unity to reproduce the observed emission measure, while the second hypothesis results in a filling factor of about 0.1, in agreement with other independent multiwavelength analyses of moss. We find that the vertical extent and the height of the moss layer above the limb are also very well reproduced with the second hypothesis. We further show that the observed brightness of the moss scales linearly with the loop pressure and filling factor, independent of the loop length, and we derive a general expression for the conversion factor. Title: The Solar-B Focal Plane Package Authors: Berger, T. E.; Title, A. M.; Tarbell, T. D.; Lites, B. W.; Elmore, D. F. Bibcode: 2000SPD....31.0292B Altcode: 2000BAAS...32..827B Solar-B is a Japanese national space science mission of the Institute of Space and Astronautical Sciences (ISAS) with participation from US and UK research groups. The satellite consists of a 50-cm optical telescope and Focal Plane Package (FPP) designed for high resolution photospheric and chromospheric imaging and spectro-polarimetry as well as two coronal instruments: the X-Ray Telescope (XRT) and the Extreme-ultraviolet Imaging Spectrometer (EIS). Solar-B will be launched into a Sun-synchronous orbit in August of 2004. A team of Lockheed Martin Solar and Astrophysics Laboratory (LMSAL), High Altitude Observatory, and ISAS personnel are designing the FPP instrument. It consists of a narrow-band tunable birefringent filter system, a wide band interference filter system, and a spectro-polarimeter system for very high sensitivity Stokes polarimetry, all of which will be fabricated at LMSAL. We describe the main science goals of the FPP as well as the current instrument design and performance characteristics. This work is supported by NASA contract NAS8-00014 (Solar-B FPP). Title: The Solar Photosphere Authors: Berger, Tom Bibcode: 2000astu.confE...4B Altcode: No abstract at ADS Title: Dynamics of Transition Region `Moss' at high time resolution Authors: De Pontieu, B.; Berger, T. E.; Schrijver, C. J.; Title, A. M. Bibcode: 1999SoPh..190..419D Altcode: Recent observations of solar active regions made with the Transition Region and Coronal Explorer (TRACE) have revealed finely textured, low-lying extreme ultraviolet (EUV) emission, called the moss. It appears as a bright, dynamic pattern with dark inclusions, structured on spatial scales of 1 to 3 Mm. The moss has been interpreted as the upper transition region above active region plage and below relatively hot loops. Here we study the temporal variability of the morphology of the moss using a 2-hr time sequence of high-cadence TRACE 171 Å images and G-band, Ca ii K-line and Hα filtergrams from the Swedish Vacuum Solar Telescope (SVST, La Palma) on 1 June 1999. The data provide a unique view of the connections between the photosphere, chromosphere, transition region and corona in an active region. We find that the moss is dynamic on time scales of 10-30 s due to intrinsic changes in brightness, obscuration by chromospheric jets and motion caused by physical interaction with these jets. The temporal variations of the bright moss elements occur on shorter time scales than those of the Ca ii K-line bright points. The bright moss elements generally do not occur directly above the G-band or Ca ii K-line bright points in the photosphere or lower chromosphere. This suggests that the upper transition region emission often occurs at the interface of neighboring flux tubes. The temporal variability of the moss brightness on 30 s time scales may suggest that the energy source of these intensity changes occurs relatively locally (height <10 000 km). Title: What is Moss? Authors: Berger, T. E.; De Pontieu, B.; Fletcher, L.; Schrijver, C. J.; Tarbell, T. D.; Title, A. M. Bibcode: 1999SoPh..190..409B Altcode: TRACE observations of active regions show a peculiar extreme ultraviolet (EUV) emission over certain plage areas. Termed `moss' for its spongy, low-lying, appearance, observations and modeling imply that the phenomenon is caused by thermal conduction from 3-5 MKcoronal loops overlying the plage: moss is the upper transition region emission of hot coronal loops. The spongy appearance is due to the presence of chromospheric jets or `spicules' interspersed with the EUV emission elements. High cadence TRACE observations show that the moss EUV elements interact with the chromospheric jets on 10 s time scales. The location of EUV emission in the moss does not correlate well to the locations of underlying magnetic elements in the chromosphere and photosphere, implying a complex magnetic topology for coronal loop footpoint regions. We summarize here the key observations leading to these conclusions and discuss new implications for understanding the structuring of the outer solar atmosphere. Title: High-resolution Imaging of the Solar Chromosphere/Corona Transition Region Authors: Berger, T. E.; De Pontieu, B.; Schrijver, C. J.; Title, A. M. Bibcode: 1999ApJ...519L..97B Altcode: The properties of a previously unresolved extreme-ultraviolet (EUV) emission in solar active regions are examined using coordinated data sets from the Transition Region and Coronal Explorer (TRACE) satellite, the Michelson Doppler Imager on the Solar and Heliospheric Observatory satellite, the Soft X-Ray Telescope (SXT) on the Yohkoh satellite, and the ground-based Swedish Vacuum Solar Telescope (SVST) on La Palma. The emission appears most prominently in TRACE Fe IX/Fe X 171 Å images as a bright dynamic network surrounding dark inclusions on scales of 2-3 Mm, confined to layers approximately 1-3 Mm thick with base heights approximately 2-4 Mm above the photosphere. It is seen only above plage regions that underlie (3-5)×106 K coronal loops visible in SXT images. The bright EUV elements emit at temperatures of about 106 K. Fine-scale motions and brightness variations of the emission occur on timescales of 1 minute or less. The dark inclusions correspond to jets of chromospheric plasma seen in simultaneous SVST filtergrams in the wings of Hα. The combined characteristics imply that we are at least partially resolving the structure and dynamics of the conductively heated upper transition region between the solar chromosphere and corona. Title: A new view of the solar outer atmosphere by the Transition Region and Coronal Explorer Authors: Schrijver, C. J.; Title, A. M.; Berger, T. E.; Fletcher, L.; Hurlburt, N. E.; Nightingale, R. W.; Shine, R. A.; Tarbell, T. D.; Wolfson, J.; Golub, L.; Bookbinder, J. A.; DeLuca, E. E.; McMullen, R. A.; Warren, H. P.; Kankelborg, C. C.; Handy, B. N.; De Pontieu, B. Bibcode: 1999SoPh..187..261S Altcode: The Transition Region and Coronal Explorer (TRACE) - described in the companion paper by Handy et al. (1999) - provides an unprecedented view of the solar outer atmosphere. In this overview, we discuss the initial impressions gained from, and interpretations of, the first million images taken with TRACE. We address, among other topics, the fine structure of the corona, the larger-scale thermal trends, the evolution of the corona over quiet and active regions, the high incidence of chromospheric material dynamically embedded in the coronal environment, the dynamics and structure of the conductively dominated transition region between chromosphere and corona, loop oscillations and flows, and sunspot coronal loops. With TRACE we observe a corona that is extremely dynamic and full of flows and wave phenomena, in which loops evolve rapidly in temperature, with associated changes in density. This dynamic nature points to a high degree of spatio-temporal variability even under conditions that traditionally have been referred to as quiescent. This variability requires that coronal heating can turn on and off on a time scale of minutes or less along field-line bundles with cross sections at or below the instrumental resolution of 700 km. Loops seen at 171 Å (∼1 MK) appear to meander through the coronal volume, but it is unclear whether this is caused by the evolution of the field or by the weaving of the heating through the coronal volume, shifting around for periods of up to a few tens of minutes and lighting up subsequent field lines. We discuss evidence that the heating occurs predominantly within the first 10 to 20 Mm from the loop footpoints. This causes the inner parts of active-region coronae to have a higher average temperature than the outer domains. Title: Dynamics of the Solar Chromosphere. II. Ca II H2V and K2V Grains versus Internetwork Fields Authors: Lites, B. W.; Rutten, R. J.; Berger, T. E. Bibcode: 1999ApJ...517.1013L Altcode: We use the Advanced Stokes Polarimeter at the NSO/Sacramento Peak Vacuum Tower Telescope to search for spatio-temporal correlations between enhanced magnetic fields in the quiet solar internetwork photosphere and the occurrence of Ca II H2V grains in the overlying chromosphere. We address the question of whether the shocks that produce the latter are caused by magnetism-related processes, or whether they are of purely hydrodynamic nature. The observations presented here are the first in which sensitive Stokes polarimetry is combined synchronously with high-resolution Ca II H spectrometry. We pay particular attention to the nature and significance of weak polarization signals from the internetwork domain, obtaining a robust estimate of our magnetographic noise level at an apparent flux density of only 3 Mx cm-2. For the quiet Sun internetwork area analyzed here, we find no direct correlation between the presence of magnetic features with apparent flux density above this limit and the occurrence of H2V brightenings. This result contradicts the one-to-one correspondence claimed by Sivaraman & Livingston. We also find no correspondence between H2V grains and the horizontal-field internetwork features discovered by Lites et al. Title: Dynamics of Transition Region Moss Authors: Berger, T. E.; de Pontieu, B.; Schrijver, C. J.; Title, A. M. Bibcode: 1999AAS...194.7901B Altcode: 1999BAAS...31..963B We examine the dynamics of solar transition region "moss", the 10(6) K EUV emission at the footpoint regions of 2--3 MK active region coronal loops. Comparisons of TRACE 171 Angstroms movies with SVST (La Palma) Ca II K-line, Hα , and G-band movies are made. Local Correlation Tracking (LCT) flowmapping techniques are used to establish the photospheric flowfield in plage regions with and without associated moss. The relation of moss emission to chromospheric spicules or fibrils is examined in detail using Hα movies and dopplergrams. In addition, several microflare events occuring in plage regions are analyzed using TRACE and SVST movies. This research was supported by NASA contract NAS5-38099 (TRACE) and NASA SR&T grant NASW-98008. Title: The Solar-B Solar Optical Telescope Focal Plane Package Authors: Levay, M.; Berger, T.; Rosenberg, W.; Tarbell, T.; Title, A.; Bogdan, T.; Elmore, D.; Lites, B. Bibcode: 1999AAS...194.7610L Altcode: 1999BAAS...31R.957L The primary goal of the Solar-B mission is to understand the physical processes responsible for dynamics and heating of the outer solar atmosphere. The Focal Plane Package (FPP) instrument for the 50-cm Solar Optical Telescope provides precise measurements of the vector magnetic field, vertical and horizontal flows, and thermal conditions in the photosphere and low chromosphere with spatial resolution as high as 0.16 arcsec and a field-of-view as large as 320 x 160 arcsec. The FPP can measure continuously and at high cadence to follow the evolution of solar features. The FPP consists of broad ( 8 Angstroms) and narrow ( 100 m Angstroms) filters and a spectro-polarimeter that provides precise polarimetry with high spectral resolution ( 25 m Angstroms). A correlation tracker and tip-tilt mirror ensure that all focal planes are stable to better than 0.01 arcsec. A major design consideration of the FPP is cooperative science operations with the other Solar-B instruments. Solar-B is a Japanese mission with US and UK partners; S. Tsuneta is the PI of the Solar Optical Telescope and A. Title the US PI of the FPP. It is scheduled to launch in Japanese FY 2004. Title: Dynamics and Plasma Diagnostics of Transition Region ``Moss'' using SOHO/CDS, TRACE and SVST (La Palma) Authors: de Pontieu, B.; Berger, T. E.; Fletcher, L.; Schrijver, C. J.; Title, A. M. Bibcode: 1999AAS...194.7804D Altcode: 1999BAAS...31..961D Recent observations of solar active regions with the Transition Region And Coronal Explorer (TRACE) have revealed finely textured, low-lying extreme ultraviolet (EUV) emission, called the ``moss'', appearing as a bright dynamic pattern with dark inclusions. The moss has been interpreted as the upper transition region by Berger et al., (1999). In this poster we study the physical conditions in the moss plasma, as well as its dynamics and connections to photosphere and chromosphere. Using simultaneous SOHO Coronal Diagnostic Spectrometer (CDS) and TRACE observations of Active Region (AR) 8227 on 30-May-1998 we determine the physical parameters of the moss material. We find T_e = 0.6-1.5 10(6) K and n_e = 2-5 10(9) cm(-3) at a temperature of 1.3 10(6) K. The pressure in the moss plasma is higher than that in coronal loops observed in the TRACE Fe IX/X 171 Angstroms passband, and moss emission is associated with high temperature loops, observed by SXT and by CDS in lines of T_max > 2.5 10(6) K. The volume filling factor of the moss plasma is of the order 0.1 and the path along which the emission originates is of the order 1,000 km long. We examine the dynamics of the moss plasma, by making comparisons of TRACE 171 Angstroms movies with SVST (La Palma) Ca II K-line, Hα , and G-band movies. Local Correlation Tracking (LCT) flowmapping techniques are used to establish the photospheric flowfield in plage regions with and without associated moss. The relation of moss emission to chromospheric spicules or fibrils is examined in detail using Hα movies and dopplergrams. In addition, several miniflare events occuring in plage regions are analyzed using TRACE and SVST movies. This research was supported by NASA contract NAS5-38099 (TRACE) and NASA SR&T grant NASW-98008. Title: Coordinated Observations of Transition Region Dynamics using TRACE and the SVST Authors: Berger, T.; de Pontieu, B.; Schrijver, C.; Title, A.; Scharmer, G. Bibcode: 1999ASPC..183..365B Altcode: 1999hrsp.conf..365B No abstract at ADS Title: Dynamics of the Quiet Solar Chromosphere Authors: Rutten, R. J.; Lites, B. W.; Berger, T. E.; Shine, R. A. Bibcode: 1999ASPC..158..249R Altcode: 1999ssa..conf..249R No abstract at ADS Title: Measurements of Solar Magnetic Element Dispersal Authors: Berger, Thomas E.; Löfdahl, Mats G.; Shine, Richard A.; Title, Alan M. Bibcode: 1998ApJ...506..439B Altcode: The dispersal of magnetic elements in the solar photospheric flow field is studied by tracking individual ``magnetic bright points'' (MBPs) identified in a G-band 4305 Å filtergram time series obtained at the 50 cm Swedish Vacuum Solar Telescope on La Palma, Spain. The time series spans approximately 70 minutes with a field of view of 29" × 29" near disk center. All images in the time series are restored to near the telescope diffraction limit (~0.2" in the G band) using partitioned phase diverse speckle techniques. Regions of enhanced magnetic network and quiet Sun are examined. In the network region, automated tracking of individual MBPs reveals approximately Gaussian diffusion, with indications for slightly ``superdiffusive'' dispersal. The inferred Gaussian diffusion coefficient is 60.4 +/- 10.9 km2 s-1. In the quiet-Sun region, local correlation tracking velocity measurements show the dispersal of artificial tracers to be non-Gaussian over most of our data set with indications of an asymptotic approach to a 285 km2 s-1 Gaussian diffusion. Title: Measurements of Solar Magnetic Element Motion from High-Resolution Filtergrams Authors: Berger, Thomas E.; Löfdahl, Mats G.; Shine, Richard S.; Title, Alan M. Bibcode: 1998ApJ...495..973B Altcode: Solar photospheric flowfield properties on sub-0.5" scales are measured using local correlation tracking (LCT) and object tracking of magnetic bright points (MBPs: photospheric bright points associated with magnetic elements). The dataset is a 70 minute time series of cospatial and cotemporal G-band 4305 Å and wideband 4686 Å filtergrams obtained with the 50 cm Swedish Vacuum Solar Telescope on the island of La Palma, Spain. We examine a 29" × 70" field of view (FOV) near disk center and compare a 29" × 29" magnetic network subfield and a 27" × 27" apparently nonmagnetic ``quiet-Sun'' subfield. The mean time between frames is 23.75 s. Each frame is created by partitioned phase-diverse speckle restoration of three image pairs acquired rapidly in sequence. Angular resolution is ~0.4" or less in all frames of the restored data set.

From LCT on a 0.4" grid with 0.83" FWHM apodization, we find the flow speeds to be Rayleigh distributed with a mode of 550 m s-1 and an average of 950 m s-1 in the network FOV; in the quiet FOV the modal speed is 700 m s-1 with a mean of 1100 m s-1. Within the network FOV, a ``magnetic region'' defined by the loci of tracked MBPs exhibit even greater alteration: rms contrast of the region is 8% higher in the G band compared to areas outside, LCT speeds are reduced by a factor of 1.6, and the convective flow structures are smaller and much more chaotic. Mesogranulation is entirely absent in the magnetic region. The modal and mean speeds of 534 tracked MBPs are 300 m s-1 and 1470 m s-1, respectively. MBPs split and merge with mean times of 320 and 404 s respectively. The mean lifetime of MBPs in the data set is 9.33 minutes although approximately 5% of the objects can be tracked for the entire 70 minute duration of the time series. Title: On the Dynamics of Magnetic Flux Concentrations in Quiet Photospheric Network. Authors: Sakai, J. I.; Ryutova, M.; Schrijver, K.; Shine, R.; Tarbell, T.; Berger, T.; Title, A.; Hagenaar, H. Bibcode: 1997SPD....28.0260S Altcode: 1997BAAS...29..904S Magnetic flux concentrations in the quiet photospheric network show a complex dynamics which includes merging of colliding fluxes, the "total" or partial cancellation of neighboring fluxes, fragmentation and others. We propose a mechanism to explain the observed phenomena based on the idea that magnetic flux concentrations in the photospheric network are essentially non-collinear. We show that non-collinearity of colliding fluxes leads to the whole new class of effects which are observed; for example, the apparent cancellation of opposite polarity fluxes turns into the formation of horizontal magnetic fluxes (which later may appear as a new weaker bipoles) and is accompanied by the shock formation and mini-flares. In the case of shock formation the reconnection area becomes a source of the acoustic emission; mini-flares may be seen as bright points. The energetics of these processes strongly depends on geometry of "collision" and physical parameters of colliding fluxes. For example, if colliding fluxes have comparable and "small" cross sections, the reconnection results in complete reorganization of their magnetic fields; if merging fluxes are large enough or considerably different, magnetic flux may be only partially reconnected and partially survived. Reconnection of non-collinear equal polarity fluxes leads to the "scattering" processes which include the fragmentation into several smaller fluxes if initially colliding concentrations carried different amount of magnetic flux. We give the example of numerical simulation for the case of merging and fragmentation process occurring during the collision of collinear "strong" and "weak" magnetic flux concentrations. The calculation results shown to be consistent with observational data from both the SOHO/MDI instrument and the Swedish Vacuum Solar Telescope on La Palma. This research is supported by NASA contract NAG5-3077 at Stanford University and the MDI contract PR 9162 at Lockheed. Title: Phase-Diversity Restoration of two Simultaneous 70-minute Photospheric Sequences. Authors: Lofdahl, M. G.; Berger, T. E.; Shine, R. A.; Title, A. M. Bibcode: 1997SPD....28.0218L Altcode: 1997BAAS...29..896L Seeing effects have been corrected in two cospatial and cotemporal 70-minute sequences of images collected in the G-band 4305 Angstroms and wideband 4686 Angstroms. The data were obtained with the 50 cm Swedish Vacuum Solar Telescope on the island of La Palma, Spain. The 29arcsecx 70arcsec field-of-view (FOV) near disk center contains both an enhanced network region and an (apparently) non-magnetic ``quiet'' region of granulation. The mean time between restored frames is 23.5 s. Each of the 180 images is created with Phase-Diverse Speckle (PDS) imaging, using two different focus positions sampled at the best three snapshots of the atmospheric turbulence (seeing) during a 20-second selection window. Wavefronts are estimated for each focused--defocused image pair and a restored frame is produced from all six images. The average resolution in the restored sequence is about 0farcs4 (corresponding to spatial frequencies up to half the diffraction limit of the telescope), which is good enough to allow detection of ~ 0farcs2 bright points. The data is used for statistical measurements of magnetic element speed, interaction frequency, and lifetime (see accompanying poster by T. E. Berger et al). We show destretched and space-time filtered movies of both the G-band and continuum images, as well as raw data to demonstrate the effect of the restoration process. This work was supported by NASA contracts NAS5-30386 at Stanford and NAS8-39747 and Independent Research Funds at Lockheed-Martin. MGL was supported by the Swedish Science Research Council. Title: Comparison of Granulation Correlation Tracking (CT) and Feature Tracking (FT) Results from SOHO/MDI and the Swedish Vacuum Solar Telescope on La Palma Authors: Shine, R.; Strous, L.; Simon, G.; Berger, T.; Hurlburt, N.; Tarbell, T.; Title, A.; Scharmer, G. Bibcode: 1997SPD....28.0262S Altcode: 1997BAAS...29Q.904S We have computed photospheric velocity flow maps from simultaneous observations taken with MDI and at the Swedish Vacuum Solar Tower (SVST) on La Palma on August 15, 1996. Both sets consist of a series of photospheric images, and flow maps are computed by following the local motions of granules. The MDI data have the important advantages of very stable images and longer continuous coverage of the same area of the solar surface. This longer coverage is necessary to study the evolution of mesogranules, supergranules, and to detect possible low amplitude motions on scales larger than supergranules. However, the high resolution mode of MDI is limited by the small telescope size to about 1.2 arc seconds angular resolution and uses a 0.6 arc second pixel size. This is adequate to show granulation but has the rms constrast significantly reduced to about 2%. Early efforts adapting techniques that were successful with higher resolution ground based images gave poor results and although new methods have now been developed, there are still some problems with accuracy. On the other hand, the SVST images have much higher angular resolution (as good as 0.2 arc second) but suffer from variable atmospheric distortion. They also have a much smaller field of view. By detailed comparison of the two data sets and by using CT and FT techniques to track the motions, we hope to understand the sources of any differences between them and to develop credible correction parameters to the MDI data sets if necessary. This work was supported by NASA Grant NAG5-3077 at Stanford and Lockheed Martin, by AFOSR and the Fellows Program of AF Phillips Lab at NSO/SP, and by the Swedish Royal Academy of Sciences. Title: Measurements of Magnetic Element Dynamics in the Network Authors: Berger, T. E.; Lofdahl, M. G.; Shine, R. A.; Title, A. M. Bibcode: 1997SPD....28.0219B Altcode: 1997BAAS...29..896B Statistical measurements of magnetic element speed, interaction frequency, and lifetime in an enhanced network region at disk center are presented. The primary dataset is a 70 min time series of G-band 4305 Angstroms filtergrams taken at the 50 cm Swedish Vacuum Solar Telescope (SVST) on the island of La Palma, Spain. A second time series of 4686 Angstroms wide-band continuum filtergrams, cospatial and simultaneous to within several milliseconds with the G-band images, is also studied. The field-of-view is near Sun center and includes a region of enhanced network activity with many G-band bright points. Both time series are corrected for seeing to very near the telescope diffraction limit by the technique of Phase Diverse Speckle (PDS) restoration (see accompanying poster by M. G. Lofdahl et al). We show destretched and space-time filtered movies of both the G-band and continuum images in two fields-of-view: a region of quiet granulation and the region of enhanced network activity. Within the network, local correlation tracking measurements on a 0\farcs4 grid show the RMS speed to be 778 m s(-1) ; outside the network the RMS speed is 1168 m s(-1) . Corkflow simulations show that normal convective flow patterns (granulation and mesogranulation) are absent in the network. Magnetic elements move with modal and mean speeds of 100 m s(-1) and 815 m s(-1) , respectively. The mean interaction frequency (time between either merging or splitting) is 220 s. The mean lifetime of tracked magnetic elements in the network is 9.33 min although 5% of the elements are tracked for the entire 70 min of the times series. This work was supported by NASA contracts NAS5-30386 at Stanford and NAS8-39747 and Independent Research Funds at Lockheed-Martin. MGL was supported by the Swedish Science Research Council. Title: Observation and Analysis of Small-Scale Solar Magnetic Structure Authors: Berger, Thomas Edward Bibcode: 1997PhDT........14B Altcode: Properties of small-scale magnetic structures in the photosphere are analyzed in multi-spectral time-series image sets obtained at the 50 cm Swedish Solar Vacuum Telescope (SVST) on the island of La Palma, Spain. Several of the images are among the highest resolution images of the solar photosphere yet obtained. Sub-arcsecond-scale magnetic 'elements' are identified, segmented, and tracked using bright points found in very high spatial resolution G-band 4305 A filtergrams. Simultaneous images including Ca II K-line filtergrams, Fe I 6302 A magnetograms, and 4686 A broadband continuum filtergrams allow cross-wavelength comparison of properties. Angular resolution of the filtergrams is typically 0.25 '' and temporal resolution is in the range of 20-100 sec; magnetogram resolution approaches 0.3'' in some images and is generally below 0.5''. To above an 84% statistical confidence level, G-band bright points occur exclusively at sites of kilogauss, sub-arcsecond, magnetic flux concentrations in the photosphere; magnetic flux concentration is a necessary but not sufficient condition for the occurrence of G-band bright points. The measured distribution of magnetic element diameters in active region network is log-normal with a modal value of 220 km (0.3''). The smallest elements observed are 120 km (0.17'') in diameter; the largest are about 600 km (0.7'') in diameter. The average contrast with respect to quiet Sun of magnetic elements in the G-band is 30%: 2-3 times higher than the average continuum contrast. Magnetic element contrast does not vary with size within the size range of G-band bright point measurements. Average contrast increases with limbward heliocentric angle to a peak of about 80% at μ = /cosθ = 0.3; there is evidence of a decrease with further increase in angle. Magnetic elements undergo a continual fragmentation/merging evolution driven by the granular convective flowfield of the photosphere; morphological time scales are on the order of 100 seconds. Velocities of individual elements range from 1-5 km s-1 with an RMS value of 2.4 km s-1. The range of motion is typically on granular and mesogranular scales (1000-2500 km) with an average value of 2100 km. Individual fragments from clusters have a characteristic lifetime on the order of the granulation correlation time (6-8 minutes). The lifetime of clusters associated with persistent sinks in the granular flowfield is on the order of hours. Classical statistical analysis of displacement versus time yields a diffusion coefficient for network magnetic elements of 224.8± 0.2 km s-1. In general, the results are inconsistent with the idea of small-scale magnetic flux in the photosphere being contained in stable, isolated, 'flux tubes' and emphasize the need for better understanding of the formation and the thermal (and∨ non-thermal) heating of magnetic regions in the photosphere. Title: On the dynamics of magnetic flux concentrations in quiet photospheric network. Authors: Sakai, J. I.; Ryutova, M.; Schrijver, K.; Shine, R. A.; Tarbell, T. D.; Berger, T. E.; Title, A. M.; Hagenaar, H. J. Bibcode: 1997BAAS...29T.904S Altcode: No abstract at ADS Title: Double-Gaussian Models of Bright Points or Why Bright Points Are Usually Dark Authors: Title, A. M.; Berger, T. E. Bibcode: 1996ApJ...463..797T Altcode: We have modeled the structure of small bright features, "bright points" seen in an outstanding CH filter (0-band) image. In our model, bright points consist of a Gaussian bright core centered in a Gaussian dark surround. The basis for this approach is the observation that nearly all of the bright points in the image exist within intergranular lanes, vertices between granules, or local brightness depressions. Using reasonable estimates for the size and depth of vertices and lanes, the model predicts that bright points clearly detectable in images with 0".2 resolution will seldom be detectable in images with resolutions beyond 0".4. This occurs because the transfer function of the telescope and atmosphere averages the bright points with their comparably sized dark surroundings to near zero contrast when blurred beyond 0".4. These results explain the great rarity of images that clearly show bright points. Furthermore, the image shows many bright points with core diameters equal to that of the FWHM of a point-spread function of a perfect telescope. If the intensity profiles of these bright points were Gaussian on a flat background, then their intrinsic brightness would have to be unrealistically high and they would not disappear on images blurred beyond 0".4, but would simply gradually expand in size and drop in contrast as the blur increased. Because the bright points are sites of magnetic fields, our model helps to explain lower resolution disk center observations that show magnetic fields occur in regions that are dark relative to the mean continuum level. The modeling also suggests that bright points with diameters of 0".1 or less would be undetectable in the current generation of 0.5 m high-resolution solar telescopes, under any seeing conditions. Title: Observation and Analysis of Small-scale Solar Magnetic Structure Authors: Berger, T. Bibcode: 1996AAS...188.3312B Altcode: 1996BAAS...28..869B Solar magnetic flux elements on spatial scales below 350 km (0\arcsec.5) are analyzed using G-Band 4305 Angstroms, Ca II K-line, and 4686 Angstroms continuum filtegrams as well as Fe I 6302 Angstroms and 5250 Angstroms magnetograms acquired nearly simultaneously at the Swedish Solar Vacuum Telescope on La Palma. Spatial resolution is below 0\arcsec.3 in the majority of images. Phase-diversity image restoration is applied to yield a 180 frame (78 minute) image set in which nearly every frame exhibits 0\arcsec.2 spatial resolution. Image processing algorithms are developed which successfully segment the magnetic elements from the surrounding granulation for analysis. The FWHM of magnetic elements demarcated by G-band bright points in disk-center plage is log-normally distributed with a modal value of 220 km and an average value of 250 km. Average disk center contrast of magnetic elements in the G-band is 31% with maximum values frequently exceeding 70% relative to the quiet-Sun average. Simulataneous 4686 Angstroms continuum contrast is 2 to 3 times lower. The average G-band contrast of magnetic elements shows no size dependency over a range of 150---600 km in diameter. G-band bright points occur without exception on sites of isolated magnetic flux concentrations or peninsular concentrations extending from larger concentrations of flux; isolated magnetic flux concentrations are found without associated G-band bright points. Magnetic elements demarcated by G-band bright points occupy no more than 1---2% of plage and active network regions by area at any one time. Magnetic elements move in the intergranular flowfield at speeds from 0.5 to 5 km sec(-1) . The RMS speed is 2.4 km sec(-1) over an average range of 2100 km (3\arcsec). Continual fragmentation and merging of magnetic elements is the normal evolutionary mode for small-scale magnetic elements. The time scale for the dynamics is approximately 6--8 minutes, but significant morphological changes occur on time scales as short as 100 seconds. Analysis of the tracks of individual elements yields a diffusion coefficient of 224.8+/-0.2 {km}(2{sec}(-1)) . Indications of anomolous diffusivity consistent with diffusion on a fractal geometry are found. This research was supported by the SOI-MDI NASA contract NAG5-3077 at Stanford University and NASA contract NAS8-39747 and independent research funds at Lockheed-Martin. Title: On the Dynamics of Small-Scale Solar Magnetic Elements Authors: Berger, T. E.; Title, A. M. Bibcode: 1996ApJ...463..365B Altcode: We report on the dynamics of the small-scale solar magnetic field, based on analysis of very high resolution images of the solar photosphere obtained at the Swedish Vacuum Solar Telescope. The data sets are movies from 1 to 4 hr in length, taken in several wavelength bands with a typical time between frames of 20 5. The primary method of tracking small-scale magnetic elements is with very high contrast images of photospheric bright points, taken through a 12 Å bandpass filter centered at 4305 Å in the Fraunhofer "G band." Previous studies have established that such bright points are unambiguously associated with sites of small-scale magnetic flux in the photosphere, although the details of the mechanism responsible for the brightening of the flux elements remain uncertain. The G band bright points move in the intergranular lanes at speeds from 0.5 to 5 km s-1. The motions appear to be constrained to the intergranular lanes and are primarily driven by the evolution of the local granular convection flow field. Continual fragmentation and merging of flux is the fundamental evolutionary mode of small-scale magnetic structures in the solar photosphere. Rotation and folding of chains or groups of bright points are also observed. The timescale for magnetic flux evolution in active region plage is on the order of the correlation time of granulation (typically 6-8 minutes), but significant morphological changes can occur on timescales as short as 100 5. Smaller fragments are occasionally seen to fade beyond observable contrast. The concept of a stable, isolated subarcsecond magnetic "flux tube" in the solar photosphere is inconsistent with the observations presented here. Title: Motion and Evolution of Solar Magnetic Elements Authors: Berger, T. E.; Schrijver, C. J.; Shine, R. S.; Tarbell, T. D.; Title, A. M.; Scharmer, G. Bibcode: 1995AAS...18710104B Altcode: 1995BAAS...27.1426B The dynamics of sub-arcsecond solar magnetic flux tubes are analyzed based on very-high resolution movies of photospheric bright points obtained in 1994 at the 50-cm Swedish Solar Vacuum Telescope (SVST) on the island of La Palma, Spain. The bright points are imaged using a 12 Angstroms bandpass interference filter centered at 4305 Angstroms in the ``G Band'' molecular bandhead of the CH molecule. The image sets typically consist of up to 4 hours of consecutive images taken at a 10 to 20 second cadence. Spatial resolution throughout the movies averages less than 0\arcsec.5 and many frames in the sets exhibit resolution down to 0\arcsec.25. Magnetic flux elements in the photosphere are shown to move continually along the intergranular lanes at speeds of up to 5 km/sec and ranges up to several thousand km. Evolution of individual magnetic elements is dominated by the local evolution of surrounding granules. Fragmentation and merging is the fundamental mode of evolution of the majority of magnetic elements seen in our data. Rotation and folding of chains or groups of elements is also frequently observed. The time scale for the fragmentation/merging evolution of the elements is on the order of the lifetime of granulation (6--8 minutes), but significant morphological changes are seen to occur on time scales as short as 100 seconds. The concept of a stable, isolated, sub-arcsecond magnetic flux element in the solar photosphere is inconsistent with the observations presented here. Title: New Observations of Subarcsecond Photospheric Bright Points Authors: Berger, T. E.; Schrijver, C. J.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Scharmer, G. Bibcode: 1995ApJ...454..531B Altcode: We have used an interference filter centered at 4305 Å within the bandhead of the CH radical (the "G band") and real-time image selection at the Swedish Vacuum Solar Telescope on La Palma to produce very high contrast images of subarcsecond photospheric bright points at all locations on the solar disk. During the 6 day period of 1993 September 15-20 we observed active region NOAA 7581 from its appearance on the East limb to a near disk-center position on September 20. A total of 1804 bright points were selected for analysis from the disk center image using feature extraction image processing techniques. The measured FWHM distribution of the bright points in the image is subnormal with a modal value of 220 km (0".30) and an average value of 250 km (0".35). The smallest measured bright point diameter is 120 km (0".17) and the largest is 600 km (0".69). Approximately 60% of the measured bright points are circular (eccentricity ∼1.0), the average eccentricity is 1.5, and the maximum eccentricity corresponding to filigree in the image is 6.5. The peak contrast of the measured bright points is normally distributed. The contrast distribution variance is much greater than the measurement accuracy, indicating a large spread in intrinsic bright-point contrast. When referenced to an averaged "quiet-Sun area 1n the image, the modal contrast is 29% and the maximum value is 75%; when referenced to an average intergranular lane brightness in the image, the distribution has a modal value of 61 % and a maximum of 119%. The bin-averaged contrast of G-band bright points is constant across the entire measured size range. The measured area of the bright points, corrected for population and selection effects, covers about 1.8% of the total image area. Large pores and micropores occupy an additional 2% of the image area, implying a total area fraction of magnetic proxy features in the image of 3.8%. We discuss the implications of this area fraction measurement in the context of previously published measurements which show that typical active region plage has a magnetic filling factor on the order of 10% or greater. The results suggest that in the active region analyzed here, less than 50% of the small-scale magnetic flux tubes are demarcated by visible proxies such as bright points or pores. Title: Frame Selection Techniques for Solar Movies Authors: Shine, R. A.; Tarbell, T.; Title, A.; Scharmer, G.; Simon, G.; Brandt, P.; Berger, T. Bibcode: 1995SPD....26..506S Altcode: 1995BAAS...27..957S No abstract at ADS Title: Properties of Sub-Arcsecond Facular Bright Points Authors: Berger, T.; Schrijver, C.; Shine, R.; Tarbell, T.; Title, A.; Scharmer, G. Bibcode: 1995SPD....26..505B Altcode: 1995BAAS...27..957B No abstract at ADS Title: On the Relation Between Facular Bright Points and the Magnetic Field Authors: Berger, Thomas; Shine, Richard; Tarbell, Theodore; Title, Alan; Scharmer, Goran Bibcode: 1994AAS...185.8607B Altcode: 1994BAAS...26.1465B Multi-spectral images of magnetic structures in the solar photosphere are presented. The images were obtained in the summers of 1993 and 1994 at the Swedish Solar Telescope on La Palma using the tunable birefringent Solar Optical Universal Polarimeter (SOUP filter), a 10 Angstroms wide interference filter tuned to 4304 Angstroms in the band head of the CH radical (the Fraunhofer G-band), and a 3 Angstroms wide interference filter centered on the Ca II--K absorption line. Three large format CCD cameras with shuttered exposures on the order of 10 msec and frame rates of up to 7 frames per second were used to create time series of both quiet and active region evolution. The full field--of--view is 60times 80 arcseconds (44times 58 Mm). With the best seeing, structures as small as 0.22 arcseconds (160 km) in diameter are clearly resolved. Post--processing of the images results in rigid coalignment of the image sets to an accuracy comparable to the spatial resolution. Facular bright points with mean diameters of 0.35 arcseconds (250 km) and elongated filaments with lengths on the order of arcseconds (10(3) km) are imaged with contrast values of up to 60 % by the G--band filter. Overlay of these images on contemporal Fe I 6302 Angstroms magnetograms and Ca II K images reveals that the bright points occur, without exception, on sites of magnetic flux through the photosphere. However, instances of concentrated and diffuse magnetic flux and Ca II K emission without associated bright points are common, leading to the conclusion that the presence of magnetic flux is a necessary but not sufficient condition for the occurence of resolvable facular bright points. Comparison of the G--band and continuum images shows a complex relation between structures in the two bandwidths: bright points exceeding 350 km in extent correspond to distinct bright structures in the continuum; smaller bright points show no clear relation to continuum structures. Size and contrast statistical cross--comparisons compiled from measurements of over two-thousand bright point structures are presented. Preliminary analysis of the time evolution of bright points in the G--band reveals that the dominant mode of bright point evolution is fission of larger structures into smaller ones and fusion of small structures into conglomerate structures. The characteristic time scale for the fission/fusion process is on the order of minutes. Title: Stanford MAMA detector characterization facility Authors: Timothy, J. Gethyn; Bergamini, Paolo; Berger, Thomas E.; Bumala, Robert W.; Liu, Sharon; Martinez, Ted; Slater, David C. Bibcode: 1993SPIE.2006...59T Altcode: We have designed and fabricated a high-vacuum facility for the detailed characterization of the Multi-Anode Microchannel Array (MAMA) detector systems at Extreme Ultraviolet and Far Ultraviolet wavelengths between about 300 angstroms and 3000 angstroms. The first task for this facility is the characterization of the MAMA detectors for the European Space Agency/NASA Solar and Heliosphere Observatory (SOHO) mission. This paper describes the different configurations of the characterization facility and outlines the SOHO MAMA characterization procedures. Title: Performance characteristics of the MAMA detectors for the SUMER instrument on the SOHO Mission Authors: Timothy, J. Gethyn; Bergamini, Paolo; Berger, Thomas E.; Bumala, Robert W.; Slater, David C. Bibcode: 1993SPIE.2006...69T Altcode: We have initiated the characterizations of the Multi-Anode Microchannel Array (MAMA) detector systems for the European Space Agency/NASA Solar and Heliospheric Observatory (SOHO) mission. In this paper we briefly review the configurations of the SOHO MAMA detectors and describe their expected performance characteristics based on the results of characterizations of the curved-channel microchannel plates and of the initial characterization of the first engineering model detector system for the Solar Ultraviolet Measurements of Emitted Radiation instrument. Title: Spectroscopic characterization of the EUV toroidal grating for the HiRES rocket Authors: Naletto, Giampiero; Perin, Marco; Tondello, Giuseppe; Villoresi, Paolo; Contarini, Gabriella; Timothy, J. Gethyn; Bergamini, Paolo; Berger, Thomas E. Bibcode: 1993SPIE.2006...22N Altcode: The evaluation of the performances of a toroidal grating for the high-resolution EUV spectroheliometer (HiRES) has been realized. This is a holographically ruled grating operating in a normal incidence Rowland configuration at the 510 - 630 angstroms spectral range. An analysis of the grating resolution performances has been realized by means of a scintillator- intensifier-CCD detector showing very good results. Also a measurement of the grating diffraction efficiency has been performed, showing on the contrary a value lower than the predicted one. Title: The High Resolution Extreme-Ultraviolet Spectroheliometer (HiRES) Experiment: Capabilities and Observing Goals Authors: Berger, T. E.; Timothy, J. G.; Walker, A. B. C., Jr.; Jain, S. K.; Saxena, A. K.; Bhattacharyya, J. C.; Huber, M. C. E.; Tondello, G.; Naletto, G. Bibcode: 1993BAAS...25.1209B Altcode: No abstract at ADS Title: HiRES: High Resolution Extreme Ultraviolet Spectroheliometer. Authors: Berger, T.; Bergamini, P.; Kirby, H.; Timothy, J. G.; Walker, A. B. C.; Bhattacharyya, J. C.; Jain, S. K.; Saxena, A. K.; Huber, M. C. E.; Naletto, G.; Tondello, G. Bibcode: 1993uxrs.conf..289B Altcode: 1993uxsa.conf..289B The HiRES sounding rocket payload is designed to obtain very high spatial, spectral, and temporal resolution images of the solar chromospheric and coronal plasmas in the extreme ultraviolet (EUV) wavelength range from 500 to 650 Å. The instrument consists of a 450 mm f/15 Gregorian telescope feeding a 1-m normal incidence stigmatic spectrometer. The stigmatic spectrometer utilizes a toroidal diffraction grating formed by a unique elastic substrate deformation technique in order to achieve simultaneous spatial and spectral focusing at two points on the detector plane. Spatial resolution on the order of 0.4 arcsecond across a 3×3 arcmin2 field of view is obtained. Temporal resolution of the order of milliseconds is achieved by the use of an advanced imaging Multi-Anode Microchannel Array (MAMA) detector. A hydrogen-alpha 6562.8 Å camera and a 0.25-m EUV solar irradiance spectrometer are also included in the payload. Title: An imaging extreme ultraviolet spectrometer. Authors: Bergamini, P.; Berger, T. E.; Giaretta, G.; Huber, M. C. E.; Naletto, G.; Timothy, J. G.; Tondello, G. Bibcode: 1993uxrs.conf..285B Altcode: 1993uxsa.conf..285B A laboratory extreme ultraviolet (EUV) imaging spectrometer has been fabricated and tested. This instrument is used to test and to characterize toroidal gratings like those which will be employed in the high-resolution spectroheliometer (HiRES) configured for flight on a sounding rocket. The imaging spectrometer will be used also for characterization and calibration of Multi Anode Microchannel Array (MAMA) detectors foreseen on the ESA/NASA Solar Heliospheric Observatory (SOHO) satellite. The spectrometer employs a concave toroidal grating illuminated at normal incidence in a 1 meter Rowland circle mounting: high efficiency is achieved because the grating is the only reflecting surface. The grating is able to produce stigmatic images over a wavelength range of about 100 Å or 200 Å centered respectively around 600 Å or 1200 Å. The results of the initial imaging tests and the measurements carried out are presented and discussed. Title: Interferometric methods for assessment of toroidal diffraction grating performance Authors: Baker, Phillip; Bergamini, Paolo; Berger, Tom; Timothy, J. G. Bibcode: 1993SPIE.1742..453B Altcode: The measurement of the shape and optical performance of toroidal mirrors has always presented a challenge to the manufacturer and user of these types of optical elements. This report presents a technique for evaluating the complex shape and optical performance of long radius toroidal mirrors that are to be used in the EUV. The measurement techniques will be discussed and examples given. Interferometric analysis will be presented. Performance spot diagrams and MTF analysis will be discussed. Manufacturing techniques will be evaluated with respect to the application of more definitive measurement technology. Title: Design and test of a High-Resolution EUV Spectroheliometer Authors: Berger, Thomas E.; Timothy, J. G.; Walker, Arthur B. C., Jr.; Kirby, Helen; Morgan, Jeffrey S.; Jain, Surendra K.; Saxena, Ajay K.; Bhattacharyya, Jagadish C.; Huber, Martin C. E.; Tondello, Giuseppe Bibcode: 1992SPIE.1546..446B Altcode: 1992SPIE.2011..446B The HiRES High-Resolution EUV Spectroheliometer is a sounding rocket instrument yielding very high spatial, spectral, and temporal resolution images of the solar outer atmosphere, on the basis of a 45-cm Gregorian telescope feeding a normal-incidence stigmatic EUV spectrometer with imaging multianode microchannel-array detector system, as well as an IR spectrometer with imaging CCD detector system. Attention is given to the expected performance of this system, including the effects of vibrational misalignments due to the sounding rocket flight environment. Title: HiRES: a high-resolution stigmatic extreme ultraviolet spectroheliometer for sudies of the fine-scale structure of the solar chromosphere, transition region, and corona. Authors: Timothy, J. G.; Berger, Thomas E.; Morgan, Jeffrey S.; Walker, Arthur B. C., Jr.; Jain, Surendra K.; Saxena, Ajay K.; Bhattacharyya, Jagadish C.; Huber, Martin C. E.; Tondello, Giuseppe; Naletto, Giampiero Bibcode: 1991OptEn..30.1142T Altcode: The authors describe the design of a high-resolution stigmatic extreme-ultraviolet spectroheliometer, which consists of a 45 cm Gregory telescope coupled to a spectrometer employing a single toroidal diffraction grating in a normal-incidence Rowland circle mounting and an imaging pulse-counting multianode microchannel array (MAMA) detector system. The spectroheliometer will produce spatially resolved spectra of the chromosphere, transition region, and corona with an angular resolution of 0.4″or better, a spectral resolution λ/Δλ of about 104 in first order, and a temporal resolution of the order of seconds. Because of the geometric fidelity of the MAMA detector system, the spectroheliometer will be able to determine Doppler shifts to a resolution of at least 2 mÅ at wavelengths near 600Å (≡1.0 km s-1), depending on the level of the accumulated signal. Title: High-resolution stigmatic EUV spectroheliometer for studies of the fine scale structure of the solar chromosphere, transition region, and corona Authors: Timothy, J. Gethyn; Berger, Thomas E.; Morgan, Jeffrey S.; Walker, Arthur B.; Bhattacharyya, Jagadish C.; Jain, Surendra K.; Saxena, Ajay K.; Huber, Martin C.; Tondello, Giuseppe; Naletto, Giampiero Bibcode: 1991SPIE.1343..350T Altcode: No abstract at ADS