Author name code: muglach ADS astronomy entries on 2022-09-14 author:"Muglach, Karin" ------------------------------------------------------------------------ Title: Evaluating current methods for establishing magnetic connectivity across the solar atmosphere Authors: Pinto, Rui; Kouloumvakos, Athanasios; Linker, Jon; Arge, Charles; Reiss, Martin; Muglach, Karin; Ko, Yuan-Kuen; Henney, Carl J. Bibcode: 2022cosp...44.3504P Altcode: Establishing magnetic connectivity from the solar surface to any point in the interplanetary space is a key challenge in today's space physics, fundamental for the determination of causal links between different types of solar and heliospheric phenomena that take place at large distances from each other. Solar Orbiter and Parker Solar Probe constitute a landmark in terms of connectivity science. They led to collective efforts to relate remote observations to in-situ data (traditionally studied by different communities) from one or more spacecraft, and to build tools and methods that establish connectivity systematically. We report on the progresses of the ISWAT team S2-05 on the design of a set of case studies meant to cover a diverse set of connectivity scenarios that can be studied using different combinations of models and datasets, while trying to maximize the number of possible diagnostics. Title: Photospheric Flow Fields in a Coronal Bright Point Authors: Peat, Aaron; Labrosse, Nicolas; Muglach, Karin Bibcode: 2022cosp...44.2565P Altcode: The relationship between the flows in the photosphere and the migration of magnetic polarity patches leading to a coronal bright point is investigated. As seen in SDO/AIA images the formation of this coronal bright point began end of day on 2017-09-24, with the event peaking at approximately 10.00 on 2017-09-25, and ending 2017-09-27. In all, the evolution of the bright point was followed over about 3 days. We employ Fourier Local Correlation Tracking (FLCT) to recover the photospheric flow fields in HMI Intensity images around the area in which the bright point forms. Then, using the flow vectors produced by FLCT, we investigate the relationship between these photospheric flow fields and the flux emergence, and the effect they have on the formation and evolution of the coronal bright point. Title: Unifying the validation of ambient solar wind models in the community Authors: Reiss, Martin; Muglach, Karin; Chakraborty, Shibaji Bibcode: 2022cosp...44.3505R Altcode: To make progress in space weather research and awareness, we need international community strategies and procedures to assess our modeling assets. Here we present the actions of the Ambient Solar Wind Validation Team embedded in the COSPAR ISWAT initiative. Our team's mission is to provide the space weather community with an assessment of the state-of-the-art in solar wind forecasting. To do so, we develop an open online platform that allows the community to test the quality of solar wind models with unified metrics and document progress over time. We discuss challenges in realizing our objectives, present a status update, and outline future perspectives. We furthermore highlight community activities in the ISWAT initiative that complement our efforts by addressing key science questions related to the solar magnetic field and solar wind origins. Title: Velocities of an Erupting Filament Authors: Wang, Shuo; Jenkins, Jack M.; Muglach, Karin; Martinez Pillet, Valentin; Beck, Christian; Long, David M.; Choudhary, Debi Prasad; McAteer, James Bibcode: 2022ApJ...926...18W Altcode: 2021arXiv211107830W Solar filaments exist as stable structures for extended periods of time before many of them form the core of a coronal mass ejection (CME). We examine the properties of an erupting filament on 2017 May 29-30 with high-resolution He I 10830 Å and Hα spectra from the Dunn Solar Telescope, full-disk Dopplergrams of He I 10830 Å from the Chromospheric Telescope, and EUV and coronograph data from SDO and STEREO. Pre-eruption line-of-sight velocities from an inversion of He I with the HAZEL code exhibit coherent patches of 5 Mm extent that indicate counter-streaming and/or buoyant behavior. During the eruption, individual, aligned threads appear in the He I velocity maps. The distribution of velocities evolves from Gaussian to strongly asymmetric. The maximal optical depth of He I 10830 Å decreased from τ = 1.75 to 0.25, the temperature increased by 13 kK, and the average speed and width of the filament increased from 0 to 25 km s-1 and 10 to 20 Mm, respectively. All data sources agree that the filament rose with an exponential acceleration reaching 7.4 m s-2 that increased to a final velocity of 430 km s-1 at 22:24 UT; a CME was associated with this filament eruption. The properties during the eruption favor a kink/torus instability, which requires the existence of a flux rope. We conclude that full-disk chromospheric Dopplergrams can be used to trace the initial phase of on-disk filament eruptions in real time, which might potentially be useful for modeling the source of any subsequent CMEs. Title: Information Infrastructure for the Validation of Ambient Solar Wind Models Authors: Muglach, Karin; Reiss, Martin; Wiegand, Chiu; Mullinix, Richard; Kuznetsova, Maria Bibcode: 2021AGUFMSH44C..05M Altcode: Over the past decades, many empirical and physics-based numerical models for predicting the evolving ambient solar wind flow at Earth have been developed. To evaluate the predictive skill of these models, they are usually compared with solar wind measurements taken by in-situ spacecraft. The activities of the Ambient Solar Wind Validation Team embedded in the COSPAR ISWAT initiative are centered around the validation of these solar wind models. An important part of such a model-observation comparison is keeping track of versions of models and model runs via their metadata. In this presentation, we show our ambient solar wind validation platform that we have set up using the Comprehensive Assessment of Models and Events using Library Tools (CAMEL) framework provided by the Community Coordinated Modeling Center (the figure included in this abstract shows an early version of CAMEL). We discuss the CAMEL framework as well as other information infrastructure that we utilize to make this community validation effort possible. Title: The Observational Uncertainty of Coronal Hole Boundaries in Automated Detection Schemes Authors: Reiss, Martin; Muglach, Karin; Moestl, Christian; Arge, Charles; Bailey, Rachel; Delouille, Veronique; Garton, Tadhg; Hamada, Amr; Hofmeister, Stefan; Illarionov, Egor; Jarolim, Robert; Kirk, Michael; Kosovichev, Alexander; Krista, Larisza; Lee, Sangwoo; Lowder, Chris; MacNeice, Peter; Veronig, Astrid Bibcode: 2021AGUFMSH15G2083R Altcode: Solar coronal holes are the observational manifestation of the solar magnetic field open to the heliosphere and are of pivotal importance for understanding the origin and acceleration of the solar wind. Space missions such as the Solar Dynamics Observatory now allow us to observe coronal holes in unprecedented detail. Instrumental effects and other factors, however, pose a challenge to automated detection of coronal holes in solar imagery. The science community addresses these challenges with a variety of detection schemes. Until now, scant attention has been paid to assessing the disagreement between these schemes. Here we present the first comprehensive comparison of widely-applied automated detection schemes in solar and space science. By tying together scientific expertise worldwide, we study a coronal hole observed by the Atmospheric Imaging Assembly instrument on 2018 May 30. We find that the choice of detection scheme significantly affects the location of the coronal hole boundary. Depending on the detection scheme, the physical properties of the coronal hole including the area, mean intensity, and mean magnetic field strength vary by a factor of up to 4.5 between the maximum and minimum values. This presentation discusses the implications of these findings for coronal hole research from the past decade. We also outline future strategies on how to use our results to diagnose and improve coronal magnetic field models. Title: Magnetic Field Curvature In A Filament Channel Derived From Oscillation Measurements And MHD Modeling Authors: Kucera, T. A.; Luna, M.; Torok, T.; Muglach, K.; Downs, C.; Sun, X.; Thompson, B.; Karpen, J.; Gilbert, H. Bibcode: 2021AAS...23811306K Altcode: We have used measurements of repeated large amplitude longitudinal oscillations (LALOs) in an active region filament to diagnose the curvature of the magnetic field in the filament channel and compared the results with predictions of an MHD flux-rope model based on magnetograms of the region. In May and June of 2014 Active Region 12076 exhibited a complex of filaments undergoing repeated oscillations over the course of twelve days. The central filament channel exhibited emerging and then canceling magnetic flux that resulted in multiple activations, filament eruptions, and eight oscillation events, which we analyzed using GONG H-alpha data. Luna and Karpen (2012) model LALOs as oscillations of magnetized filament plasma moving along dipped magnetic field lines with gravity as a restoring force. Under this model the period of these oscillations can be used to estimate the curvature of the magnetic field in the location of the filament threads. Utilizing this, we find that the measured periods in the central filament ranging from 34-74 minutes should correspond to magnetic field curvatures of about 30-136 Mm. We also derive radii of curvature for the central filament channel using a flux-rope model that is based on an SDO/HMI magnetogram of the region. The rope is constructed using the analytic expressions by Titov et al. (2018) and then numerically relaxed towards a force-free state in the zero-beta MHD approximation, where gravity and thermal pressure are neglected. For comparison, we also employ a nonlinear force-free field (NLFFF) extrapolation of the active region. We compare the results of these different ways of attempting to determine the field in the filament channel. Title: The Observational Uncertainty of Coronal Hole Boundaries in Automated Detection Schemes Authors: Reiss, Martin A.; Muglach, Karin; Möstl, Christian; Arge, Charles N.; Bailey, Rachel; Delouille, Véronique; Garton, Tadhg M.; Hamada, Amr; Hofmeister, Stefan; Illarionov, Egor; Jarolim, Robert; Kirk, Michael S. F.; Kosovichev, Alexander; Krista, Larisza; Lee, Sangwoo; Lowder, Chris; MacNeice, Peter J.; Veronig, Astrid; Cospar Iswat Coronal Hole Boundary Working Team Bibcode: 2021ApJ...913...28R Altcode: 2021arXiv210314403R Coronal holes are the observational manifestation of the solar magnetic field open to the heliosphere and are of pivotal importance for our understanding of the origin and acceleration of the solar wind. Observations from space missions such as the Solar Dynamics Observatory now allow us to study coronal holes in unprecedented detail. Instrumental effects and other factors, however, pose a challenge to automatically detect coronal holes in solar imagery. The science community addresses these challenges with different detection schemes. Until now, little attention has been paid to assessing the disagreement between these schemes. In this COSPAR ISWAT initiative, we present a comparison of nine automated detection schemes widely applied in solar and space science. We study, specifically, a prevailing coronal hole observed by the Atmospheric Imaging Assembly instrument on 2018 May 30. Our results indicate that the choice of detection scheme has a significant effect on the location of the coronal hole boundary. Physical properties in coronal holes such as the area, mean intensity, and mean magnetic field strength vary by a factor of up to 4.5 between the maximum and minimum values. We conclude that our findings are relevant for coronal hole research from the past decade, and are therefore of interest to the solar and space research community. 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: The Photospheric Footpoints of Solar Coronal Hole Jets Authors: Muglach, K. Bibcode: 2021ApJ...909..133M Altcode: We study the photospheric footpoints of a set of 35 coronal jets in a coronal hole as observed by Hinode/EIS. We use SDO/AIA data to coalign the spectroscopic EIS data with SDO/HMI line-of-sight magnetograms and calculate the plane-of-sky flow field using local correlation tracking (LCT) on SDO/HMI white light images. The jets are put into categories according to the changes observed in the photospheric magnetic flux at the footpoints of the coronal bright point where the jets originate: flux cancellation, complex flux changes (flux appearance/emergence and cancellation), and no flux changes. We also present three jets in detail. Observed magnetic flux evolution, LCT flow field structure and location of the jet footpoints at supergranular boundaries do not support the flux emergence scenario used in most jet simulations and are also not consistent with a rotational photospheric driver. Detailed numerical jet simulations using our observed photospheric features, in particular converging flows and flux cancellation do not currently exist, although such models would provide a realistic eruptive event scenario. Title: Improving Understanding and Assessment of the Ambient Solar Wind Authors: Reiss, Martin; Moestl, Christian; Linker, Jon; Mullinix, Richard; Rastaetter, Lutz; Temmer, Manuela; Arge, Charles; MacNeice, Peter; Wiegand, Chiu; Muglach, Karin; Ko, Kuen Bibcode: 2021cosp...43E2398R Altcode: The Sun's magnetic field drives the evolving ambient solar wind flow and the magnetic field embedded within it. Thus, studying the magnetic field configuration in the solar atmosphere is of crucial importance for improving our understanding of and ultimately predicting space weather from Sun to Earth. Coronal holes are regions of low intensity emission in EUV and X-ray images. Coronal holes are closely associated with open magnetic field lines, along which the solar wind accelerates to supersonic speeds. Therefore, they play a central role in shaping the structure of the heliosphere and defining key properties in interplanetary space, such as the solar wind bulk speed, magnetic field strength, and field orientation. Answering vital research questions related to the ambient solar wind requires an interdisciplinary strategy and the coordinated collaboration of international partners. Here we present the COSPAR ISWAT activities for improving the understanding and assessment of the evolving ambient solar wind flow embedded in the 'Coronal Hole Boundary Working Team' and the 'Ambient Solar Wind Validation Team'. Specifically, we present our progress in evaluating the uncertainty of coronal hole boundary locations in solar observations, and our progress in establishing an online hub for validation of ambient solar wind models. In context, we demonstrate the first application of a new online platform enabling developers and end-users to directly assess the quality of state-of-the-art solar wind model solutions. To conclude, we present the objectives, current status and roadmaps of both action teams, and discuss the main challenges we face in the realization of our objectives. Title: Activities related to the COSPAR ISWAT Cluster: Ambient Solar Magnetic Field, Heating and Spectral Irradiance Authors: Reiss, Martin; Pevtsov, Alexei; Linker, Jon; Pinto, Rui; Arge, Charles; Muglach, Karin; Henney, Carl J. Bibcode: 2021cosp...43E2413R Altcode: The understanding of the magnetic field configuration in the solar atmosphere is of crucial importance for improving the modelling and ultimately the prediction of space weather from Sun to Earth. The magnetic field provides the energy source that heats the solar corona and accelerates the solar wind, and it also defines the structure of the heliosphere. However, many related unresolved questions require an interdisciplinary strategy and the coordinated cooperation of international partners. Here we present the activities of the 'Ambient Solar Magnetic Field, Heating and Spectral Irradiance' cluster embedded in the COSPAR ISWAT initiative. The action teams in this cluster will focus on critical scientific challenges in the space weather community related to the construction of global solar magnetic field maps, use of vector field synoptic maps for applied space weather modelling and research, magnetic connectivity from the surface of the Sun to any point in interplanetary space, magnetic topology of open field lines along which solar wind flows accelerate to supersonic speeds, and the solar spectral irradiance driving ionization and heating in the Earth's upper atmosphere. We will outline the objectives of the individual action teams and present the current status and roadmaps. To encourage the formation of new action teams, we will also discuss additional challenges that should be addressed by the space weather community. Title: The COSPAR ISWAT initiative for open validation analysis for models of the evolving ambient solar wind Authors: Reiss, Martin; Kuznetsova, Maria; Mullinix, Richard; Rastaetter, Lutz; Temmer, Manuela; MacNeice, Peter; Wiegand, Chiu; Muglach, Karin Bibcode: 2021cosp...43E2363R Altcode: Validation analysis plays a critical role in applied space weather research and prediction. First and foremost to inform developers and users of space weather models about the strengths and weaknesses of the models, and also to provide an unbiased assessment of progress over time. Here we present the activities of the Ambient Solar Wind Validation Team embedded in the COSPAR ISWAT initiative. The objective of this action team is to establish an online hub for validation analysis of ambient solar wind models in correspondence with the space weather community, allowing developers and end-users to directly assess the quality of state-of-the-art model solutions. To this end, we choose and agree on a set of comprehensive validation metrics reflecting the community needs and integrate them into the existing Comprehensive Assessment of Models and Events using Library Tools (CAMEL) web application hosted by NASA's Community Coordinated Modelling Center. CAMEL is an interactive visualization tool allowing developers and users to compare space weather and space science model output to observations. Specifically, we make use of CAMEL to quantitatively assess the relationship between state-of-the-art solar wind model solutions and observational data in terms of point-to-point statistics and more advanced event-based validation measures. In this presentation, we will demonstrate the first application of the new online platform with examples of state-of-the-art model solutions. We will also discuss the main challenges we face in the realization of our objectives, and present the current status and the roadmap of the action team. Title: An Adaptive Prediction System for Specifying Solar Wind Conditions Near the Sun Authors: Reiss, M.; MacNeice, P. J.; Muglach, K.; Arge, C. N.; Moestl, C.; Riley, P.; Bailey, R.; Hinterreiter, J.; Weiss, A.; Owens, M. J.; Henney, C. J.; Amerstorfer, U.; Amerstorfer, T. Bibcode: 2020AGUFMSM047..01R Altcode: Understanding Earth's space weather environment requires a clear picture of the evolving ambient solar wind flow. Critical scientific goals in space weather research and prediction are to develop, implement and optimize approaches for specifying the large-scale solar wind conditions near the Sun. Here we present an adaptive prediction system that fuses information from in situ measurements in the vicinity of Earth into solar wind models to better inform the inner boundary conditions of heliospheric models. By doing so, we attempt to advance the predictive abilities of established solar wind models such as the Wang-Sheeley-Arge approach. We validate the resulting solar wind predictions for the years 2006 to 2015. The adaptive prediction system improves all the coronal and heliospheric model combinations investigated by around 15 to 20 percent in terms of established validation metrics. We discuss why this is the case, and conclude that our findings have important implications for future developments in space weather research and prediction. Title: Filament Oscillations in Active Region 12076 Authors: Kucera, T. A.; Muglach, K.; Luna Bennasar, M.; Karpen, J.; Thompson, B.; Gilbert, H. Bibcode: 2020AAS...23633004K Altcode: We present an analysis of repeated large amplitude longitudinal oscillations (LALO) in filaments in Active Region 12076 in May and June of 2014. Most of the oscillations were associated with a region of emerging and then canceling magnetic flux that resulted in multiple activations and filament eruptions. We analyze twelve separate oscillations that occur in a complex of filaments in the active region over twelve days. Luna and Karpen (2012) model LALO in filaments oscillations of magnetized filament plasma moving along dipped magnetic field lines with gravity as a restoring force. Under this model the period of these oscillations can be used to estimate the curvature of the magnetic field in the location of the filament, providing observationally derived values to compare with models of the magnetic field in the active region corona. Periods ranged from 26-74 minutes, corresponding to magnetic field curvatures of about 20-130 Mm. Title: Magnetic Structure of an Erupting Filament Authors: Wang, Shuo; Jenkins, Jack M.; Martinez Pillet, Valentin; Beck, Christian; Long, David M.; Prasad Choudhary, Debi; Muglach, Karin; McAteer, James Bibcode: 2020ApJ...892...75W Altcode: 2020arXiv200202104W The full 3D vector magnetic field of a solar filament prior to eruption is presented. The filament was observed with the Facility Infrared Spectropolarimeter at the Dunn Solar Telescope in the chromospheric He I line at 10830 Å on 2017 May 29 and 30. We inverted the spectropolarimetric observations with the Hanle and Zeeman Light code to obtain the chromospheric magnetic field. A bimodal distribution of field strength was found in or near the filament. The average field strength was 24 Gauss, but prior to the eruption we find the 90th percentile of field strength was 435 Gauss for the observations on May 29. The field inclination was about 67° from the solar vertical. The field azimuth made an angle of about 47°-65° to the spine axis. The results suggest an inverse configuration indicative of a flux rope topology. He I intensity threads were found to be coaligned with the magnetic field direction. The filament had a sinistral configuration as expected for the southern hemisphere. The filament was stable on 2017 May 29 and started to rise during two observations on May 30, before erupting and causing a minor coronal mass ejection. There was no obvious change of the magnetic topology during the eruption process. Such information on the magnetic topology of erupting filaments could improve the prediction of the geoeffectiveness of solar storms. Title: Forecasting the Ambient Solar Wind with Numerical Models. II. An Adaptive Prediction System for Specifying Solar Wind Speed near the Sun Authors: Reiss, Martin A.; MacNeice, Peter J.; Muglach, Karin; Arge, Charles N.; Möstl, Christian; Riley, Pete; Hinterreiter, Jürgen; Bailey, Rachel L.; Weiss, Andreas J.; Owens, Mathew J.; Amerstorfer, Tanja; Amerstorfer, Ute Bibcode: 2020ApJ...891..165R Altcode: 2020arXiv200309336R The ambient solar wind flows and fields influence the complex propagation dynamics of coronal mass ejections in the interplanetary medium and play an essential role in shaping Earth's space weather environment. A critical scientific goal in the space weather research and prediction community is to develop, implement, and optimize numerical models for specifying the large-scale properties of solar wind conditions at the inner boundary of the heliospheric model domain. Here we present an adaptive prediction system that fuses information from in situ measurements of the solar wind into numerical models to better match the global solar wind model solutions near the Sun with prevailing physical conditions in the vicinity of Earth. In this way, we attempt to advance the predictive capabilities of well-established solar wind models for specifying solar wind speed, including the Wang-Sheeley-Arge model. In particular, we use the Heliospheric Upwind eXtrapolation (HUX) model for mapping the solar wind solutions from the near-Sun environment to the vicinity of Earth. In addition, we present the newly developed Tunable HUX (THUX) model, which solves the viscous form of the underlying Burgers equation. We perform a statistical analysis of the resulting solar wind predictions for the period 2006-2015. The proposed prediction scheme improves all the investigated coronal/heliospheric model combinations and produces better estimates of the solar wind state at Earth than our reference baseline model. We discuss why this is the case and conclude that our findings have important implications for future practice in applied space weather research and prediction. Title: Tracking supergranulation near the poles with SDO/HMI Authors: Attié, R.; Kirk, M. S.; Tremblay, B.; Muglach, K.; Hess Webber, S. A.; Pesnell, W. D.; Thompson, B. J. Bibcode: 2019AGUFMSH13B..01A Altcode: Due to the spherical curvature of the Sun, solar observers suffer from an increasing loss of resolution as we move away from the solar equator. Thus knowledge of the photospheric flows near the poles has eluded the scope of traditional flow tracking algorithms that are using granules as tracers of the underlying flows. Using the new "Balltracking" framework which we adapted to the observations from SDO/HMI, we present an unprecedented analysis of the horizontal flow fields at latitudes beyond +/- 60 degrees. The flow fields are derived every 4 hours at a spatial resolution of 4 Mm. Using flow segmentation techniques, we extract geometric and spectral information on the supergranular cells and compare them with those of the supergranulation at lower latitude. The correlation with the dynamics of moving magnetic features is also investigated. Title: Searching for a Boundary Layer as a Source of the Slow Solar Wind Authors: Ko, Y. K.; Muglach, K.; Riley, P.; Wang, Y. M. Bibcode: 2019AGUFMSH41F3330K Altcode: Recent investigations in the solar wind plasma and magnetic field characteristics indicate a likely existence of a "boundary layer" where the slow solar wind originates from. Such a boundary layer resides at the coronal hole boundary where the open field lines emanating from it expand super-radially into the corona. We select two adjacent coronal holes that are the sources of two consecutive solar wind streams measured by ACE. One is a low-latitude extension of the north polar coronal hole that past the central meridian on August 18, 2015, and the other is an equatorial coronal hole that past the central meridian on August 20. We use data from SDO/AIA, SDO/HMI and Hinode/EIS in combination with PFSS and 3D MHD models to investigate the evolution of the coronal and magnetic field properties at the boundary of these coronal holes and search for signatures of such a boundary layer. Title: Assessing the uncertainty of coronal hole boundary locations Authors: Reiss, M.; MacNeice, P. J.; Muglach, K.; Kirk, M. S.; Arge, C. N.; Moestl, C. Bibcode: 2019AGUFMSM31C3182R Altcode: The ambient solar wind flows, and the magnetic fields embedded within it, are driven by the Sun's magnetic field. Thus, studying the magnetic field configuration in the solar atmosphere is of key importance for improving understanding and ultimately predicting Earth's space weather environment. The configuration of open magnetic field lines, commonly known as coronal holes, is especially important for predicting key properties in the interplanetary space such as solar wind bulk speed, magnetic field strength, and field orientation. In addition, the dynamic evolution of coronal hole boundaries is understood as having a critical role in the origin of the slow solar wind. Despite the importance of these features there has been no systematic analysis of the reliability of established coronal hole detection techniques. The objectives of this action team are threefold: First, to study and compare different coronal hole detection techniques with open communication with the space weather community. Second, to develop strategies to quantitatively assess the spatial and temporal uncertainty of coronal hole boundary locations. Third, to use this information to further improve the predictive capabilities of numerical models of the evolving ambient solar wind. We will discuss challenges towards the realization of these objectives and present the current status and the roadmap of the action team. Title: The life of coronal bright points Authors: Muglach, Karin; Leisner, Andrew Bibcode: 2019AAS...23411703M Altcode: Coronal bright points are small-scale magnetic regions found all over the solar disk. They are visible in coronal emission lines which sample plasma at around 1-2 MK. In this study we follow the complete lifetime of several coronal bright points, from the time they appear in the SDO/AIA coronal filtergrams to the time they fade again into the quiet solar background emission. In addition to the hot coronal emission, lower temperature chromospheric filtergrams (e.g. AIA 304 Å) sometimes show the formation of dark absorption structures similar to filaments. From SDO/HMI we can get the accompanying evolution of the photospheric magnetic flux density and also calculate the plane-of-sky plasma flow field using local correlation tracking. Most of the coronal bright points show some jet activity during their lifetime and these data allow to us to study both the energy buildup of the coronal bright point and the initiation of the jets. Title: Precursors of magnetic flux emergence in the moat flows of active region AR12673 Authors: Attie, Raphael; Kirk, Michael; Thompson, Barbara; Muglach, Karin; Norton, Aimee Bibcode: 2018csc..confE..34A Altcode: We report on observations of magnetic disturbances in active region AR12673 between Sep. 1 and Sep. 3, 2017 seen as a disruption of the moat flow several hours before the onset of strong flux emergence near the main sunspot. The moat flow is commonly known as a radially oriented strong outflow of photospheric plasma surrounding sunspots which ends abruptly and thus shapes an annular pattern around the penumbra. Using highly accurate methods of tracking this photospheric flow applied to SDO/HMI data, we are able to describe the evolution of the moat surrounding the main sunspot of AR 12673. We find that several hours before the emergence of strong magnetic flux near the main sunspot the moat boundaries are broken at these very same locations. This behavior is observed both on Sep. 1st and Sep. 3rd. There is no such behavior observed in the absence of flux emergence. These observational results pose the question of how often they occur in other active regions and whether the disruption of the moat flow might be, like in this case, an indication of impending enhanced magnetic activity or simply a coincidental event. Title: GONG Catalog of Solar Filament Oscillations Near Solar Maximum Authors: Luna, M.; Karpen, J.; Ballester, J. L.; Muglach, K.; Terradas, J.; Kucera, T.; Gilbert, H. Bibcode: 2018ApJS..236...35L Altcode: 2018arXiv180403743L We have cataloged 196 filament oscillations from the Global Oscillation Network Group Hα network data during several months near the maximum of solar cycle 24 (2014 January-June). Selected examples from the catalog are described in detail, along with our statistical analyses of all events. Oscillations were classified according to their velocity amplitude: 106 small-amplitude oscillations (SAOs), with velocities <10 {km} {{{s}}}-1, and 90 large-amplitude oscillations (LAOs), with velocities >10 {km} {{{s}}}-1. Both SAOs and LAOs are common, with one event of each class every two days on the visible side of the Sun. For nearly half of the events, we identified their apparent trigger. The period distribution has a mean value of 58 ± 15 minutes for both types of oscillations. The distribution of the damping time per period peaks at τ/P = 1.75 and 1.25 for SAOs and LAOs, respectively. We confirmed that LAO damping rates depend nonlinearly on the oscillation velocity. The angle between the direction of motion and the filament spine has a distribution centered at 27° for all filament types. This angle agrees with the observed direction of filament-channel magnetic fields, indicating that most of the cataloged events are longitudinal (i.e., undergo field-aligned motions). We applied seismology to determine the average radius of curvature in the magnetic dips, R ≈ 89 Mm, and the average minimum magnetic field strength, B ≈ 16 G. The catalog is available to the community online and is intended to be expanded to cover at least 1 solar cycle. Title: Advance detection of strong photospheric flux emergence revealed by disruption of moat flows Authors: Attié, Raphael; Thompson, Barbara J.; Muglach, Karin; Norton, Aimee Ann Bibcode: 2018tess.conf30602A Altcode: We report on observations of precursors of magnetic disturbances in AR 12673 seen as a disruption of the moat flow several hours before the onset of strong flux emergence near the main sunspot. The moat flow is commonly known as a radially oriented strong outflow of photospheric plasma surrounding sunspots which ends abruptly and thus shapes an annular pattern around the penumbra. Using highly accurate methods of tracking this photospheric flow applied to SDO/HMI data, we are able to describe the evolution of the moat surrounding the main sunspot of AR 12673. We find that several hours before the emergence of strong magnetic flux near the main sunspot the moat boundaries are broken at these very same locations. Because we detect this specific behavior both on Sep. 1st and Sep. 3rd, our observations suggest that the disruption of the moat flow is a precursor of the enhanced magnetic activity which, in this case, led to the strong flaring activity starting on Sep 6th. This study is part of a broader statistical survey that aims at characterizing emerging active regions. In light of these new observations, our survey will also determine to what extent such a disruption of the moat flow is followed by strong flux emergence around sunspots, i.e., is this a peculiar response specific to AR 12673, or is it a characteristic disturbance defining a subset of active regions prone to flaring activity? Title: Space Weather Research and Forecasting Capabilities at the Community Coordinated Modeling Center (CCMC) Authors: Collado-Vega, Y. M.; Kuznetsova, M.; Mays, L.; Pulkkinen, A.; Zheng, Y.; Muglach, K.; Thompson, B.; Chulaki, A.; Taktakishvili, A.; CCMC Team Bibcode: 2018LPICo2063.3090C Altcode: The Community Coordinated Modeling Center (CCMC) supports and enables the research and development of the latest and future space weather models and facilitates the deployment of the latest advances in research of space weather operations. Title: CCMC: bringing space weather awareness to the next generation Authors: Chulaki, A.; Muglach, K.; Zheng, Y.; Mays, M. L.; Kuznetsova, M. M.; Taktakishvili, A.; Collado-Vega, Y. M.; Rastaetter, L.; Mendoza, A. M. M.; Thompson, B. J.; Pulkkinen, A. A.; Pembroke, A. D. Bibcode: 2017AGUFMSH21A2635C Altcode: Making space weather an element of core education is critical for the future of the young field of space weather. Community Coordinated Modeling Center (CCMC) is an interagency partnership established to aid the transition of modern space science models into space weather forecasting while supporting space science research. Additionally, over the past ten years it has established itself as a global space science education resource supporting undergraduate and graduate education and research, and spreading space weather awareness worldwide. A unique combination of assets, capabilities and close ties to the scientific and educational communities enable our small group to serve as a hub for rising generations of young space scientists and engineers. CCMC offers a variety of educational tools and resources publicly available online and providing access to the largest collection of modern space science models developed by the international research community. CCMC has revolutionized the way these simulations are utilized in classrooms settings, student projects, and scientific labs. Every year, this online system serves hundreds of students, educators and researchers worldwide. Another major CCMC asset is an expert space weather prototyping team primarily serving NASA's interplanetary space weather needs. Capitalizing on its unique capabilities and experiences, the team also provides in-depth space weather training to hundreds of students and professionals. One training module offers undergraduates an opportunity to actively engage in real-time space weather monitoring, analysis, forecasting, tools development and research, eventually serving remotely as NASA space weather forecasters. In yet another project, CCMC is collaborating with Hayden Planetarium and Linkoping University on creating a visualization platform for planetariums (and classrooms) to provide simulations of dynamic processes in the large domain stretching from the solar corona to the Earth's upper atmosphere, for near real-time and historical space weather events. Title: Large-Amplitude Oscillations as a Probe of Solar Prominences Authors: Luna Bennasar, M.; Karpen, J. T.; Gilbert, H. R.; Kucera, T. A.; Muglach, K. Bibcode: 2016AGUFMSH41E..01L Altcode: Large-amplitude oscillations in prominences are among the most spectacular phenomena of the solar atmosphere. Such an oscillations involve motions with velocities above 20 km/s, and large portions of the filament that move in phase. These are triggered by energetic disturbances as flares and jets. These oscillations are an excellent tool to probe the not directly measurable filament morphology. In addition, the damping of these motions can be related with the process of evaporation of chromospheric plasma associated to coronal heating. In these talk I will show recent observational and theoretical progress on large-amplitude seismology on prominences. Title: The Photospheric Footprints of Coronal Hole Jets Authors: Muglach, Karin Bibcode: 2016usc..confE...6M Altcode: Coronal jets are transient, collimated ejections of plasma that are a common feature of solar X-ray and EUV image sequences. Of special interest are jets in coronal holes due to their possible contribution to the solar wind outflow. From a sample of 35 jet events I will investigate the photospheric signatures at the footpoints of these jets. White light images from the HMI on board SDO are used to derive the plane-of-sky flow field using local correlation tracking, and HMI magnetograms show the development of the magnetic flux. Both the evolution of the magnetic field and flows allow one to study the photospheric driver of these jets. One particularly interesting example demonstrates that the untwisting jet involves a tiny filament whose eruption is most likely triggered by the emergence of a small magnetic bipole close to one of its legs. Title: Correlation of Coronal Plasma Properties and Solar Magnetic Field in a Decaying Active Region Authors: Ko, Yuan-Kuen; Young, Peter R.; Muglach, Karin; Warren, Harry P.; Ugarte-Urra, Ignacio Bibcode: 2016ApJ...826..126K Altcode: We present the analysis of a decaying active region observed by the EUV Imaging Spectrometer on Hinode during 2009 December 7-11. We investigated the temporal evolution of its structure exhibited by plasma at temperatures from 300,000 to 2.8 million degrees, and derived the electron density, differential emission measure, effective electron temperature, and elemental abundance ratios of Si/S and Fe/S (as a measure of the First Ionization Potential (FIP) Effect). We compared these coronal properties to the temporal evolution of the photospheric magnetic field strength obtained from the Solar and Heliospheric Observatory Michelson Doppler Imager magnetograms. We find that, while these coronal properties all decreased with time during this decay phase, the largest change was at plasma above 1.5 million degrees. The photospheric magnetic field strength also decreased with time but mainly for field strengths lower than about 70 Gauss. The effective electron temperature and the FIP bias seem to reach a “basal” state (at 1.5 × 106 K and 1.5, respectively) into the quiet Sun when the mean photospheric magnetic field (excluding all areas <10 G) weakened to below 35 G, while the electron density continued to decrease with the weakening field. These physical properties are all positively correlated with each other and the correlation is the strongest in the high-temperature plasma. Such correlation properties should be considered in the quest for our understanding of how the corona is heated. The variations in the elemental abundance should especially be considered together with the electron temperature and density. Title: Converging Supergranular Flows and the Formation of Coronal Plumes Authors: Wang, Y. -M.; Warren, H. P.; Muglach, K. Bibcode: 2016ApJ...818..203W Altcode: Earlier studies have suggested that coronal plumes are energized by magnetic reconnection between unipolar flux concentrations and nearby bipoles, even though magnetograms sometimes show very little minority-polarity flux near the footpoints of plumes. Here we use high-resolution extreme-ultraviolet (EUV) images and magnetograms from the Solar Dynamics Observatory (SDO) to clarify the relationship between plume emission and the underlying photospheric field. We find that plumes form where unipolar network elements inside coronal holes converge to form dense clumps, and fade as the clumps disperse again. The converging flows also carry internetwork fields of both polarities. Although the minority-polarity flux is sometimes barely visible in the magnetograms, the corresponding EUV images almost invariably show loop-like features in the core of the plumes, with the fine structure changing on timescales of minutes or less. We conclude that the SDO observations are consistent with a model in which plume emission originates from interchange reconnection in converging flows, with the plume lifetime being determined by the ∼1 day evolutionary timescale of the supergranular network. Furthermore, the presence of large EUV bright points and/or ephemeral regions is not a necessary precondition for the formation of plumes, which can be energized even by the weak, mixed-polarity internetwork fields swept up by converging flows. Title: A coronal hole jet observed with Hinode and the Solar Dynamics Observatory Authors: Young, Peter R.; Muglach, Karin Bibcode: 2014PASJ...66S..12Y Altcode: 2014PASJ..tmp..106Y; 2014arXiv1402.4389Y; 2014PASJ...66..S12Y A small blowout jet was observed at the boundary of the south polar coronal hole on 2011 February 8 at around 21:00 UT. Images from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO) revealed an expanding loop rising from one footpoint of a compact, bipolar bright point. Magnetograms from the Helioseismic Magnetic Imager (HMI) on board SDO showed that the jet was triggered by the cancelation of a parasitic positive polarity feature near the negative pole of the bright point. The jet emission was present for 25 min and it extended 30 Mm from the bright point. Spectra from the Extreme Ultraviolet Imaging Spectrometer on board Hinode yielded a temperature and density of 1.6 MK and 0.9-1.7 × 108 cm-3 for the ejected plasma. Line-of-sight velocities reached up to 250 km s-1 and were found to increase with height, suggesting plasma acceleration within the body of the jet. Evidence was found for twisting motions within the jet based on variations of the line-of-sight velocities across the jet width. The derived angular speed was in the range (9-12) × 10-3 rad s-1, consistent with previous measurements from jets. The density of the bright point was 7.6 × 108 cm-3, and the peak of the bright point's emission measure occurred at 1.3 MK, with no plasma above 3 MK. Title: NASA Space Weather Research Center: Addressing the Unique Space Weather Needs of NASA Robotic Missions Authors: Zheng, Y.; Pulkkinen, A. A.; Kuznetsova, M. M.; Maddox, M. M.; Mays, M. L.; Taktakishvili, A.; Chulaki, A.; Thompson, B. J.; Collado-Vega, Y. M.; Muglach, K.; Evans, R. M.; Wiegand, C.; MacNeice, P. J.; Rastaetter, L. Bibcode: 2014AGUFMSM31A4151Z Altcode: The Space Weather Research Center (SWRC) has been providing space weather monitoring and forecasting services to NASA's robotic missions since its establishment in 2010. Embedded within the Community Coordinated Modeling Center (CCMC) (see Maddox et al. in Session IN026) and located at NASA Goddard Space Flight Center, SWRC has easy access to state-of-the-art modeling capabilities and proximity to space science and research expertise. By bridging space weather users and the research community, SWRC has been a catalyst for the efficient transition from research to operations and operations to research. In this presentation, we highlight a few unique aspects of SWRC's space weather services, such as addressing space weather throughout the solar system, pushing the frontier of space weather forecasting via the ensemble approach, providing direct personnel and tool support for spacecraft anomaly resolution, prompting development of multi-purpose tools and knowledge bases (see Wiegand et al. in the same session SM004), and educating and engaging the next generation of space weather scientists. Title: The Interaction of Solar Eruptions and Large-Scale Coronal Structures Revealed Through Modeling and Observational Analysis Authors: Evans, R. M.; Savcheva, A. S.; Zink, J. L.; Muglach, K.; Kozarev, K. A.; Opher, M.; van der Holst, B. Bibcode: 2014AGUFMSH11D..05E Altcode: We use numerical and observational approaches to explore how the interaction of a coronal mass ejection (CME) with preexisting structures in the solar atmosphere influences its evolution and space weather effects. We study two aspects of CME evolution: deflection of the CME's propagation direction, and expansion. First, we perform a statistical study of the influence of coronal holes on CME trajectories for more than 50 events during years 2010-2014. Second, we use the Space Weather Modeling Framework (SWMF) to model CME propagation in the Alfven Wave Solar Model (AWSoM), which includes a sophisticated treatment of the physics of coronal heating and solar wind acceleration. The major progress in these simulations is that the initial conditions of the eruptions are highly data-constrained. From the simulations, we determine the CME's trajectory and expansion. We calculate the pile-up of material along the front and sides of a CME due to its expansion, and constrain the properties of the pile-up under a range of conditions. Finally, we will discuss the connection between these plasma density structures and the acceleration of protons to energies relevant to space weather. Title: A Statistical Study of Coronal Mass Ejections and Coronal Holes during 2010-2014 Authors: Zink, J. L.; Evans, R. M.; Muglach, K. Bibcode: 2014AGUFMSH53A4199Z Altcode: When analyzing CMEs in real time for space weather forecasting, a lack of sufficient coronagraph images can make it difficult to determine the CME's location. In these cases, usually the location of significant disk signatures (for example, an associated flare) is used to estimate the CME's location. Although this assumption seems reasonable, observational and numerical studies have shown that CME locations can deviate by ten or more degrees from the source location close to the solar surface. In this work, we present a study of more than 50 events during 2010-2014 covering a range of CME speeds, widths, and source locations. We use the CCMC's space weather Database Of Notifications, Knowledge, and Information (DONKI) to select events, and use the SWPC's CME Analysis Tool to measure CMEs in the SOHO/LASCO and STEREO/SECCHI coronagraph images. We find a range of deflections, from less than 5 degrees to more than 15 degrees. It has been proposed that CMEs deflect during propagation due to interactions with other large-scale structures such as coronal holes, streamers, current sheets, and other CMEs. In this study we focus on the influence of coronal holes. We use a combination of SDO/AIA and SECCHI/EUVI images to locate coronal holes near the CME source locations. We present the calculated CME deflection angles as a function of height in the corona, average speed, average width, and coronal hole properties. The goal of this study is to determine appropriate ranges of latitudes and longitudes that can be used in CME ensemble modeling. This requires that coronal hole observations are more systematically incorporated in real time CME analysis for space weather forecasting. J. Zink conducted this research with support from the Undergraduate Research Scholars Program at GMU. R. Evans is supported through an appointment to the NASA Postdoctoral Program at GSFC, administered by Oak Ridge Associated Universities through a contract with NASA. Title: Observations and Implications of Large-Amplitude Longitudinal Oscillations in a Solar Filament Authors: Karpen, J. T.; Luna Bennasar, M.; Knizhnik, K. J.; Muglach, K.; Gilbert, H. R.; Kucera, T. A.; Uritsky, V. M.; Asfaw, T. T. Bibcode: 2014AGUFMSH51C4171K Altcode: On 20 August 2010 an energetic disturbance triggered large-amplitude longitudinal oscillations in a large fraction of a nearby filament. The triggering mechanism appears to be episodic jets connecting the energetic event with the filament threads. We analyzed this periodic motion to characterize the underlying physics of the oscillation as well as the filament properties. The results support our previous theoretical conclusions that the restoring force of large-amplitude longitudinal oscillations is solar gravity, and the damping mechanism is the ongoing accumulation of mass onto the oscillating threads. Based on our previous work, we used the fitted parameters to determine the magnitude and radius of curvature of the dipped magnetic field along the filament, as well as the mass accretion rate onto the filament threads. These derived properties are nearly uniform along the filament, indicating a remarkable degree of homogeneity throughout the filament channel. Moreover, the estimated mass accretion rate implies that the footpoint heating responsible for the thread formation, according to the thermal nonequilibrium model, agrees with previous coronal heating estimates. We also estimated the magnitude of the energy released in the nearby event by studying the dynamic response of the filament threads, and concluded that the initiating event is likely to be a microflare. Using a nonlinear force-free field extrapolation of the photospheric magnetogram to estimate the coronal magnetic structure, we determined the possible connectivity between the jet source and the oscillating prominence segments. We will present the results of this investigation and discuss their implications for filament structure and heating. This work was supported by NASA's H-SR program. Title: Solar Dynamics Observatory and Hinode Observations of a Blowout Jet in a Coronal Hole Authors: Young, P. R.; Muglach, K. Bibcode: 2014SoPh..289.3313Y Altcode: 2013arXiv1309.7324Y; 2014SoPh..tmp...24Y A blowout jet occurred within the south coronal hole on 9 February 2011 at 09:00 UT and was observed by the Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) onboard the Solar Dynamics Observatory, and by the EUV Imaging Spectrometer (EIS) and X-Ray Telescope (XRT) onboard the Hinode spacecraft during coronal-hole monitoring performed as part of Hinode Operations Program No. 177. Images from AIA show expanding hot and cold loops from a small bright point with plasma ejected in a curtain up to 30 Mm wide. The initial intensity front of the jet had a projected velocity of 200 km s−1, and the line-of-sight (LOS) velocities measured by EIS are between 100 and 250 km s−1. The LOS velocities increased along the jet, implying that an acceleration mechanism operates within the body of the jet. The jet plasma had a density of 2.7×108 cm−3 and a temperature of 1.4 MK. During the event a number of bright kernels were seen at the base of the bright point. The kernels have sizes of ≈ 1000 km, are variable in brightness, and have lifetimes of 1 - 15 minutes. An XRT filter ratio yields temperatures of 1.5 - 3.0 MK for the kernels. The bright point existed for at least ten hours, but disappeared within two hours after the jet, which lasted for 30 minutes. HMI data reveal converging photospheric flows at the location of the bright point, and the mixed-polarity magnetic flux canceled over a period of four hours on either side of the jet. Title: Temporal Evolution of Solar Wind Ion Composition and their Source Coronal Holes During the Declining Phase of Cycle 23 Authors: Ko, Yuan-Kuen; Muglach, Karin; Wang, Yi-Ming; Young, Peter R.; Lepri, Susan T. Bibcode: 2014AAS...22432366K Altcode: We present our analysis of the temporal trend in the solar wind (SW) ion charge states and the properties in the associated source coronal holes (CHs) during the declining phase of solar cycle 23. We find that the SW ions exhibit a trend of decreasing ionization state with time, consistent with previous studies. However the rate of decrease is different between the slow and fast SW. The photospheric magnetic field strength in both regions is found to exhibit similar trend of decrease with time. On the other hand, the temporal trend is different in the line emissions from different layers of the atmosphere (chromosphere, transit region and corona). Within each CH, the coronal emission generally increases toward the boundary of the CH as the underlying photospheric magnetic field strength increases, the net unbalanced field strength decreases and the magnetic field becomes less unipolar. But the coronal emission averaged over the entire CH area does not have appreciable change with time. We find that ions which freeze-in at lower altitude in the corona, such as C and O ions, have a stronger correlation between their ionization state and the average photospheric magnetic field strength in the slow SW, while Fe ions which freeze-in at higher altitude have a stronger correlation in the fast SW. Our analyses provide important clues for how the SW is formed, heated and accelerated in response to the long-term evolution of the solar magnetic field at its source coronal hole. Title: Observations and Implications of Large-Amplitude LongitudinalOscillations in a Solar Filament Authors: Karpen, Judith T.; Luna, Manuel; Knizhnik, Kalman J.; Muglach, Karin; Gilbert, Holly; Kucera, Therese A.; Uritsky, Vadim Bibcode: 2014AAS...22411106K Altcode: On 20 August 2010 an energetic disturbance triggered large-amplitude longitudinal oscillations in a large fraction of a nearby filament. The triggering mechanism appears to be episodic jets connecting the energetic event with the filament threads. We analyzed this periodic motion to characterize the underlying physics of the oscillation as well as the filament properties. The results support our previous theoretical conclusions that the restoring force of large-amplitude longitudinal oscillations is solar gravity, and the damping mechanism is the ongoing accumulation of mass onto the oscillating threads. Based on our previous work, we used the fitted parameters to determine the magnitude and radius of curvature of the dipped magnetic field along the filament, as well as the mass accretion rate onto the filament threads. These derived properties are nearly uniform along the filament, indicating a remarkable degree of homogeneity throughout the filament channel. Moreover, the estimated mass accretion rate implies that the footpoint heating responsible for the thread formation, according to the thermal nonequilibrium model, agrees with previous coronal heating estimates. We also estimated the magnitude of the energy released in the nearby event by studying the dynamic response of the filament threads, and concluded that the initiating event is likely to be a microflare. We will present the results of this investigation and discuss their implications for filament structure and heating. This work was supported by NASA’s H-SR program. Title: Temporal Evolution of Solar Wind Ion Composition and their Source Coronal Holes during the Declining Phase of Cycle 23. I. Low-latitude Extension of Polar Coronal Holes Authors: Ko, Yuan-Kuen; Muglach, Karin; Wang, Yi-Ming; Young, Peter R.; Lepri, Susan T. Bibcode: 2014ApJ...787..121K Altcode: We analyzed 27 solar wind (SW) intervals during the declining phase of cycle 23, whose source coronal holes (CHs) can be unambiguously identified and are associated with one of the polar CHs. We found that the SW ions have a temporal trend of decreasing ionization state, and such a trend is different between the slow and fast SW. The photospheric magnetic field, both inside and at the outside boundary of the CH, also exhibits a trend of decrease with time. However, EUV line emissions from different layers of the atmosphere exhibit different temporal trends. The coronal emission inside the CH generally increases toward the CH boundary as the underlying field increases in strength and becomes less unipolar. In contrast, this relationship is not seen in the coronal emission averaged over the entire CH. For C and O SW ions that freeze-in at lower altitude, stronger correlation between their ionization states and field strength (both signed and unsigned) appears in the slow SW, while for Fe ions that freeze-in at higher altitude, stronger correlation appears in the fast SW. Such correlations are seen both inside the CH and at its boundary region. On the other hand, the coronal electron temperature correlates well with the SW ion composition only in the boundary region. Our analyses, although not able to determine the likely footpoint locations of the SW of different speeds, raise many outstanding questions for how the SW is heated and accelerated in response to the long-term evolution of the solar magnetic field. Title: Photospheric Signatures of Coronal Hole Jets Authors: Muglach, Karin; Young, Peter R. Bibcode: 2014AAS...22432333M Altcode: Coronal jets are transient, collimated ejections of plasma that are a common feature of solar X-ray and EUV image sequences. Of special interest is the contribution that coronal hole jets make to the solar wind outflow. A new class of coronal hole jets, termed "dark jets", has been identified with the EUV Imaging Spectrometer (EIS) on board Hinode. The jets are identified in EUV spectral lines with line-of-sight velocities of 50-100 km/s and enhanced line widths, yet they show little or no intensity signature in image sequences from the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory (SDO) or the X-Ray Telescope on board Hinode.In this contribution we will investigate the photosphere at the footpoint of these jets. White light images from the Helioseismic Magnetic Imager (HMI) on board SDO are used to derive the plane-of-sky flow field using local correlation tracking, and HMI magnetograms show the evolution of the magnetic flux. Both the evolution of the magnetic field and flows allow us to study the photospheric driver of these jets. Title: Characterization of Near-Sun Coronal Mass Ejection Deflection using Coronagraph Image Sequences Authors: Zink, Jenna; Evans, Rebekah M.; Muglach, Karin Bibcode: 2014shin.confE.167Z Altcode: When analyzing CMEs in real time for space weather forecasting, a lack of sufficient coronagraph images can make it difficult to determine the CME"s longitude. In these cases, usually the location of significant disk signatures (for example, an associated flare) is used to estimate the CME"s location. Although this assumption seems reasonable, observational and numerical studies have shown that CME locations can deviate by ten or more degrees from the source location close to the solar surface. An accurate determination of the CME location is essential for CME arrival predictions. For example, results from CME ensemble modeling carried out by the NASA/GSFC Space Weather Research Center have shown that a variation of a CME"s position by 10 degrees can change the arrival time at 1 AU by 8 hours. Title: Observations and Implications of Large-amplitude Longitudinal Oscillations in a Solar Filament Authors: Luna, M.; Knizhnik, K.; Muglach, K.; Karpen, J.; Gilbert, H.; Kucera, T. A.; Uritsky, V. Bibcode: 2014ApJ...785...79L Altcode: 2014arXiv1403.0381L On 2010 August 20, an energetic disturbance triggered large-amplitude longitudinal oscillations in a nearby filament. The triggering mechanism appears to be episodic jets connecting the energetic event with the filament threads. In the present work, we analyze this periodic motion in a large fraction of the filament to characterize the underlying physics of the oscillation as well as the filament properties. The results support our previous theoretical conclusions that the restoring force of large-amplitude longitudinal oscillations is solar gravity, and the damping mechanism is the ongoing accumulation of mass onto the oscillating threads. Based on our previous work, we used the fitted parameters to determine the magnitude and radius of curvature of the dipped magnetic field along the filament, as well as the mass accretion rate onto the filament threads. These derived properties are nearly uniform along the filament, indicating a remarkable degree of cohesiveness throughout the filament channel. Moreover, the estimated mass accretion rate implies that the footpoint heating responsible for the thread formation, according to the thermal nonequilibrium model, agrees with previous coronal heating estimates. We estimate the magnitude of the energy released in the nearby event by studying the dynamic response of the filament threads, and discuss the implications of our study for filament structure and heating. Title: Evidence for Two Separate Heliospheric Current Sheets of Cylindrical Shape During Mid-2012 Authors: Wang, Y. -M.; Young, P. R.; Muglach, K. Bibcode: 2014ApJ...780..103W Altcode: During the reversal of the Sun's polar fields at sunspot maximum, outward extrapolations of magnetograph measurements often predict the presence of two or more current sheets extending into the interplanetary medium, instead of the single heliospheric current sheet (HCS) that forms the basis of the standard "ballerina skirt" picture. By comparing potential-field source-surface models of the coronal streamer belt with white-light coronagraph observations, we deduce that the HCS was split into two distinct structures with circular cross sections during mid-2012. These cylindrical current sheets were centered near the heliographic equator and separated in longitude by roughly 180° a corresponding four-sector polarity pattern was observed at Earth. Each cylinder enclosed a negative-polarity coronal hole that was identifiable in extreme ultraviolet images and gave rise to a high-speed stream. The two current sheet systems are shown to be a result of the dominance of the Sun's nonaxisymmetric quadrupole component, as the axial dipole field was undergoing its reversal during solar cycle 24. Title: Large-amplitude longitudinal oscillations in solar prominences Authors: Luna, Manuel; Karpen, Judith; Díaz, Antonio; Knizhnik, Kalman; Muglach, Karin; Gilbert, Holly; Kucera, Therese Bibcode: 2014IAUS..300..155L Altcode: Large-amplitude longitudinal (LAL) prominence oscillations consist of periodic mass motions along a filament axis. The oscillations appear to be triggered by an energetic event, such as a microflare, subflare, or small C-class flare, close to one end of the filament. Observations reveal speeds of several tens to 100 km/s, periods of order 1 hr, damping times of a few periods, and displacements equal to a significant fraction of the prominence length. We have developed a theoretical model to explain the restoring force and the damping mechanism. Our model demonstrates that the main restoring force is the projected gravity in the flux tube dips where the threads oscillate. Although the period is independent of the tube length and the constantly growing mass, the motions are strongly damped by the steady accretion of mass onto the threads. We conclude that the LAL movements represent a collective oscillation of a large number of cool, dense threads moving along dipped flux tubes, triggered by a nearby energetic event. Our model yields a powerful seismological method for constraining the coronal magnetic field strength and radius of curvature at the thread locations. Title: Observational Study of Large Amplitude Longitudinal Oscillations in a Solar Filament Authors: Knizhnik, Kalman; Luna, Manuel; Muglach, Karin; Gilbert, Holly; Kucera, Therese; Karpen, Judith Bibcode: 2014IAUS..300..428K Altcode: 2013arXiv1310.7657K On 20 August 2010 an energetic disturbance triggered damped large-amplitude longitudinal (LAL) oscillations in almost an entire filament. In the present work we analyze this periodic motion in the filament to characterize the damping and restoring mechanism of the oscillation. Our method involves placing slits along the axis of the filament at different angles with respect to the spine of the filament, finding the angle at which the oscillation is clearest, and fitting the resulting oscillation pattern to decaying sinusoidal and Bessel functions. These functions represent the equations of motion of a pendulum damped by mass accretion. With this method we determine the period and the decaying time of the oscillation. Our preliminary results support the theory presented by Luna and Karpen (2012) that the restoring force of LAL oscillations is solar gravity in the tubes where the threads oscillate, and the damping mechanism is the ongoing accumulation of mass onto the oscillating threads. Following an earlier paper, we have determined the magnitude and radius of curvature of the dipped magnetic flux tubes hosting a thread along the filament, as well as the mass accretion rate of the filament threads, via the fitted parameters. Title: A Spectroscopic Survey of Coronal Hole Jets Authors: Young, Peter R.; Muglach, K. Bibcode: 2013SPD....44...19Y Altcode: Coronal hole jets have been suggested to make a significant contribution to the solar wind, but spectroscopic measurements - which provide the best means of measuring the mass flux - have been rare due to the difficulty of capturing jets with narrow slit spectrometers. A continuous two day coronal hole measurement made with the Hinode/EIS instrument is reported, which has revealed over 30 jets seen in the coronal Fe XII 195.12 (1.5 MK) emission line. More than half of the events have no clear signature in SDO/AIA or Hinode/XRT images and thus represent a separate class of jet events not previously reported. The jets show a wide range of morphologies, ranging from classic columnar features to mini-CME events. Statistics of the events will be presented: their relation to bright points and the coronal hole boundary; durations; and repeated occurrence. Velocity, density and temperature measurements derived from the EIS spectra will be presented, and mass flux estimated. The photospheric signatures of the jets, as determined from SDO/HMI, will be shown in a separate presentation (Muglach & Young). Title: Photospheric signatures of coronal hole jets Authors: Muglach, Karin; Young, P. R. Bibcode: 2013SPD....44...20M Altcode: Jets in EUV and X-ray images have been observed for several decades. Many of them originate in coronal holes which have received special interest as possible contributors to the solar wind. A new class of CH jets are observed with Hinode/EIS which show pronounced signatures in EUV spectral lines. Coronal velocities of up to 200 km/s and enhancements in line width are measured. On the other hand these jets are hardly visible in imaging data like SDO/AIA and Hinode/XRT (see contribution by Young and Muglach). In this contribution we will investigate the photospheric signatures at the footpoint of these jets. We use SDO/HMI magnetograms to show the evolution of the magnetic flux. From SDO white light images we derive the plane-of-sky flow field using local correlation tracking. Both the evolution of the magnetic field and the flows allow us to study the photospheric drivers of these jets. Title: Transient Brightenings Along Filament Channels as Observed with SDO/AIA and HMI Authors: Muglach, Karin; Wang, Y. Bibcode: 2013SPD....4410503M Altcode: Filament channels coincide with large-scale polarity inversion lines of the photospheric magnetic field, where flux cancellation continually takes place. High-cadence Solar Dynamics Observatory (SDO) images recorded in He II 30.4 nm and Fe IX 17.1 nm in August 2010 reveal numerous transient brightenings occurring along the edge of a filament channel within a decaying active region, where SDO line-of-sight magnetograms show strong opposite-polarity flux in close contact. The brightenings are elongated along the direction of the filament channel, with linear extents of several arcseconds, and typically last a few minutes; they sometimes have the form of multiple two-sided ejections with speeds on the order of 100 km/s. Remarkably, some of the brightenings rapidly develop into larger scale events, forming sheetlike structures that are eventually torn apart by the diverging flows in the filament channel and ejected in opposite directions. In some cases, the flow patterns that develop in the channel may bring successive horizontal loops together and cause a cascade to larger scales. One of these brightening events was the initiation of a large-amplitude longitudinal oscillation of the filament. We interpret the brightenings as resulting from reconnections among filament-channel field lines having one footpoint located in the region of canceling flux. Title: The velocity signature of coronal jets as observed with Hinode/EIS Authors: Muglach, K.; Young, P. R. Bibcode: 2013enss.confE..59M Altcode: In this contribution we show preliminary results of a study of jets in coronal holes. We use Hinode/EIS to investigate the spectroscopic signatures of the jets and SDO/AIA and HMI to derive additional information on the plasma and magnetic field evolution. EIS was scanning a low latitude coronal hole and tracking it for about 2 days as it rotated over the solar disk. The coronal jets are best revealed through Doppler and line width maps of Fe XII 195.1 A (formed at 1.5 MK), and have sizes of 10-100 arcsec. Higher spatial and time resolution is provided by SDO: coronal and chromospheric images from AIA show the time evolution of the jet and line-of-sight magnetograms show the evolution of the magnetic footpoints of the jet. We present several examples of these extended jets and describe their properties as derived from the diagnostics we have available. Title: Transient Brightenings Associated with Flux Cancellation along a Filament Channel Authors: Wang, Y. -M.; Muglach, K. Bibcode: 2013ApJ...763...97W Altcode: Filament channels coincide with large-scale polarity inversion lines of the photospheric magnetic field, where flux cancellation continually takes place. High-cadence Solar Dynamics Observatory (SDO) images recorded in He II 30.4 nm and Fe IX 17.1 nm during 2010 August 22 reveal numerous transient brightenings occurring along the edge of a filament channel within a decaying active region, where SDO line-of-sight magnetograms show strong opposite-polarity flux in close contact. The brightenings are elongated along the direction of the filament channel, with linear extents of several arcseconds, and typically last a few minutes; they sometimes have the form of multiple two-sided ejections with speeds on the order of 100 km s-1. Remarkably, some of the brightenings rapidly develop into larger scale events, forming sheetlike structures that are eventually torn apart by the diverging flows in the filament channel and ejected in opposite directions. We interpret the brightenings as resulting from reconnections among filament-channel field lines having one footpoint located in the region of canceling flux. In some cases, the flow patterns that develop in the channel may bring successive horizontal loops together and cause a cascade to larger scales. Title: Properties of a Decaying Sunspot Authors: Balthasar, H.; Beck, C.; Gömöry, P.; Muglach, K.; Puschmann, K. G.; Shimizu, T.; Verma, M. Bibcode: 2013CEAB...37..435B Altcode: 2013arXiv1301.1562B A small decaying sunspot was observed with the Vacuum Tower Telescope (VTT) on Tenerife and the Japanese Hinode satellite. We obtained full Stokes scans in several wavelengths covering different heights in the solar atmosphere. Imaging time series from Hinode and the Solar Dynamics Observatory (SDO) complete our data sets. The spot is surrounded by a moat flow, which persists also on that side of the spot where the penumbra already had disappeared. Close to the spot, we find a chromospheric location with downflows of more than 10 km s^{-1} without photospheric counterpart. The height dependence of the vertical component of the magnetic field strength is determined in two different ways that yielded different results in previous investigations. Such a difference still exists in our present data, but it is not as pronounced as in the past. Title: A Preliminary Study of Active Region Canopies With AIA Authors: Lucchini, Scott; Saar, S.; Muglach, K. Bibcode: 2013AAS...22115905L Altcode: Active region canopies are areas frequently accompanying active regions which have extensive horizontal magnetic fields. The large-scale canopy fields have a significant effect on the kinds of structures which can exist beneath them, and how they evolve. Using data from the Atmospheric Imaging Assembly (AIA), we developed methods to automatically identify these regions. A Differential Emission Measure (DEM) analysis is consistent with the idea that the long, hotter active region loops overlie quite cool, small-scale features ("fibrils"). We suggest that the overlying loops restrict the growth of underlying structures to mostly very short, cool features. We also studied evolution of canopy regions over time. In several cases, a large quiescent filament formed out of the former canopy region over the course of a few solar rotations, confirming previous suggestions. The canopy remains visible for several rotations after its active regions have begun to decay; in this time, the fibril magnetic fields gradually align in such a way as to form a filament channel. Further analysis of our large canopy database should uncover more information on the frequency and characteristics of these canopy-to-filament evolutions, as well as other canopy properties. This work is supported by the NSF REU program at SAO (grant ATM-0851866) and contract SP02H1701R from Lockheed Martin to SAO for SDO research. Title: A Long-Lived Equatorial Coronal Hole and the Associated Solar Wind Authors: Ko, Y.; Young, P. R.; Muglach, K.; Wang, Y.; Lepri, S. T.; Laming, J. M.; Popecki, M. Bibcode: 2012AGUFMSH53A2261K Altcode: We study an equatorial coronal hole that came back rotation after rotation in a course of eight months from July 2007 to March 2008. This coronal hole was also one of the source regions of the solar wind measured by ACE during this period. The associated solar wind speed profiles for the 10 solar rotations are similar that start with a fast wind above 600 km/s and gradually lower down to below 400 km/s. The ion composition data indicate a decreasing trend in the ionization states of heavy ions, especially for the Fe ions. This recurring coronal hole presents a good opportunity for studying the relations between the solar wind at a range of speeds and the solar source that produces it. We present a detailed study of the solar wind from this coronal hole, concentrating on the ion charge and elemental composition properties, and the variation in the magnetic and spectroscopic properties in this source coronal hole. We discuss implications in the solar wind formation based on the relations between these properties of the source coronal hole and the associated solar wind. Title: Evidence for Two Separate But Interlaced Components of the Chromospheric Magnetic Field Authors: Muglach, Karin; Reardon, K.; Wang, Y.; Warren, H. Bibcode: 2012AAS...22012403M Altcode: Chromospheric fibrils are generally thought to trace out horizontal magnetic fields that fan out from flux concentrations in the photosphere. A high-resolution (0.2") image taken in the core of the Ca II 854.2 nm line shows the dark fibrils within an active region remnant as fine, looplike features that are aligned parallel to each other and have lengths on the order of a supergranular diameter ( 30 Mm). Comparison with a line-of-sight magnetogram confirms that the fibrils are centered above intranetwork areas, with one end rooted just inside
the neighboring plage or strong unipolar network but the other endpoint less clearly defined. Focusing on a particular arcade-like structure lying entirely on one side of a filament channel (large-scale polarity inversion), we find that the total amount of positive-polarity flux underlying this ``fibril arcade'' is 50 times greater than the total amount of negative-polarity flux. Thus, if the fibrils represent closed loops, they must consist of very weak fields (in terms of flux density), which are interpenetrated by a more vertical field that contains most of the flux. This surprising result suggests that the fibrils in unipolar regions connect the network to the nearby intranetwork flux, while the bulk of the network flux is diverted upward into the corona and connects to remote regions of the opposite polarity. We conclude that the chromospheric field near the edge of the network has an interlaced structure resembling that in sunspot penumbrae, with the fibrils representing the low-lying horizontal flux that remains trapped within the highly nonpotential chromospheric layer. Title: An Exploration of the Emission Properties of X-ray Bright Points Seen With SDO Authors: Saar, Steven H.; Elsden, T.; Muglach, K. Bibcode: 2012AAS...22020713S Altcode: We present preliminary results of a study of X-ray Bright Point (XBP) EUV emission and its dependence on other properties. The XBPs were located using a new, automated XBP finder for AIA developed as part of the Feature Finding Team for SDO Computer Vision. We analyze XBPs near disk center, comparing AIA EUV fluxes, HMI LOS magnetic fields, and photospheric flow fields (derived from HMI data) to look for relationships between XBP emission, magnetic flux, velocity fields, and XBP local environment. We find some evidence for differences in the mean XBP temperature with environment. Unsigned magnetic flux is correlated with XBP emission, though other parameters play a role. The majority of XBP footpoints are approaching each other, though at a slight angle from head-on on average. We discuss the results in the context of XBP heating. Title: A First Look at Magnetic Field Data Products from SDO/HMI Authors: Liu, Y.; Scherrer, P. H.; Hoeksema, J. T.; Schou, J.; Bai, T.; Beck, J. G.; Bobra, M.; Bogart, R. S.; Bush, R. I.; Couvidat, S.; Hayashi, K.; Kosovichev, A. G.; Larson, T. P.; Rabello-Soares, C.; Sun, X.; Wachter, R.; Zhao, J.; Zhao, X. P.; Duvall, T. L., Jr.; DeRosa, M. L.; Schrijver, C. J.; Title, A. M.; Centeno, R.; Tomczyk, S.; Borrero, J. M.; Norton, A. A.; Barnes, G.; Crouch, A. D.; Leka, K. D.; Abbett, W. P.; Fisher, G. H.; Welsch, B. T.; Muglach, K.; Schuck, P. W.; Wiegelmann, T.; Turmon, M.; Linker, J. A.; Mikić, Z.; Riley, P.; Wu, S. T. Bibcode: 2012ASPC..455..337L Altcode: The Helioseismic and Magnetic Imager (HMI; Scherrer & Schou 2011) is one of the three instruments aboard the Solar Dynamics Observatory (SDO) that was launched on February 11, 2010 from Cape Canaveral, Florida. The instrument began to acquire science data on March 24. The regular operations started on May 1. HMI measures the Doppler velocity and line-of-sight magnetic field in the photosphere at a cadence of 45 seconds, and the vector magnetic field at a 135-second cadence, with a 4096× 4096 pixels full disk coverage. The vector magnetic field data is usually averaged over 720 seconds to suppress the p-modes and increase the signal-to-noise ratio. The spatial sampling is about 0".5 per pixel. HMI observes the Fe i 6173 Å absorption line, which has a Landé factor of 2.5. These data are further used to produce higher level data products through the pipeline at the HMI-AIA Joint Science Operations Center (JSOC) - Science Data Processing (Scherrer et al. 2011) at Stanford University. In this paper, we briefly describe the data products, and demonstrate the performance of the HMI instrument. We conclude that the HMI is working extremely well. Title: Decorrelation Times of Photospheric Fields and Flows Authors: Welsch, B. T.; Kusano, K.; Yamamoto, T. T.; Muglach, K. Bibcode: 2012ApJ...747..130W Altcode: 2011arXiv1110.6117W We use autocorrelation to investigate evolution in flow fields inferred by applying Fourier local correlation tracking (FLCT) to a sequence of high-resolution (0farcs3), high-cadence (sime 2 minute) line-of-sight magnetograms of NOAA active region (AR) 10930 recorded by the narrowband filter imager of the Solar Optical Telescope aboard the Hinode satellite over 2006 December 12 and 13. To baseline the timescales of flow evolution, we also autocorrelated the magnetograms, at several spatial binnings, to characterize the lifetimes of active region magnetic structures versus spatial scale. Autocorrelation of flow maps can be used to optimize tracking parameters, to understand tracking algorithms' susceptibility to noise, and to estimate flow lifetimes. Tracking parameters varied include: time interval Δt between magnetogram pairs tracked, spatial binning applied to the magnetograms, and windowing parameter σ used in FLCT. Flow structures vary over a range of spatial and temporal scales (including unresolved scales), so tracked flows represent a local average of the flow over a particular range of space and time. We define flow lifetime to be the flow decorrelation time, τ. For Δt > τ, tracking results represent the average velocity over one or more flow lifetimes. We analyze lifetimes of flow components, divergences, and curls as functions of magnetic field strength and spatial scale. We find a significant trend of increasing lifetimes of flow components, divergences, and curls with field strength, consistent with Lorentz forces partially governing flows in the active photosphere, as well as strong trends of increasing flow lifetime and decreasing magnitudes with increases in both spatial scale and Δt. Title: On the Solar Wind Ion Composition Properties With Source Regions from Low-Latitude and Polar Coronal Holes of Opposite Polarity Authors: Ko, Y.; Muglach, K.; Wang, Y.; Young, P. R.; Lepri, S. T.; Laming, J. M.; Popecki, M. Bibcode: 2011AGUFMSH43F..04K Altcode: During Years 2004-2007 there were frequent appearances of low-latitude coronal holes (CHs) and low-latitude extension of polar CHs. These CHs were the source regions of the solar wind measured in-situ at L1. We find that the ion composition has distinct properties between solar wind originating from CHs of opposite polarity. Specifically, the charge states measured by ACE/SWICS were systematically lower-ionized for solar wind ions from CHs of positive polarity (the 'south CH') than those of negative polarity (the 'north CH'), regardless of the solar wind speed. Such differentiation is apparent only in the low-latitude extension of polar CHs and those non-polar CHs with predicted footpoints at latitude higher than 15 degrees. Interestingly, earlier work based on Ulysses fast wind data during the declining/minimum phase of Cycle 22 found that it was the north polar CH that was associated with lower solar wind charge states, opposite to what we found in the following solar cycle. We present these results and search for solar properties that may be factors that govern this north-south difference. Title: Evidence for Two Separate but Interlaced Components of the Chromospheric Magnetic Field Authors: Reardon, K. P.; Wang, Y. -M.; Muglach, K.; Warren, H. P. Bibcode: 2011ApJ...742..119R Altcode: Chromospheric fibrils are generally thought to trace out low-lying, mainly horizontal magnetic fields that fan out from flux concentrations in the photosphere. A high-resolution (~0farcs1 pixel-1) image, taken in the core of the Ca II 854.2 nm line and covering an unusually large area, shows the dark fibrils within an active region remnant as fine, looplike features that are aligned parallel to each other and have lengths comparable to a supergranular diameter. Comparison with simultaneous line-of-sight magnetograms confirms that the fibrils are centered above intranetwork areas (supergranular cell interiors), with one end rooted just inside the neighboring plage or strong unipolar network but the other endpoint less clearly defined. Focusing on a particular arcade-like structure lying entirely on one side of a filament channel (large-scale polarity inversion), we find that the total amount of positive-polarity flux underlying this "fibril arcade" is ~50 times greater than the total amount of negative-polarity flux. Thus, if the fibrils represent closed loops, they must consist of very weak fields (in terms of total magnetic flux), which are interpenetrated by a more vertical field that contains most of the flux. This surprising result suggests that the fibrils in unipolar regions connect the network to the nearby intranetwork flux, while the bulk of the network flux links to remote regions of the opposite polarity, forming a second, higher canopy above the fibril canopy. The chromospheric field near the edge of the network thus has an interlaced structure resembling that in sunspot penumbrae. Title: Tracking Vector Magnetograms from the Solar Dynamics Observatory Authors: Schuck, P. W.; Sun, X.; Muglach, K.; Hoeksema, J. T.; HMI Vector Field Team Bibcode: 2011sdmi.confE..36S Altcode: The differential affine velocity estimator for vector magnetograms (DAVE4VM) has been developed for estimating photospheric velocities. The accuracy of this technique has been demonstrated on synthetic magnetograms from MHD simulations. The algorithm was initially formulated in Cartesian coordinates. Thus, for best results, solar vector magnetograms must be transformed from the image plane into a Mercator map or some other Cartesian-like projection before applyng DAVE4VM. Recently, DAVE4VM has been modified to incorporate directly the projected spherical geometry of Helioprojective-Cartesian coordinates, thus permitting direct application of the method to image plane vector magnetograms. We will discuss the new algorithm and tests of the modified method and present first results of DAVE4VM applied to Solar Dynamics Observatory vector magnetograms. Title: On the ion composition properties in the solar wind from the north and south polar coronal holes Authors: Ko, Yuan-Kuen; Muglach, Karin; Wang, Yi-Ming; Young, Peter R.; Lepri, Susan T.; Laming, J. Martin; Popecki, Mark A. Bibcode: 2011shin.confE.158K Altcode: During Years 2005-2007 in the declining phase of Cycle 23 there were frequent appearances of equatorial coronal holes (CHs) and low-latitude extension of polar CHs that were the source regions of the solar wind measured in-situ at L1 a few days after these CHs past the central meridian. We find that the solar wind heavy ions emanating from the south and north polar CHs have distinct composition properties. Specifically, the charge states measured by ACE/SWICS were systematically lower for solar wind ions from the south polar CHs than those from the north polar CHs, regardless of the solar wind speed. Interestingly, earlier work based on Ulysses data during the declining/minimum phase of Cycle 22 found that it was the north polar CH that was associated with lower solar wind charge states, opposite to what we found in the following solar cycle. We present these results and search for solar properties that may be factors that govern this north-south difference. Implications in solar wind formation are discussed. Title: The Evolution of Dark Canopies Around Active Regions Authors: Wang, Y. -M.; Robbrecht, E.; Muglach, K. Bibcode: 2011ApJ...733...20W Altcode: 2011arXiv1103.4373W As observed in spectral lines originating from the chromosphere, transition region, and low corona, active regions are surrounded by an extensive "circumfacular" area which is darker than the quiet Sun. We examine the properties of these dark moat- or canopy-like areas using Fe IX 17.1 nm images and line-of-sight magnetograms from the Solar Dynamics Observatory. The 17.1 nm canopies consist of fibrils (horizontal fields containing extreme-ultraviolet-absorbing chromospheric material) clumped into featherlike structures. The dark fibrils initially form a quasiradial or vortical pattern as the low-lying field lines fanning out from the emerging active region connect to surrounding network and intranetwork elements of opposite polarity. The area occupied by the 17.1 nm fibrils expands as supergranular convection causes the active-region flux to spread into the background medium; the outer boundary of the dark canopy stabilizes where the diffusing flux encounters a unipolar region of opposite sign. The dark fibrils tend to accumulate in regions of weak longitudinal field and to become rooted in mixed-polarity flux. To explain the latter observation, we note that the low-lying fibrils are more likely to interact with small loops associated with weak, opposite-polarity flux elements in close proximity, than with high loops anchored inside strong unipolar network flux. As a result, the 17.1 nm fibrils gradually become concentrated around the large-scale polarity inversion lines (PILs), where most of the mixed-polarity flux is located. Systematic flux cancellation, assisted by rotational shearing, removes the field component transverse to the PIL and causes the fibrils to coalesce into long PIL-aligned filaments. Title: Studying Solar Active Regions with HMI Data Authors: Liu, Yang; Hoeksema, J.; Hayashi, K.; Sun, X.; Schuck, P.; Muglach, K. Bibcode: 2011SPD....42.2102L Altcode: 2011BAAS..43S.2102L Full disk field of view, continuous time coverage, high temporal and spatial resolutions, and consistent data quality, these specifications of the HMI observational data allows us to study in detail the evolution of solar active regions during the course from emerging to decaying. Using the HMI vector magnetic field data (test version), we study the magnetic energy and helicity in emerging active regions. First, we apply the code DAVE4VM (Schuck 2008) to the time-series vector magnetic field data to derive the plasma velocity; then we break down the energy and helicity fluxes into two components, one due to vertical advection of the magnetic field through the photosphere, and the other due to the horizontal motion that shears the field lines. We analyze the roles these two processes play in accumulating the energy and helicity in the corona, and explore their correlations with the evolution of active regions. Title: The Photospheric Velocity Field of Active Regions Derived from SDO/HMI Vector Magnetograms Authors: Muglach, Karin; Schuck, P.; HMI vector magnetogram Team Bibcode: 2011SPD....42.2112M Altcode: 2011BAAS..43S.2112M We present a first analysis of solar active regions observed with the Helioseismic and Magnetic Imager (HMI) on the Solar Dynamics Observatory (SDO). Since HMI continuously observes the complete solar disk at a good spatial resolution we are able to follow active regions over several days, providing the opportunity to study the evolution of the flow field during the various stages of development of the active regions. HMI measures the photospheric vector magnetic field at a cadence of 12 min. To determine the velocity field we use the optical flow technique DAVE4VM (differential affine velocity estimator for vector magnetograms) and apply it to the vector magnetic field data from SDO/HMI. Title: The Evolution of Dark Canopies Around Active Regions Authors: Muglach, Karin; Wang, Y. M.; Robbrecht, E. Bibcode: 2011SPD....42.1718M Altcode: 2011BAAS..43S.1718M As observed in spectral lines originating from the chromosphere, transition region, and low corona, active regions are surrounded by an extensive 'circumfacular' area which is darker than the quiet Sun. We examine the properties of these dark moat- or canopy-like areas using Fe IX 17.1 nm images and line-of-sight magnetograms from the Solar Dynamics Observatory. The 17.1 nm canopies consist of fibrils (horizontal fields containing EUV-absorbing chromospheric material) clumped into featherlike structures. The dark fibrils initially form a quasiradial or vortical pattern as the low-lying field lines fanning out from the emerging active region connect to surrounding network and intranetwork elements of the opposite polarity. The area occupied by the 17.1 nm fibrils expands as supergranular convection causes the active region flux to spread into the background medium; the outer boundary of the dark canopy stabilizes where the diffusing flux encounters a unipolar region of the opposite sign. The dark fibrils tend to accumulate in regions of weak longitudinal field and to become rooted in mixed-polarity flux. To explain the latter observation, we note that the low-lying fibrils are more likely to interact with small loops associated with weak, opposite-polarity flux elements in close proximity, than with high loops anchored inside strong unipolar network flux. As a result, the 17.1 nm fibrils gradually become concentrated around the large-scale polarity inversion lines (PILs), where most of the mixed-polarity flux is located. Systematic flux cancellation, assisted by rotational shearing, removes the field component transverse to the PIL and causes the fibrils to coalesce into long PIL-aligned filaments. Title: The Evolution of Photospheric Flows in Active Regions Authors: Muglach, K.; Schuck, P. W.; Hoeksema, J. T.; Sun, X.; Liu, Y. Bibcode: 2010AGUFMSH11A1605M Altcode: We will present first results of an analysis of the photospheric flow field in and around active region AR 11066. It emerged on 2nd May, 2010 near central meridian and developed into a small active region with simple bipolar structure. We will use SDO/HMI data to estimate the photospheric flow field applying the optical flow technique DAVE4VM (differential affine velocity estimator for vector magnetograms). Using both line-of-sight and vector magnetograms we will study the evolution of the photospheric flow velocity during the early stage of development of the active region. Title: Tracking Vector Magnetograms from the Solar Dynamics Observatory Authors: Schuck, P. W.; Sun, X.; Muglach, K.; Hoeksema, J. T. Bibcode: 2010AGUFMSH14A..07S Altcode: The differential affine velocity estimator for vector magnetograms (DAVE4VM) has been developed for estimating photospheric velocities. The accuracy of this technique has been demonstrated on synthetic magnetograms from MHD simulations. The algorithm was initially formulated in Cartesian coordinates. Thus, for best results, solar vector magnetograms must be transformed from the image plane into a Mercator map or some other Cartesian-like projection before applyng DAVE4VM. Recently, DAVE4VM has been modified to incorporate directly the projected spherical geometry of Helioprojective-Cartesian coordinates, thus permitting direct application of the method to image plane vector magnetograms. We will discuss the new algorithm and tests of the modified method and present first results of DAVE4VM applied to Solar Dynamics Observatory vector magnetograms. Title: Correlation Times of Solar Active Regions Authors: Muglach, Karin; Schuck, P. W.; Linton, M. G. Bibcode: 2010AAS...21640213M Altcode: 2010BAAS...41..875M The aim of this project is to determine the photospheric velocity field in solar magnetic regions. A systematic characterization of the flow field can provide important insight into the formation of active regions and filaments as well as the development of unstable magnetic configurations that lead to the initation of flares and coronal mass ejections. We plan to derive the flow fields from vector magnetograms obtained with the Stokes Polarimeter (SP) onboard the Hinode satellite and using the new optical flow technique DAVE4VM (differential affine velocity estimator for vector magnetograms). All local correlation tracking methods rely on comparing images (taken at different times) and deriving the spatial displacement of structures found in these images via a generalized cross-correlation. If the structures undergo significant development during the time the images are taken, the cross-correlation will not give meaningful results. As we will use magnetogram data for the tracking, we need to evaluate the temporal evolution and correlation times of the magnetic field vector B. We will determine the correlation times of the longitudinal and transverse components of the magnetic field vector in regions of different magnetic field strength and structure. This allows us to find the optimal cadence necessary for a good performance of the DAVE4VM code. Title: Understanding Solar Eruptions with SDO/HMI Measuring Photospheric Flows, Testing Models, and Steps Towards Forecasting Solar Eruptions Authors: Schuck, Peter W.; Linton, M.; Muglach, K.; Hoeksema, T. Bibcode: 2010AAS...21640214S Altcode: 2010BAAS...41Q.875S The Solar Dynamics Observatory (SDO) is carrying the first full-disk imaging vector magnetograph, the Helioseismic and Magnetic Imager (HMI), into an inclined geosynchronous orbit. This magnetograph will provide nearly continuous measurements of photospheric vector magnetic fields at cadences of 90 seconds to 12 minutes with 1" resolution, precise pointing, and unfettered by atmospheric seeing. The enormous data stream of 1.5 Terabytes per day from SDO will provide an unprecedented opportunity to understand the mysteries of solar eruptions. These ground-breaking observations will permit the application of a new technique, the differential affine velocity estimator for vector magnetograms (DAVE4VM), to measure photospheric plasma flows in active regions. These measurements will permit, for the first time, accurate assessments of the coronal free energy available for driving CMEs and flares. The details of photospheric plasma flows, particularly along magnetic neutral-lines, are critical to testing models for initiating coronal mass ejections (CMEs) and flares. Assimilating flows and fields into state-of-the art 3D MHD simulations that model the highly stratified solar atmosphere from the convection zone to the corona represents the next step towards achieving NASA's Living with a Star forecasting goals of predicting "when a solar eruption leading to a CME will occur." Our presentation will describe these major science and predictive advances that will be delivered by SDO/HMI. Title: Doppler-shift, Intensity, and Density Oscillations Observed with the Extreme Ultraviolet Imaging Spectrometer on Hinode Authors: Mariska, John T.; Muglach, K. Bibcode: 2010ApJ...713..573M Altcode: 2010arXiv1003.0420M Low-amplitude Doppler-shift oscillations have been observed in coronal emission lines in a number of active regions with the EUV Imaging Spectrometer (EIS) on the Hinode satellite. Both standing and propagating waves have been detected and many periods have been observed, but a clear picture of all the wave modes that might be associated with active regions has not yet emerged. In this study, we examine additional observations obtained with EIS in plage near an active region on 2007 August 22-23. We find Doppler-shift oscillations with amplitudes between 1 and 2 km s-1 in emission lines ranging from Fe XI 188.23 Å, which is formed at log T = 6.07, to Fe XV 284.16 Å, which is formed at log T = 6.32. Typical periods are near 10 minutes. We also observe intensity and density oscillations for some of the detected Doppler-shift oscillations. In the better-observed cases, the oscillations are consistent with upwardly propagating slow magnetoacoustic waves. Simultaneous observations of the Ca II H line with the Hinode Solar Optical Telescope Broadband Filter Imager show some evidence for 10 minute oscillations as well. Title: The three-dimensional structure of sunspots. II. The moat flow at two different heights Authors: Balthasar, H.; Muglach, K. Bibcode: 2010A&A...511A..67B Altcode: 2009arXiv0912.3661B