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Author name code: bothmer
ADS astronomy entries on 2022-09-14
author:"Bothmer, Volker" 

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Title: Near-Sun Observations of CMEs with WSIPR on Parker Solar
    Probe in April 2021
Authors: Bothmer, Volker; Chifu, Iulia
2022cosp...44.1461B    Altcode:
  During the pre-encounter days from April 20 to 27, 2021, more than
  20 CMEs have been identified in observations made by the WISPR inner
  telescope onboard the Parker Solar Probe (PSP) spacecraft. The WISPR
  CME observations reveal unprecedented fine structures compared to
  previous observations from near-Earth orbit. The PSP trajectory
  during the 8th encounter with a perihelion of below 15,7 solar radii
  on April 29, following its 4th Venus flyby in February 2021, was
  ideally suited to compare the WISPR observations with simultaneous
  STEREO/SECCHI/COR2A/HI1A and SOHO/LASCO/C2/C3 observations from
  near-Earth orbit and with observations of the low corona made in EUV
  wavelengths by SDO and STEREO/SECCHI/EUVI A. Here we present a summary
  of the physics characteristics of the observed CMEs, their near-Sun
  evolution and interactions seen in white-light. The identification
  of their solar origins in SDO/AIA and STEREO/EUVIA, and the results
  derived from the multipoint studies have important implications for a
  better understanding of the heliospheric manifestations of the solar
  photospheric and coronal magnetic fields.

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Title: On modeling ICME cross sections as static MHD columns
Authors: Bhattacharjee, Debesh; Nieves-Chinchilla, Teresa; Bothmer,
   Volker; Subramanian, Prasad; Vourlidas, Angelos
2022cosp...44.1376B    Altcode:
  Solar coronal mass ejections (CMEs) are observed to expand during
  their propagation through the solar wind. However, their cross-sections
  are usually modeled as static plasma columns within the framework of
  magnetohydrodynamics (MHD). In this study, we test the validity of
  this approach using in-situ plasma data from 151 magnetic clouds
  (MCs) observed by the WIND spacecraft and 45 observed by the
  Helios spacecrafts. We find that the most probable cross-section
  expansion speeds for the WIND events are only $\approx 0.06$ times
  the Alfvén speed inside the MCs while the most probable cross-section
  expansion speeds for the Helios MCs is $\approx 0.03$. Hence, the MC
  cross-sections can be considered approximately static over an Alfvén
  crossing timescale. Using estimates of electrical conductivity arising
  from Coulomb collisions, we find that the Lundquist number inside MCs is
  high ( $\approx 10^{13}$), suggesting that the MHD description is well
  justified. The Joule heating rates using our conductivity estimates
  are several orders of magnitude lower than the requirement for plasma
  heating inside MCs at 1 AU. The low heating rates are consistent
  with the MHD description which assumes no dissipation. However, the
  discrepancy with the heating requirement suggests possible departures
  from MHD and the need for a better understanding of plasma heating
  inside MCs.

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Title: Multi-spacecraft analysis of multi-CME events observed by
    WISPR on Parker Solar Probe in April 2021
Authors: Chifu, Iulia; Bothmer, Volker
2022cosp...44.1466C    Altcode:
  One week before Parker Solar Probe's (PSP) 8th perihelion, from 20
  to 27 April 2021, the Sun showed increased activity as manifested
  in the release of multiple CMEs into interplanetary space. Among
  these, we selected a series of three interacting CMEs identified
  in the observations of the WISPR-I telescope on 26 April and in the
  coronagraph images of STEREO-A/SECCHI/COR2 and HI and SOHO/LASCO/C2/C3
  on 25 April. We applied different methods for the 3D reconstruction of
  the CMEs in order to derive their physical properties and kinematics
  and to investigate potential in-situ crossings of the PSP trajectory. In
  one CME event, WISPR imaged details of a small flux rope that could be
  traced back to the Sun as identified from SDO and STEREO-A/SECCHI/EUVI
  observations. In this study, we present the results of the 3D
  reconstruction methods for these CME events.

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Title: Evolution of ICME sheath and leading-edge structure in the
    inner heliosphere
Authors: Temmer, Manuela; Bothmer, Volker
2022cosp...44.1439T    Altcode:
  We investigate a data sample of 40 interplanetary CME (ICME) events
  from Helios 1 and 2 data that cover the distance range 0.3-1au. For
  comparison, we add a sample of 5 ICMEs observed with Parker Solar
  Probe during 2018-2021. From the solar wind plasma and magnetic field
  measurements, we extract the ICME sub-structures sheath, leading-edge,
  and magnetic ejecta. We analyze their characteristic parameters as
  function of distance and present the main findings of this study: a)
  the average starting distance for actual sheath formation appears to
  be located at a distance of about 13 Rs; b) the sheath density becomes
  dominant over the magnetic ejecta density beyond 38 Rs; c) the sheath
  size could be related to the ambient solar wind density and magnetic
  ejecta characteristics; d) a local linear relation between sheath
  density and ambient solar wind speed was found; e) the leading-edge
  does not increase in size over distance and might be an isolated
  structure wedged in between sheath and magnetic ejecta. With Parker
  Solar Probe approaching the Sun as close as 10Rs, we will certainly
  detect more CME events to obtain measurements that might re-affirm
  the presented results. The current findings can be applied to help
  improve CME propagation models.

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Title: On Modeling ICME Cross-Sections as Static MHD Columns
Authors: Bhattacharjee, Debesh; Subramanian, Prasad; Bothmer, Volker;
   Nieves-Chinchilla, Teresa; Vourlidas, Angelos
2022SoPh..297...45B    Altcode: 2022arXiv220306996B
  Solar coronal mass ejections are well-known to expand as they propagate
  through the heliosphere. Despite this, their cross-sections are usually
  modeled as static plasma columns within the magnetohydrodynamics
  (MHD) framework. We test the validity of this approach using
  in-situ plasma data from 151 magnetic clouds (MCs) observed by
  the WIND spacecraft and 45 observed by the Helios spacecraft. We
  find that the most probable cross-section expansion speeds for the
  WIND events are only ≈0.06 times the Alfvén speed inside the MCs,
  while the most probable cross-section expansion speeds for the Helios
  events is ≈0.03 . MC cross-sections can thus be considered to be
  nearly static over an Alfvén crossing timescale. Using estimates
  of electrical conductivity arising from Coulomb collisions, we find
  that the Lundquist number inside MCs is high (≈10<SUP>13</SUP>),
  suggesting that the MHD description is well justified. The Joule
  heating rates using our conductivity estimates are several orders
  of magnitude lower than the requirement for plasma heating inside
  MCs near the Earth. While the (low) heating rates we compute are
  consistent with the MHD description, the discrepancy with the heating
  requirement points to possible departures from MHD and the need for
  a better understanding of plasma heating in MCs.

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Title: HiRISE - High-Resolution Imaging and Spectroscopy Explorer
    - Ultrahigh resolution, interferometric and external occulting
    coronagraphic science
Authors: Erdélyi, Robertus; Damé, Luc; Fludra, Andrzej; Mathioudakis,
   Mihalis; Amari, T.; Belucz, B.; Berrilli, F.; Bogachev, S.; Bolsée,
   D.; Bothmer, V.; Brun, S.; Dewitte, S.; de Wit, T. Dudok; Faurobert,
   M.; Gizon, L.; Gyenge, N.; Korsós, M. B.; Labrosse, N.; Matthews,
   S.; Meftah, M.; Morgan, H.; Pallé, P.; Rochus, P.; Rozanov, E.;
   Schmieder, B.; Tsinganos, K.; Verwichte, E.; Zharkov, S.; Zuccarello,
   F.; Wimmer-Schweingruber, R.
2022ExA...tmp...21E    Altcode:
  Recent solar physics missions have shown the definite role of waves and
  magnetic fields deep in the inner corona, at the chromosphere-corona
  interface, where dramatic and physically dominant changes occur. HiRISE
  (High Resolution Imaging and Spectroscopy Explorer), the ambitious new
  generation ultra-high resolution, interferometric, and coronagraphic,
  solar physics mission, proposed in response to the ESA Voyage 2050
  Call, would address these issues and provide the best-ever and most
  complete solar observatory, capable of ultra-high spatial, spectral,
  and temporal resolution observations of the solar atmosphere, from the
  photosphere to the corona, and of new insights of the solar interior
  from the core to the photosphere. HiRISE, at the L1 Lagrangian
  point, would provide meter class FUV imaging and spectro-imaging,
  EUV and XUV imaging and spectroscopy, magnetic fields measurements,
  and ambitious and comprehensive coronagraphy by a remote external
  occulter (two satellites formation flying 375 m apart, with a
  coronagraph on a chaser satellite). This major and state-of-the-art
  payload would allow us to characterize temperatures, densities, and
  velocities in the solar upper chromosphere, transition zone, and inner
  corona with, in particular, 2D very high resolution multi-spectral
  imaging-spectroscopy, and, direct coronal magnetic field measurement,
  thus providing a unique set of tools to understand the structure and
  onset of coronal heating. HiRISE's objectives are natural complements
  to the Parker Solar Probe and Solar Orbiter-type missions. We present
  the science case for HiRISE which will address: i) the fine structure
  of the chromosphere-corona interface by 2D spectroscopy in FUV at
  very high resolution; ii) coronal heating roots in the inner corona by
  ambitious externally-occulted coronagraphy; iii) resolved and global
  helioseismology thanks to continuity and stability of observing at the
  L1 Lagrange point; and iv) solar variability and space climate with,
  in addition, a global comprehensive view of UV variability.

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Title: Characteristics and evolution of sheath and leading edge
    structures of interplanetary coronal mass ejections in the inner
    heliosphere based on Helios and Parker Solar Probe observations
Authors: Temmer, Manuela; Bothmer, Volker
2022arXiv220204391T    Altcode:
  Aims: We statistically investigate the plasma and magnetic field
  characteristics of the upstream regions of interplanetary coronal mass
  ejections (ICMEs) and their evolution as function of distance to the Sun
  in the inner heliosphere. We use a sample of 40 well-observed ICMEs from
  Helios 1/2 (0.3-1au) and 5 from Parker Solar Probe (0.32-0.75au). For
  each event we identify four main density structures, namely shock,
  sheath, leading edge (LE), and magnetic ejecta (ME) itself. Methods:
  We derive separately for each structure averaged plasma and magnetic
  field parameter values as well as duration and place the results
  into comparison with the upstream solar wind (SW) to investigate the
  interrelation between the different density structures. Results:
  The sheath structure presumably consists of compressed plasma due
  to the turbulent SW material following the shock. The sheath lies
  ahead of a region of compressed ambient SW, the LE, which is typically
  found directly in front of the magnetic driver and seems to match the
  bright leading edge commonly observed in remote sensing observations of
  CMEs. The sheath becomes denser than the ambient SW at about 0.06au,
  which we interpret as the average starting distance for actual sheath
  formation. Between 0.09-0.28au the sheath structure density starts to
  dominate over the density within the ME. The ME density seems to fall
  below the ambient SW density over 0.45-1.07au. Besides the well-known
  expansion of the ME, the sheath size shows a weak positive correlation
  with distance, while the LE seems not to expand with distance from the
  Sun. We further find a moderate anti-correlation between sheath density
  and local SW plasma speed upstream of the ICME shock. An empirical
  relation is derived connecting the ambient SW speed with sheath and LE
  density that can be used for modeling of ICME evolution. Constraints
  to those results are given.

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Title: Comparing the Heliospheric Cataloging, Analysis, and Techniques
    Service (HELCATS) Manual and Automatic Catalogues of Coronal Mass
    Ejections Using Solar Terrestrial Relations Observatory/Heliospheric
    Imager (STEREO/HI) Data
Authors: Rodriguez, L.; Barnes, D.; Hosteaux, S.; Davies, J. A.;
   Willems, S.; Pant, V.; Harrison, R. A.; Berghmans, D.; Bothmer, V.;
   Eastwood, J. P.; Gallagher, P. T.; Kilpua, E. K. J.; Magdalenic, J.;
   Mierla, M.; Möstl, C.; Rouillard, A. P.; Odstrčil, D.; Poedts, S.
2022SoPh..297...23R    Altcode:
  We present the results of a comparative study between automatic
  and manually compiled coronal mass ejection (CME) catalogues based
  on observations from the Heliospheric Imagers (HIs) onboard NASA's
  Solar Terrestrial Relations Observatory (STEREO) spacecraft. Using
  the Computer Aided CME Tracking software(CACTus), CMEs are identified
  in HI data using an automatic feature-detection algorithm, while
  the Heliospheric Imagers Catalogue(HICAT) includes CMEs that are
  detected by visual inspection of HI images. Both catalogues were
  compiled as part of the EU FP7 Heliospheric Cataloguing, Analysis and
  Techniques Service (HELCATS) project (www.helcats-fp7.eu). We compare
  observational parameters of the CMEs from CACTus to those listed in
  HICAT, such as CME frequency, position angle (PA), and PA-width. We
  also compare CACTus-derived speeds to speeds derived from applying
  geometric modelling to the majority of the HICAT CMEs, the results
  of which are listed in the HELCATS Heliospheric Imagers Geometric
  Catalogue(HIGeoCAT). We find that both CACTus and HICAT catalogues
  contain a similar number of events when we exclude events narrower than
  20<SUP>∘</SUP>, which are not included in the HICAT catalogue but are
  found to be identified by CACTus. PA-distributions are strongly peaked
  around 90<SUP>∘</SUP> and 270<SUP>∘</SUP>, with a slightly larger
  CME frequency northwards of the equatorial plane (particularly for the
  STEREO-A versions of both catalogues). The CME PA-widths in both HICAT
  and CACTus catalogues peak at approximately 60<SUP>∘</SUP>. Manually
  derived speeds from HIGeoCAT and automatically derived speeds by
  CACTus correlate well for values lower than 1000 km s<SUP>−1</SUP>,
  in particular when CMEs are propagating close to the plane of the sky.

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Title: The magnetic flux rope structure of coronal mass ejections -
    2021 Julius Bartels Medal Lecture at vEGU
Authors: Bothmer, Volker
2021EGUGA..2311152B    Altcode:
  Magnetic clouds are transient solar wind flows in the interplanetary
  medium with smooth rotations of the magnetic field vector and low
  plasma beta values. The analysis of magnetic clouds identified in the
  data of the two Helios spacecraft between 0.3 and 1 AU showed that
  they can be interpreted to first order by force-free, large-scale,
  cylindrical magnetic flux tubes. A close correlation of their
  occurrences was found with disappearing filaments at the Sun. The
  magnetic clouds that originated from the northern solar hemisphere
  showed predominantly left-handed magnetic helicities and the ones from
  the southern hemisphere predominantly right-handed ones. They were
  often preceded by an interplanetary shock wave and some were found
  to be directly following a coronal mass ejection towards the Helios
  spacecraft as detected by the Solwind coronagraph on board the P78-1
  satellite. With the SOHO mission unprecedented long-term observations of
  coronal mass ejections (CMEs) were taken with the LASCO coronagraphs,
  with a spatial and time resolution that allowed to investigate their
  internal white-light fine structure. With complementary photospheric and
  EUV observations from SOHO, CMEs were found to arise from pre-existing
  small scale loop systems, overlying regions of opposite magnetic
  polarities. From the characteristic pattern of their source regions in
  both solar hemispheres, a generic scheme was presented in which their
  projected white-light topology depends primarily on the orientation and
  position of the source region"s neutral line on the solar disk. Based
  on this interpretation the graduated cylindrical shell method was
  developed, which allowed to model the electron density distribution of
  CMEs as 3D flux ropes. This concept was validated through stereoscopic
  observations of CMEs taken by the coronagraphs of the SECCHI remote
  sensing suite on board the twin STEREO spacecraft. The observations
  further revealed that the dynamic near-Sun evolution of CMEs often
  leads to distortions of their flux rope structure. However, the
  magnetic flux rope concept of CMEs is today one of the fundamental
  methods in space weather forecasts. With the Parker Solar Probe we
  currently observe for the first time CMEs in-situ and remotely at
  their birthplaces in the solar corona and can further unravel their
  origin and evolution from the corona into the heliosphere. This lecture
  provides a state-of-the-art overview on the magnetic structure of CMEs
  and includes latest observations from the Parker Solar Probe mission.

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Title: Analysis of signal to noise ratio in coronagraph observations
    of coronal mass ejections
Authors: Hinrichs, Johannes; Davies, Jackie A.; West, Matthew J.;
   Bothmer, Volker; Bourgoignie, Bram; Eyles, Chris J.; Huke, Philipp;
   Jiggens, Piers; Nicula, Bogdan; Tappin, James
2021JSWSC..11...11H    Altcode:
  We establish a baseline signal-to-noise ratio (SNR) requirement for the
  European Space Agency (ESA)-funded Solar Coronagraph for OPErations
  (SCOPE) instrument in its field of view of 2.5-30 solar radii based
  on existing observations by the Solar and Heliospheric Observatory
  (SOHO). Using automatic detection of coronal mass ejections (CMEs),
  we anaylse the impacts when SNR deviates significantly from our
  previously established baseline. For our analysis, SNR values are
  estimated from observations made by the C3 coronagraph on the Solar and
  Heliospheric Observatory (SOHO) spacecraft for a number of different
  CMEs. Additionally, we generate a series of artificial coronagraph
  images, each consisting of a modelled coronal background and a CME,
  the latter simulated using the graduated cylindrical shell (GCS)
  model together with the SCRaytrace code available in the Interactive
  Data Language (IDL) SolarSoft library. Images are created with CME
  SNR levels between 0.5 and 10 at the outer edge of the field of view
  (FOV), generated by adding Poisson noise, and velocities between 700
  km s<SUP>-1</SUP> and 2800 km s<SUP>-1</SUP>. The images are analysed
  for the detectability of the CME above the noise with the automatic
  CME detection tool CACTus. We find in the analysed C3 images that CMEs
  near the outer edge of the field of view are typically 2% of the total
  brightness and have an SNR between 1 and 4 at their leading edge. An SNR
  of 4 is defined as the baseline SNR for SCOPE. The automated detection
  of CMEs in our simulated images by CACTus succeeded well down to SNR =
  1 and for CME velocities up to 1400 km s<SUP>-1</SUP>. At lower SNR
  and higher velocity of ≥ 2100 km s<SUP>-1</SUP> the detection started
  to break down. For SCOPE, the results from the two approaches confirm
  that the initial design goal of SNR = 4 would, if achieved, deliver a
  comparable performance to established data used in operations today,
  with a more compact instrument design, and a margin in SNR before
  existing automatic detection produces significant false positives.

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Title: CMEs in the Heliosphere: III. A Statistical Analysis of the
    Kinematic Properties Derived from Stereoscopic Geometrical Modelling
    Techniques Applied to CMEs Detected in the Heliosphere from 2008 to
    2014 by STEREO/HI-1
Authors: Barnes, D.; Davies, J. A.; Harrison, R. A.; Byrne, J. P.;
   Perry, C. H.; Bothmer, V.; Eastwood, J. P.; Gallagher, P. T.; Kilpua,
   E. K. J.; Möstl, C.; Rodriguez, L.; Rouillard, A. P.; Odstrčil, D.
2020SoPh..295..150B    Altcode: 2020arXiv200614879B
  We present an analysis of coronal mass ejections (CMEs) observed
  by the Heliospheric Imagers (HIs) onboard NASA's Solar Terrestrial
  Relations Observatory (STEREO) spacecraft. Between August 2008 and
  April 2014 we identify 273 CMEs that are observed simultaneously,
  by the HIs on both spacecraft. For each CME, we track the observed
  leading edge, as a function of time, from both vantage points,
  and apply the Stereoscopic Self-Similar Expansion (SSSE) technique
  to infer their propagation throughout the inner heliosphere. The
  technique is unable to accurately locate CMEs when their observed
  leading edge passes between the spacecraft; however, we are able to
  successfully apply the technique to 151, most of which occur once the
  spacecraft-separation angle exceeds 180<SUP>∘</SUP>, during solar
  maximum. We find that using a small half-width to fit the CME can
  result in inferred acceleration to unphysically high velocities and that
  using a larger half-width can fail to accurately locate the CMEs close
  to the Sun because the method does not account for CME over-expansion
  in this region. Observed velocities from SSSE are found to agree well
  with single-spacecraft (SSEF) analysis techniques applied to the same
  events. CME propagation directions derived from SSSE and SSEF analysis
  agree poorly because of known limitations present in the latter.

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Title: The Solar Orbiter Heliospheric Imager (SoloHI)
Authors: Howard, R. A.; Vourlidas, A.; Colaninno, R. C.; Korendyke,
   C. M.; Plunkett, S. P.; Carter, M. T.; Wang, D.; Rich, N.; Lynch,
   S.; Thurn, A.; Socker, D. G.; Thernisien, A. F.; Chua, D.; Linton,
   M. G.; Koss, S.; Tun-Beltran, S.; Dennison, H.; Stenborg, G.; McMullin,
   D. R.; Hunt, T.; Baugh, R.; Clifford, G.; Keller, D.; Janesick, J. R.;
   Tower, J.; Grygon, M.; Farkas, R.; Hagood, R.; Eisenhauer, K.; Uhl,
   A.; Yerushalmi, S.; Smith, L.; Liewer, P. C.; Velli, M. C.; Linker,
   J.; Bothmer, V.; Rochus, P.; Halain, J. -P.; Lamy, P. L.; Auchère,
   F.; Harrison, R. A.; Rouillard, A.; Patsourakos, S.; St. Cyr, O. C.;
   Gilbert, H.; Maldonado, H.; Mariano, C.; Cerullo, J.
2020A&A...642A..13H    Altcode:
  <BR /> Aims: We present the design and pre-launch performance of
  the Solar Orbiter Heliospheric Imager (SoloHI) which is an instrument
  prepared for inclusion in the ESA/NASA Solar Orbiter mission, currently
  scheduled for launch in 2020. <BR /> Methods: The goal of this paper
  is to provide details of the SoloHI instrument concept, design, and
  pre-flight performance to give the potential user of the data a better
  understanding of how the observations are collected and the sources
  that contribute to the signal. <BR /> Results: The paper discusses
  the science objectives, including the SoloHI-specific aspects, before
  presenting the design concepts, which include the optics, mechanical,
  thermal, electrical, and ground processing. Finally, a list of planned
  data products is also presented. <BR /> Conclusions: The performance
  measurements of the various instrument parameters meet or exceed the
  requirements derived from the mission science objectives. SoloHI is
  poised to take its place as a vital contributor to the science success
  of the Solar Orbiter mission.

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Title: High resolution multi-viewpoint observations of CME kinematics
    and dynamics
Authors: Mrotzek, Niclas; Bothmer, Volker
2020EGUGA..2222532M    Altcode:
  Coronal mass ejections (CMEs) are impulsive outbursts of coronal
  plasma bound in magnetic structures. Their initiation and evolution
  into the heliosphere covers several orders of magnitude of temporal and
  spatial scales that can be observed with space-borne extreme ultraviolet
  imagers, coronagraphs and heliospheric imagers. In this work we present
  a systematic investigation of the early dynamics of CMEs including their
  kinematics, orientation and geometrical evolution. For this purpose, a
  dedicated set of 21 Earth-directed CMEs between July 2011 and November
  2012 was selected and analyzed. The CME parametrization is obtained
  by applying a 3D modelling method, the Graduated Cylindrical Shell
  (GCS) model, to simultaneous multi-viewpoint observations taken with
  the SECCHI instrument suite onboard the twin STEREO spacecraft and
  with the LASCO coronagraphs onboard the SOHO satellite. By using
  these instruments, the CME dynamics including the kinematics and
  geometry, are covered in high detail over a wide spatial range. For
  the majority of events it started in the field of view of EUVI below 2
  solar radii and extended into the field of view of HI1 up to 100 solar
  radii. The results reveal interactions of the CMEs with the ambient
  solar wind. CME deflections of up to 31° in longitude and 18° in
  latitude were measured within the first 30 solar radii. Furthermore,
  evidence of CME oscillations with periods between 29 and 93 minutes
  were found. The analysis provides important implications for more
  reliable space weather forecasts and further analysis through the new
  observations from Parker Solar Probe and Solar Orbiter.

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Title: Simulating White-Light Images of Coronal Structures for Parker
Solar Probe/WISPR: Study of the Total Brightness Profiles
Authors: Nisticò, Giuseppe; Bothmer, Volker; Vourlidas, Angelos;
   Liewer, Paulett C.; Thernisien, Arnaud F.; Stenborg, Guillermo;
   Howard, Russell A.
2020SoPh..295...63N    Altcode: 2020arXiv200405447N
  The Wide-field Imager for Parker Solar Probe (WISPR) captures
  unprecedented white-light images of the solar corona and inner
  heliosphere. Thanks to the uniqueness of the Parker Solar Probe's
  (PSP) orbit, WISPR is able to image "locally" coronal structures at
  high spatial and time resolutions. The observed plane of sky, however,
  rapidly changes because of the PSP's high orbital speed. Therefore,
  the interpretation of the dynamics of the coronal structures recorded
  by WISPR is not straightforward. A first study, undertaken by Liewer et
  al. (Solar Phys.294, 93, 2019), shows how different coronal features
  (e.g., streamers, flux ropes) appear in the field-of-view of WISPR
  by means of raytracing simulations. In particular, they analyze
  the effects of the spatial resolution changes on both the images
  and the associated height-time maps, and introduce the fundamentals
  for geometric triangulation. In this follow-up paper, we focus on
  the study of the total brightness of a simple, spherical, plasma
  density structure, to understand how the analysis of Thomson-scattered
  emission by the electrons in a coronal feature can shed light into the
  determination of its kinematic properties. We investigate two cases:
  (i) a density sphere at a constant distance from the Sun for different
  heliographic longitudes; (ii) a density sphere moving outwardly with
  constant speed. The study allows us to characterize the effects of
  the varying heliocentric distance of the observer and scattering angle
  on the total brightness observed, which we exploit to contribute to a
  better determination of the position and speed of the coronal features
  observed by WISPR.

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Title: Imaging the Solar Corona From Within
Authors: Hess, P.; Howard, R.; Vourlidas, A.; Bothmer, V.; Colaninno,
   R.; DeForest, C.; Gallagher, B.; Hall, J. R.; Higginson, A.; Korendyke,
   C.; Kouloumvakos, A.; Lamy, P.; Liewer, P.; Linker, J.; Linton, M.;
   Penteado, P.; Plunkett, S.; Poirer, N.; Raouafi, N.; Rich, N.; Rochus,
   P.; Rouillard, A.; Socker, D.; Stenborg, G.; Thernisien, A.; Viall, N.
2020AAS...23514907H    Altcode:
  Parker Solar Probe (PSP), launched, in August 2018 is humanity's
  first probe of a stellar atmosphere. It will make measurements of
  the near-Sun plasma from 'within' the outer corona with gradually
  reduced perihelia from its first perihelia of 35 Rs in 2018-19 to 9.8
  Rs in 2025. Here we report the results from the imaging observations
  of the electron and dust corona, whe PSP was 35-54 Rs from the solar
  surface, taken by the Wide-field Imager for Solar Probe (WISPR). The
  spacecraft was near-corotating with the solar corona throughout the
  observing window, which is an unprecedented situation for any type of
  coronal imaging. Our initial analysis uncovers a long-hypothesized
  depletion of the primordial dust orbiting near the Sun, reveals the
  plasma structure of small-scale ejections, and provides a strict test
  for validating model predictions of the large-scale configuration of
  the coronal plasma. Thus, WISPR imaging allows the study of near-Sun
  dust dynamics as the mission progresses. The high-resolution images
  of small transients, largely unresolved from 1 AU orbits, unravel
  the sub-structures of small magnetic flux ropes and show that the
  Sun continually releases helical magnetic fields in the background
  wind. Finally, WISPR's observations of the coronal streamer evolution
  confirm the large-scale topology of the solar corona but they also
  reveal that, as recently predicted, streamers are composed of yet
  smaller sub-streamers channeling continual density fluctuations at
  all visible scales.

---------------------------------------------------------
Title: Imaging the Solar Corona from Within: First Results from the
    Parker Solar Probe Telescope
Authors: Howard, R. A.; Vourlidas, A.; Bothmer, V.; Colaninno, R. C.;
   DeForest, C.; Gallagher, B.; Hall, J. R.; Hess, P.; Higginson, A. K.;
   Korendyke, C.; Kouloumvakos, A.; Lamy, P.; Liewer, P. C.; Linker, J.;
   Linton, M.; Penteado, P. F.; Plunkett, S. P.; Poirier, N.; Raouafi,
   N.; Rich, N.; Rochus, P. L.; Rouillard, A. P.; Socker, D. G.; Stenborg,
   G.; Thernisien, A.; Viall, N. M.
2019AGUFMSH11A..04H    Altcode:
  Parker Solar Probe (PSP) launched in August 2018 is humanity's
  first probe of a stellar atmosphere. It will make measurements of
  the near-Sun plasma from 'within' the outer corona with gradually
  reduced perihelia from its first perihelia of 35 Rs in 2018-19 to 9.8
  Rs in 2025. Here we report the results from the imaging observations
  of the electron and dust corona, whe PSP was 35-54 Rs from the solar
  surface, taken by the Wide-field Imager for Solar Probe (WISPR). The
  spacecraft was near-corotating with the solar corona throughout the
  observing window, which is an unprecedented situation for any type of
  coronal imaging. Our initial analysis uncovers a long-hypothesized
  depletion of the primordial dust orbiting near the Sun, reveals the
  plasma structure of small-scale ejections, and provides a strict test
  for validating model predictions of the large-scale configuration of
  the coronal plasma. Thus, WISPR imaging allows the study of near-Sun
  dust dynamics as the mission progresses. The high-resolution images
  of small transients, largely unresolved from 1 AU orbits, unravel
  the sub-structures of small magnetic flux ropes and show that the
  Sun continually releases helical magnetic fields in the background
  wind. Finally, WISPR's observations of the coronal streamer evolution
  confirm the large-scale topology of the solar corona but they also
  reveal that, as recently predicted, streamers are composed of yet
  smaller sub-streamers channeling continual density fluctuations at
  all visible scales.

---------------------------------------------------------
Title: The Solar Orbiter Heliospheric Imager (SoloHI) for the Solar
Orbiter Mission: Science and Instrument Status
Authors: Vourlidas, A.; Howard, R. A.; Colaninno, R. C.; Korendyke,
   C.; Thernisien, A.; Linton, M.; Tun Beltran, S.; Liewer, P. C.; Velli,
   M.; Linker, J.; Bothmer, V.; Rochus, P. L.; Lamy, P. L.
2019AGUFMSH24A..08V    Altcode:
  The SoloHI instrument has completed its development effort and has been
  integrated onto the Solar Orbiter spacecraft. The mission, scheduled
  for launch in February 2020, will undergo gravity assist maneuvers
  around Venus to change both the perihelion distance as well as the
  plane of the orbit to ultimately achieve a minimum perihelion of 0.28
  AU and an orbital inclination of about 35° relative to the ecliptic
  plane. The remote sensing instruments will operate for three 10-day
  periods out of the nominal 6-month orbit. SoloHI detects sunlight
  scattered by free electrons in the corona and solar wind from 5° to
  45° elongation in visible wavelengths, providing linkage between solar
  and solar wind observations. The science investigation focuses mainly on
  the solar wind, including streamers, small-scale intensity and density
  fluctuations, jets, and Coronal Mass Ejections (CMEs). SoloHI is very
  similar to the HI-1 instrument on STEREO/SECCHI but with double the FOV
  of HI-1. In this paper, we present our preparations for the mission
  including the instrument status, our science planning strategy, our
  observing plans for cruise phase, calibrations, early science and our
  low-latency and science data products <P />This work has been supported
  by NASA.

---------------------------------------------------------
Title: Challenges in the Analysis of Images from the Wide-field Imager
    (WISPR) on Parker Solar Probe
Authors: Liewer, P. C.; Hall, J. R.; Penteado, P.; Vourlidas, A.;
   Thernisien, A.; Howard, R. A.; Qiu, J.; Nistico, G.; Bothmer, V.
2019AGUFMSH23A..09L    Altcode:
  The three-to-five-month highly elliptical orbit of Parker Solar Probe
  (PSP), approaching within 10 solar radii of the Sun, will allow the
  Wide-field Imager for Solar Probe (WISPR) to view the corona with
  unprecedented spatial resolution from multiple viewpoints. WISPR,
  located on the ram side of PSP, will image and fly through structures
  sample by the in situ instruments. WISPR has a wide fixed angular
  field-of-view (FOV), extending radially from 13.5° to 108° from
  the Sun and approximately 50° in the transverse direction, but the
  physical extent of the imaged coronal region varies directly with the
  distance of the spacecraft from the Sun. Challenges to interpreting
  the motion of density features seen in the WISPR images come from the
  wide and changing field-of-view and the unknown extent of the region
  of the coronal that co-rotates with the Sun. To relate and compare
  features seen in the images to observation by other instruments and
  spacecraft with other locations and viewpoints, it is necessary to
  relate the field-of-view of the WISPR telescopes at any given time
  to other frames of reference, such as the various Heliographic and
  Heliocentric coordinate systems. Here we discuss re-projections of
  WISPR images into several frames, made utilizing the World Coordinate
  System, which relies on information in the images' FITS headers
  (see W. T. Thompson, 2006, DOI: 10.1051/0004 6361:20054262). We will
  present methods for creating elongation vs. time images (J-maps)
  for WISPR images and also a technique for tracking observed density
  features to determine their 3D trajectories. These methods will be
  illustrated using data from WISPR's first encounters with the Sun.

---------------------------------------------------------
Title: Near-Sun observations of an F-corona decrease and K-corona
    fine structure
Authors: Howard, R. A.; Vourlidas, A.; Bothmer, V.; Colaninno, R. C.;
   DeForest, C. E.; Gallagher, B.; Hall, J. R.; Hess, P.; Higginson,
   A. K.; Korendyke, C. M.; Kouloumvakos, A.; Lamy, P. L.; Liewer, P. C.;
   Linker, J.; Linton, M.; Penteado, P.; Plunkett, S. P.; Poirier, N.;
   Raouafi, N. E.; Rich, N.; Rochus, P.; Rouillard, A. P.; Socker, D. G.;
   Stenborg, G.; Thernisien, A. F.; Viall, N. M.
2019Natur.576..232H    Altcode:
  Remote observations of the solar photospheric light scattered by
  electrons (the K-corona) and dust (the F-corona or zodiacal light)
  have been made from the ground during eclipses<SUP>1</SUP> and from
  space at distances as small as 0.3 astronomical units<SUP>2-5</SUP> to
  the Sun. Previous observations<SUP>6-8</SUP> of dust scattering have
  not confirmed the existence of the theoretically predicted dust-free
  zone near the Sun<SUP>9-11</SUP>. The transient nature of the corona
  has been well characterized for large events, but questions still
  remain (for example, about the initiation of the corona<SUP>12</SUP>
  and the production of solar energetic particles<SUP>13</SUP>) and
  for small events even its structure is uncertain<SUP>14</SUP>. Here
  we report imaging of the solar corona<SUP>15</SUP> during the first
  two perihelion passes (0.16-0.25 astronomical units) of the Parker
  Solar Probe spacecraft<SUP>13</SUP>, each lasting ten days. The view
  from these distances is qualitatively similar to the historical views
  from ground and space, but there are some notable differences. At
  short elongations, we observe a decrease in the intensity of the
  F-coronal intensity, which is suggestive of the long-sought dust
  free zone<SUP>9-11</SUP>. We also resolve the fine-scale plasma
  structure of very small eruptions, which are frequently ejected from
  the Sun. These take two forms: the frequently observed magnetic flux
  ropes<SUP>12,16</SUP> and the predicted, but not yet observed, magnetic
  islands<SUP>17,18</SUP> arising from the tearing-mode instability in
  the current sheet. Our observations of the coronal streamer evolution
  confirm the large-scale topology of the solar corona, but also reveal
  that, as recently predicted<SUP>19</SUP>, streamers are composed of
  yet smaller substreamers channelling continual density fluctuations
  at all visible scales.

---------------------------------------------------------
Title: SCOPE: a coronagraph for operational space weather prediction:
    phase A/B1 design and breadboarding
Authors: Middleton, Kevin F.; Anwand, Heiko; Bothmer, Volker; Davies,
   Jackie A.; Earle, Andrew; Ergenzinger, Klaus; Eyles, Chris J.; Hardie,
   Robert; Hellin, Marie-Laure; Hinrichs, Johannes; Huke, Philipp;
   Jiggens, Piers; Kirschner, Volker; Mazy, Emmanuel; McCarron, Thomas;
   Nicula, Bogdan; Stopfkuchen, Lars; Tappin, S. James; Tosh, Ian A. J.;
   Waltham, Nick R.; West, Matthew J.
2019SPIE11180E..3AM    Altcode:
  Accurate prediction of the arrival of solar wind phenomena, in
  particular coronal mass ejections (CMEs), is becoming more important
  given our ever-increasing reliance on technology. SCOPE is a coronagraph
  specifically optimised for operational space weather prediction,
  designed to provide early evidence of Earth-bound CMEs. In this paper,
  we present results from phase A/B1 of the instrument's development,
  which included conceptual design and a program of breadboard testing. We
  describe the conceptual design of the instrument. In particular, we
  explain the design and analysis of the straylight rejection baffles and
  occulter needed to block the image of the solar disc, in order to render
  the much fainter corona visible. We discuss the development of in-house
  analysis code to predict the straylight diffraction effects that limit
  the instrument's performance, and present results, which we compare
  against commercially available analysis tools and the results from
  breadboard testing. In particular, we discuss some of the challenges
  of predicting straylight effects in this type of instrument and the
  methods we have developed for overcoming them. We present the test
  results from an optical breadboard, designed to verify the end-to-end
  straylight rejection of the instrument. The design and development
  of both the breadboard and the test facility is presented. We discuss
  some of the challenges of measuring very low levels of straylight and
  how these drive the breadboard and test facility design. We discuss
  the test and analysis procedures developed to ensure a representative,
  complete characterisation of the instrument's straylight response.

---------------------------------------------------------
Title: Simulating White Light Images of Coronal Structures for WISPR/
Parker Solar Probe: Effects of the Near-Sun Elliptical Orbit
Authors: Liewer, P.; Vourlidas, A.; Thernisien, A.; Qiu, J.; Penteado,
   P.; Nisticò, G.; Howard, R.; Bothmer, V.
2019SoPh..294...93L    Altcode:
  The three-to-five-month elliptical orbit of Parker Solar Probe
  (PSP), approaching within 10 solar radii of the Sun, will allow the
  Wide-field Imager for Solar Probe (WISPR) to view the corona with
  unprecedented spatial resolution from multiple viewpoints. WISPR has
  a wide fixed angular field of view, extending from 13.5<SUP>∘</SUP>
  to 108<SUP>∘</SUP> from the Sun and approximately 50<SUP>∘</SUP>
  in the transverse direction, but the physical extent of the imaged
  coronal region varies directly with the distance of the spacecraft from
  the Sun. In a solar encounter period of approximately 10 days around
  perihelion, PSP covers over 100 - 200° of heliographic longitude and
  the distance from the Sun varies by a factor of two to five. In this
  paper, we use synthetic white-light images to study the effects of the
  rapid elliptical orbit on the images that can be anticipated for WISPR's
  observations. We find that sequences of images can help identify coronal
  density features that will be sampled by in-situ instruments. We also
  find that the multiple viewpoints, provided by the rapid motion near
  perihelion, can be used to obtain three-dimensional information on
  the coronal density features.

---------------------------------------------------------
Title: CMEs in the Heliosphere: II. A Statistical Analysis of the
    Kinematic Properties Derived from Single-Spacecraft Geometrical
    Modelling Techniques Applied to CMEs Detected in the Heliosphere
    from 2007 to 2017 by STEREO/HI-1
Authors: Barnes, D.; Davies, J. A.; Harrison, R. A.; Byrne, J. P.;
   Perry, C. H.; Bothmer, V.; Eastwood, J. P.; Gallagher, P. T.; Kilpua,
   E. K. J.; Möstl, C.; Rodriguez, L.; Rouillard, A. P.; Odstrčil, D.
2019SoPh..294...57B    Altcode:
  Recent observations with the Heliospheric Imagers (HIs) onboard the twin
  NASA Solar Terrestrial Relations Observatory (STEREO) spacecraft have
  provided unprecedented observations of a large number of coronal mass
  ejections (CMEs) in the inner heliosphere. In this article we discuss
  the generation of the HIGeoCAT CME catalogue and perform a statistical
  analysis of its events. The catalogue was generated as part of the
  EU FP7 HELCATS (Heliospheric Cataloguing, Analysis and Techniques
  Service) project (www.helcats-fp7.eu/). It is created by generating
  time/elongation maps for CMEs using observations from the inner (HI-1)
  and outer (HI-2) cameras along a position angle close to the CME
  apex. Next, we apply single-spacecraft geometric-fitting techniques
  to determine the kinematic properties of these CMEs, including their
  speeds, propagation directions, and launch times. The catalogue contains
  a total of 1455 events (801 from STEREO-A and 654 from STEREO-B)
  from April 2007 to the end of August 2017. We perform a statistical
  analysis of the properties of CMEs in HIGeoCAT and compare the results
  with those from the Large Angle Spectrometric Coronagraph (LASCO) CDAW
  catalogues (Yashiro et al.J. Geophys. Res. Space Phys.109, A07105,
  2004) and the COR-2 catalogue of Vourlidas et al. (Astrophys. J.838,
  141, 2004) during the same period. We find that the distributions of
  both speeds and latitudes for the HIGeoCAT CMEs correlate with the
  sunspot number over the solar cycle. We also find that the HI-derived
  CME speed distributions are generally consistent with coronagraph
  catalogues over the solar cycle, albeit with greater absolute speeds
  due to the differing methods with which each is derived.

---------------------------------------------------------
Title: What we know and don't know about coronal mass ejections -
    The answer is blowing in my presentation
Authors: Bothmer, Volker
2019EGUGA..2110529B    Altcode:
  In the same year the first interplanetary shock waves were discovered
  in the solar wind through in-situ measurements the famous song "Blowing
  in the Wind" was released by Bob Dylan. From that time on more and more
  advanced space observations of the Sun and the interplanetary medium
  have provided fundamental insights into the physics of coronal mass
  ejections (CMEs) and their heliospheric evolution. I will review our
  current understanding of CMEs, which is of extreme importance today to
  help facilitate reliable space weather predictions in the near future. I
  will also point out challenging remaining questions that need to be
  answered by future investigations. My historical walkthrough of key
  CME research will be presented from the watchtower of a space scientist
  in the context of Dylan's famous lyrics since we know "the times they
  are a-changin".

---------------------------------------------------------
Title: Raytracing simulations of Parker Solar Probe/WISPR images
Authors: Nisticò, Giuseppe; Liewer, Paulett; Vourlidas, Angelos;
   Thernisien, Arnaud; Howard, Russell; Bothmer, Volker
2019EGUGA..2114202N    Altcode:
  The Wide-field Imager for Parker Solar Probe (WISPR) provides
  unprecedented white-light images of the solar corona and inner
  heliosphere from unconventional viewpoints thanks to the close
  perihelion transits of Parker Solar Probe. WISPR images coronal
  structures at high spatial and time resolutions, but the data
  analysis needs to consider the continuous change of the observation's
  plane-of-sky and hence of the projection due to PSP's fast orbital
  speed and high orbital eccentricity. Therefore, it is important to
  understand how these factors affect the images. Here, we present an
  analysis of simulated WISPR images and discuss how WISPR data can
  be analyzed to study the physical conditions of the corona and the
  near-Sun environment.

---------------------------------------------------------
Title: Combined geometrical modelling and white-light mass
    determination of coronal mass ejections
Authors: Pluta, Adam; Mrotzek, Niclas; Vourlidas, Angelos; Bothmer,
   Volker; Savani, Neel
2019A&A...623A.139P    Altcode:
  Context. We use forward modelling on multi-viewpoint coronagraph
  observations to estimate the 3-dimensional morphology, initial speed
  and deprojected masses of Coronal Mass Ejections (CMEs). The CME
  structure is described via the Graduated Cylindrical Shell (GCS) model,
  which enables the measurement of CME parameters in a consistent and
  comparable manner. <BR /> Aims: This is the first large-scale use of the
  GCS model to estimate CME masses, so we discuss inherent peculiarities
  and implications for the mass determination with a special focus on CME
  events emerging from close to the observer's central meridian. Further,
  we analyse the CME characteristics best suited to estimate the CME mass
  in a timely manner to make it available to CME arrival predictions. <BR
  /> Methods: We apply the method to a set of 122 bright events observed
  simultaneously from two vantage points with the COR2 coronagraphs
  onboard of the twin NASA STEREO spacecraft. The events occurred between
  January 2007 and December 2013 and are compiled in an online catalogue
  within the EU FP7 project HELCATS. We statistically analyse the derived
  CME parameters, their mutual connection and their relation to the solar
  cycle. <BR /> Results: We show that the derived morphology of intense
  disk events is still systematically overestimated by up to a factor of
  2 with stereoscopic modelling, which is the same order of magnitude as
  for observations from only one vantage point. The overestimation is very
  likely a combination of projection effects as well as the increased
  complexity of separating CME shocks and streamers from CME fronts
  for such events. We further show that CME mass determination of disk
  events can lead to overestimation of the mass by about a factor of 10
  or more, in case of overlapping bright structures. <BR /> Conclusions:
  We conclude that for stereoscopic measurements of disk events, the
  measurement of the initial CME speed is the most reliable one. We
  further suggest that our presented CME speed-mass correlation is most
  suited to estimate the CME mass early from coronagraph observations.

---------------------------------------------------------
Title: Observing the corona and inner heliosphere with Parker
    Solar Probe
Authors: Nisticò, G.; Bothmer, V.; Liewer, P.; Vourlidas, , A.;
   Thernisien, A.
2019NCimC..42...21N    Altcode:
  The recently launched Parker Solar Probe (PSP) mission is expected
  to provide unprecedented views of the solar corona and inner
  heliosphere. In addition to instruments devoted to taking measurements
  of the local solar wind, the spacecraft carries a visible imager: the
  Wide-field Imager for Solar PRobe (WISPR). WISPR will take advantage
  of the proximity of the spacecraft to the Sun to perform local imaging
  of the near-Sun environment. WISPR will observe coronal structures at
  high spatial and time resolutions, although the observed plane-of-sky
  will rapidly change because of the fast transit at the perihelia. We
  present a concise description of the PSP mission, with particular
  regard to the WISPR instrument, discussing its main scientific goals,
  targets of observations, and outlining the possible synergies with
  current and upcoming space missions.

---------------------------------------------------------
Title: Oscillations of cometary tails: a vortex shedding phenomenon?
Authors: Nisticò, G.; Vladimirov, V.; Nakariakov, V. M.; Battams,
   K.; Bothmer, V.
2018A&A...615A.143N    Altcode: 2018arXiv180400997N
  Context. During their journey to perihelion, comets may appear in the
  field of view of space-borne optical instruments, showing in some
  cases a nicely developed plasma tail extending from their coma and
  exhibiting an oscillatory behaviour. <BR /> Aims: The oscillations of
  cometary tails may be explained in terms of vortex shedding because of
  the interaction of the comet with the solar wind streams. Therefore,
  it is possible to exploit these oscillations in order to infer the
  value of the Strouhal number S t, which quantifies the vortex shedding
  phenomenon, and the physical properties of the local medium. <BR />
  Methods: We used the Heliospheric Imager (HI) data of the Solar
  TErrestrial Relations Observatory (STEREO) mission to study the
  oscillations of the tails of comets 2P/Encke and C/2012 S1 (ISON) during
  their perihelion in Nov 2013. We determined the corresponding Strouhal
  numbers from the estimates of the halo size, the relative speed of the
  solar wind flow, and the period of the oscillations. <BR /> Results:
  We found that the estimated Strouhal numbers are very small, and the
  typical value of S t 0.2 would be extrapolated for size of the halo
  larger than 10<SUP>6</SUP> km. <BR /> Conclusions: Although the vortex
  shedding phenomenon has not been unambiguously revealed, the findings
  suggest that some kind of magnetohydrodynamic (MHD) instability process
  is responsible for the observed behaviour of cometary tails, which
  can be exploited for probing the physical conditions of the near-Sun
  region. <P />The movies associated to Figs. 1 and 4 are available at <A
  href="http://www.aanda.org/10.1051/0004-6361/201732474/olm">http://www.aanda.org</A>

---------------------------------------------------------
Title: Probing the inner heliosphere with comets
Authors: Nisticò, Giuseppe; Vladimirov, Vangelis; Nakariakov, Valery
   M.; Battams, Karl; Bothmer, Volker
2018shin.confE..41N    Altcode:
  Optical instruments aboard space missions have recently provided
  us with exciting observations of comets in the vicinity of their
  perihelion. At this stage, a tail of dust and ions from the comet
  nucleus is formed, which interacts with the local solar wind flow and
  exhibits an oscillatory dynamics. The observed phenomenon is attributed
  to the formation of a Kármán vortex street in the wake of the cometary
  coma, whose properties depend upon the characteristics of the comet
  itself and the local medium. We present observations of the comets
  Encke and ISON detected in 2013 with the Heliospheric Imager aboard
  the STEREO spacecraft, and discuss the possibility to exploit comets
  as natural probes of the inner heliosphere, by relating the physical
  behaviour of cometary tails with the local conditions of the solar wind.

---------------------------------------------------------
Title: Preparing for Parker Solar Probe: Tracking Moving Solar Wind
    Features in Images from the Wide-field Imager for Parker Solar Probe
    (WISPR)
Authors: Liewer, Paulett C.; Qiu, Jiong; Nisticò, Giuseppe;
   Vourlidas, Angelos; Penteado, Paulo; Thernisien, Arnaud; Howard,
   Russell; Bothmer, Volker
2018shin.confE..43L    Altcode:
  The Parker Solar Probe (PSP) trajectory, approaching within 10 solar
  radii, will allow the white light imager, WISPR, to view the inner
  corona with unprecedented spatial resolution. WISPR, with a field of
  view extending from 13.5° to 108° elongation angle from the Sun,
  will image the fine-scale coronal structure with arcminute resolution
  at high cadence ( 5 - 60 min). The dependency of Thomson scattering on
  the distance between the observer and the Sun dictates that WISPR will
  be a “local" heliospheric imager, and thus can provide a crucial link
  between the visible corona and PSP's in-situ measurements. To prepare
  for this unprecedented viewing of the structures in the inner corona,
  we are creating synthetic white light images and animations, viewed from
  the PSP trajectory, using the white-light ray-tracing package developed
  at NRL (available through SolarSoft). We will present results for small
  flux ropes moving outward through the corona as well as fly-throughs
  of finely structured coronal streamers. We also investigated whether
  the 3-D trajectory (direction and velocity) of a density enhancement
  (flux rope or

---------------------------------------------------------
Title: Simulations of PSP/WISPR observations of the corona/inner
    heliosphere with raytracing software
Authors: Nisticò, Giuseppe; Liewer, Paulett; Qiu, Jiong; Vourlidas,
   Angelos; Bothmer, Volker; Thernisien, Arnaud
2018shin.confE..40N    Altcode:
  The Wide-Field Imager for Parker Solar Probe (WISPR) will observe the
  Thomson scattered emission of the corona/inner heliosphere, covering
  a range of elongation angles from 13.5 to 108 deg, at high temporal
  (0.05-60 min) and spatial resolution (plate scale of 1.2-1.7 arcmin
  per pixel). Such images will be taken from unprecedented points of
  observation thanks to the highly-eccentric orbits of Parker Solar Probe
  (PSP), which will reach the minimum perihelion distance below 10 solar
  radii from the Sun's centre.

---------------------------------------------------------
Title: Preparing for Parker Solar Probe: Synthetic White-light
    Imagery and Analysis for the Wide-field Imager (WISPR)
Authors: Liewer, Paulett; Nisticó, Giuseppe; Howard, Russell; Bothmer,
   Volker; Thernisien, Arnaud; Vourlidas, Angelos; Penteado, Paulo
2018cosp...42E2010L    Altcode:
  The Parker Solar Probe (PSP) trajectory, approaching within 10 solar
  radii, will allow the white light imager, WISPR, to view the inner
  corona with unprecedented spatial resolution. WISPR, with a field of
  view extending from 13.5° to 108° elongation angle from the Sun, will
  image the fine-scale coronal structure with arcminute resolution. The
  dependency of the Thomson scattering on the imaging geometry (distance
  and angle from the Sun) dictates that WISPR will be very sensitive to
  the emission from plasma close to the spacecraft, in contrast to the
  situation for imaging from 1 AU. Thus, WISPR will be the first 'local'
  imager providing a crucial link between the large-scale corona and
  PSP's in-situ measurements. To prepare for this unprecedented viewing
  of the structures in the inner corona, we are creating synthetic
  white light images and animations, viewed from the PSP trajectory,
  using the white-light ray-tracing package developed at NRL (available
  through SolarSoft). We will present results for small flux ropes moving
  outward through the corona as well as fly-throughs of finely structured
  coronal streamers. Using the synthetic images, analysis techniques
  similar to traditional white light "jmaps" are used to find the "track"
  of a flux rope's elongation versus time. The "track" is compared with
  predictions using simple geometric expressions to gain information on
  the 3D trajectory of the flux rope. Additional analysis techniques,
  such as re-projections of the images, will also be discussed.

---------------------------------------------------------
Title: CMEs in the Heliosphere: I. A Statistical Analysis of the
    Observational Properties of CMEs Detected in the Heliosphere from
    2007 to 2017 by STEREO/HI-1
Authors: Harrison, R. A.; Davies, J. A.; Barnes, D.; Byrne, J. P.;
   Perry, C. H.; Bothmer, V.; Eastwood, J. P.; Gallagher, P. T.; Kilpua,
   E. K. J.; Möstl, C.; Rodriguez, L.; Rouillard, A. P.; Odstrčil, D.
2018SoPh..293...77H    Altcode: 2018arXiv180402320H
  We present a statistical analysis of coronal mass ejections (CMEs)
  imaged by the Heliospheric Imager (HI) instruments on board NASA's
  twin-spacecraft STEREO mission between April 2007 and August 2017 for
  STEREO-A and between April 2007 and September 2014 for STEREO-B. The
  analysis exploits a catalogue that was generated within the FP7
  HELCATS project. Here, we focus on the observational characteristics
  of CMEs imaged in the heliosphere by the inner (HI-1) cameras, while
  following papers will present analyses of CME propagation through
  the entire HI fields of view. More specifically, in this paper we
  present distributions of the basic observational parameters - namely
  occurrence frequency, central position angle (PA) and PA span - derived
  from nearly 2000 detections of CMEs in the heliosphere by HI-1 on
  STEREO-A or STEREO-B from the minimum between Solar Cycles 23 and 24
  to the maximum of Cycle 24; STEREO-A analysis includes a further 158
  CME detections from the descending phase of Cycle 24, by which time
  communication with STEREO-B had been lost. We compare heliospheric CME
  characteristics with properties of CMEs observed at coronal altitudes,
  and with sunspot number. As expected, heliospheric CME rates correlate
  with sunspot number, and are not inconsistent with coronal rates
  once instrumental factors/differences in cataloguing philosophy are
  considered. As well as being more abundant, heliospheric CMEs, like
  their coronal counterparts, tend to be wider during solar maximum. Our
  results confirm previous coronagraph analyses suggesting that CME launch
  sites do not simply migrate to higher latitudes with increasing solar
  activity. At solar minimum, CMEs tend to be launched from equatorial
  latitudes, while at maximum, CMEs appear to be launched over a much
  wider latitude range; this has implications for understanding the
  CME/solar source association. Our analysis provides some supporting
  evidence for the systematic dragging of CMEs to lower latitude as they
  propagate outwards.

---------------------------------------------------------
Title: Coronal Magnetic Structure of Earthbound CMEs and In Situ
    Comparison
Authors: Palmerio, E.; Kilpua, E. K. J.; Möstl, C.; Bothmer, V.;
   James, A. W.; Green, L. M.; Isavnin, A.; Davies, J. A.; Harrison, R. A.
2018SpWea..16..442P    Altcode: 2018arXiv180304769P
  Predicting the magnetic field within an Earth-directed coronal
  mass ejection (CME) well before its arrival at Earth is one of the
  most important issues in space weather research. In this article,
  we compare the intrinsic flux rope type, that is, the CME orientation
  and handedness during eruption, with the in situ flux rope type for 20
  CME events that have been uniquely linked from Sun to Earth through
  heliospheric imaging. Our study shows that the intrinsic flux rope
  type can be estimated for CMEs originating from different source
  regions using a combination of indirect proxies. We find that only
  20% of the events studied match strictly between the intrinsic and in
  situ flux rope types. The percentage rises to 55% when intermediate
  cases (where the orientation at the Sun and/or in situ is close to
  45°) are considered as a match. We also determine the change in the
  flux rope tilt angle between the Sun and Earth. For the majority of
  the cases, the rotation is several tens of degrees, while 35% of the
  events change by more than 90°. While occasionally the intrinsic flux
  rope type is a good proxy for the magnetic structure impacting Earth,
  our study highlights the importance of capturing the CME evolution
  for space weather forecasting purposes. Moreover, we emphasize that
  determination of the intrinsic flux rope type is a crucial input for
  CME forecasting models.

---------------------------------------------------------
Title: Simulating observations of the corona/inner heliosphere with
    the Wide-Field Imager for Parker Solar Probe by raytracing software
Authors: Nisticò, Giuseppe; Liewer, Paulett; Bothmer, Volker;
   Vourlidas, Angelos
2018EGUGA..2018677N    Altcode:
  The Wide-Field Imager for Parker Solar PRobe (WISPR) will provide us
  with white-light images of the corona/inner heliosphere offset from the
  Sun, covering a range of elongation angles from 13.5 to 108 deg, with
  a high temporal (0.05-60 min) and spatial resolution (plate scale of
  1.2-1.7 arcmin per pixel). Such images will be taken from unprecedented
  points of observation thanks to the highly-eccentric orbits of
  Parker Solar Probe (PSP), which will reach the minimum perihelion
  distance below 10 solar radii from the Sun's centre. Therefore,
  it is important to understand how WISPR images will look during the
  perihelion phases and when PSP will eventually fly throughout various
  coronal structures, e.g. streamers, expanding flux ropes, and jets. In
  this talk we will provide a collection of synthetic WISPR images for
  different coronal structures by using the raytracing tools available
  with the SolarSoftWare package. We will discuss the effects due to the
  varying radial distance and the high orbital speed ( 200 km/s) of PSP
  on the WISPR images, including the possibility of 3D reconstruction
  and the determination of the correct kinematics for expanding flux
  ropes and jets.

---------------------------------------------------------
Title: Connecting Coronal Mass Ejections to Their Solar Active Region
Sources: Combining Results from the HELCATS and FLARECAST Projects
Authors: Murray, Sophie A.; Guerra, Jordan A.; Zucca, Pietro; Park,
   Sung-Hong; Carley, Eoin P.; Gallagher, Peter T.; Vilmer, Nicole;
   Bothmer, Volker
2018SoPh..293...60M    Altcode: 2018arXiv180306529M
  Coronal mass ejections (CMEs) and other solar eruptive phenomena can be
  physically linked by combining data from a multitude of ground-based
  and space-based instruments alongside models; however, this can be
  challenging for automated operational systems. The EU Framework Package
  7 HELCATS project provides catalogues of CME observations and properties
  from the Heliospheric Imagers on board the two NASA/STEREO spacecraft
  in order to track the evolution of CMEs in the inner heliosphere. From
  the main HICAT catalogue of over 2,000 CME detections, an automated
  algorithm has been developed to connect the CMEs observed by STEREO
  to any corresponding solar flares and active-region (AR) sources
  on the solar surface. CME kinematic properties, such as speed and
  angular width, are compared with AR magnetic field properties, such as
  magnetic flux, area, and neutral line characteristics. The resulting
  LOWCAT catalogue is also compared to the extensive AR property
  database created by the EU Horizon 2020 FLARECAST project, which
  provides more complex magnetic field parameters derived from vector
  magnetograms. Initial statistical analysis has been undertaken on the
  new data to provide insight into the link between flare and CME events,
  and characteristics of eruptive ARs. Warning thresholds determined
  from analysis of the evolution of these parameters is shown to be a
  useful output for operational space weather purposes. Parameters of
  particular interest for further analysis include total unsigned flux,
  vertical current, and current helicity. The automated method developed
  to create the LOWCAT catalogue may also be useful for future efforts
  to develop operational CME forecasting.

---------------------------------------------------------
Title: Key results and services of HELCATS
Authors: Bothmer, Volker; Harrison, Richard; Davies, Jackie; Rouillard,
   Alexis
2018EGUGA..20.7441B    Altcode:
  The EU FP7 project HELCATS (HELIOSPHERIC CATALOGUING, ANALYSIS &amp;
  TECHNIQUES SERVICE) has provided new insights into solar wind structure
  through combining the comprehensive analysis of heliospheric imaging
  observations from the NASA STEREO spacecraft, in concert with associated
  remote-sensing and in-situ measurements, with a thorough assessment
  of appropriate techniques and models. The project recognised that the
  advent of wide-angle imaging of the inner heliosphere has revolutionised
  the study of transient and quasi-stationary structures in the solar
  wind, in particular Coronal Mass Ejections (CMEs) and Co-rotating
  Interaction Regions (CIRs). Prior to the development of wide-angle
  imaging of the inner heliosphere, signatures of such solar wind
  features could only be observed within a few solar radii of the Sun,
  and in the vicinity of a few near-Earth and interplanetary probes making
  in-situ measurements of the solar wind. Heliospheric imaging has, for
  the first time, filled that vast and crucial observational gap. This
  presentation summarises the key results and services established by
  the HELCATS project.

---------------------------------------------------------
Title: Solar-wind predictions for the Parker Solar Probe orbit
Authors: Bothmer, Volker; Venzmer, Malte
2018EGUGA..20.5245B    Altcode:
  The Parker Solar Probe (PSP) (formerly Solar Probe Plus) mission
  will be humanity's first in situ exploration of the solar corona
  with closest perihelia at 9.86 solar radii distance to the Sun. It
  will help answer hitherto unresolved questions on the heating of the
  solar corona and the source and acceleration of the solar wind and
  solar energetic particles. The scope of the study presented here is
  to model the solar-wind environment for PSP's unprecedented distances
  in its prime mission phase during the years 2018-2025. The study is
  performed within the Coronagraphic German And US SolarProbePlus Survey
  (CGAUSS) which is the German contribution to the PSP mission as part
  of the Wide-field Imager for Solar PRobe (WISPR). Here we present an
  empirical solar-wind model for the inner heliosphere which has been
  derived from OMNI and Helios data.

---------------------------------------------------------
Title: Solar-wind predictions for the Parker Solar Probe
    orbit. Near-Sun extrapolations derived from an empirical solar-wind
    model based on Helios and OMNI observations
Authors: Venzmer, M. S.; Bothmer, V.
2018A&A...611A..36V    Altcode: 2017arXiv171107534V
  Context. The Parker Solar Probe (PSP; formerly Solar Probe Plus) mission
  will be humanitys first in situ exploration of the solar corona with
  closest perihelia at 9.86 solar radii (R<SUB>⊙</SUB>) distance to
  the Sun. It will help answer hitherto unresolved questions on the
  heating of the solar corona and the source and acceleration of the
  solar wind and solar energetic particles. The scope of this study is
  to model the solar-wind environment for PSPs unprecedented distances
  in its prime mission phase during the years 2018 to 2025. The study
  is performed within the Coronagraphic German And US SolarProbePlus
  Survey (CGAUSS) which is the German contribution to the PSP mission
  as part of the Wide-field Imager for Solar PRobe. Aim. We present an
  empirical solar-wind model for the inner heliosphere which is derived
  from OMNI and Helios data. The German-US space probes Helios 1 and
  Helios 2 flew in the 1970s and observed solar wind in the ecliptic
  within heliocentric distances of 0.29 au to 0.98 au. The OMNI database
  consists of multi-spacecraft intercalibrated in situ data obtained near
  1 au over more than five solar cycles. The international sunspot number
  (SSN) and its predictions are used to derive dependencies of the major
  solar-wind parameters on solar activity and to forecast their properties
  for the PSP mission. <BR /> Methods: The frequency distributions for the
  solar-wind key parameters, magnetic field strength, proton velocity,
  density, and temperature, are represented by lognormal functions. In
  addition, we consider the velocity distributions bi-componental shape,
  consisting of a slower and a faster part. Functional relations to
  solar activity are compiled with use of the OMNI data by correlating
  and fitting the frequency distributions with the SSN. Further, based
  on the combined data set from both Helios probes, the parameters
  frequency distributions are fitted with respect to solar distance
  to obtain power law dependencies. Thus an empirical solar-wind model
  for the inner heliosphere confined to the ecliptic region is derived,
  accounting for solar activity and for solar distance through adequate
  shifts of the lognormal distributions. Finally, the inclusion of SSN
  predictions and the extrapolation down to PSPs perihelion region enables
  us to estimate the solar-wind environment for PSPs planned trajectory
  during its mission duration. <BR /> Results: The CGAUSS empirical
  solar-wind model for PSP yields dependencies on solar activity and solar
  distance for the solar-wind parameters' frequency distributions. The
  estimated solar-wind median values for PSPs first perihelion in 2018
  at a solar distance of 0.16 au are 87 nT, 340 km s<SUP>-1</SUP>, 214
  cm<SUP>-3</SUP>, and 503 000 K. The estimates for PSPs first closest
  perihelion, occurring in 2024 at 0.046 au (9.86 R<SUB>⊙</SUB>),
  are 943 nT, 290 km s<SUP>-1</SUP>, 2951 cm<SUP>-3</SUP>, and 1 930 000
  K. Since the modeled velocity and temperature values below approximately
  20 R<SUB>⊙</SUB>appear overestimated in comparison with existing
  observations, this suggests that PSP will directly measure solar-wind
  acceleration and heating processes below 20 R<SUB>⊙</SUB> as planned.

---------------------------------------------------------
Title: The Solar Orbiter Heliospheric Imager (SoloHI) for the Solar
    Orbiter Mission
Authors: Howard, R.; Colaninno, R. C.; Plunkett, S. P.; Thernisien,
   A. F.; Wang, D.; Rich, N.; Korendyke, C.; Socker, D. G.; Linton, M.;
   McMullin, D. R.; Vourlidas, A.; Liewer, P. C.; De Jong, E.; Velli,
   M.; Mikic, Z.; Bothmer, V.; Philippe, L.; Carter, M. T.
2017AGUFMSH23D2681H    Altcode:
  The SoloHI instrument has completed its development effort and has been
  integrated onto the Solar Orbiter (SolO) spacecraft. The SolO mission,
  scheduled for launch in February 2019, will undergo gravity assist
  maneuvers around Venus to change both the perihelion distance as well
  as the plane of the orbit to ultimately achieve a minimum perihelion
  of 0.28 AU and an orbital inclination of about 35° relative to the
  ecliptic plane. The remote sensing instruments will operate for three
  10-day periods out of the nominal 6-month orbit. SoloHI will observe
  sunlight scattered by free electrons in the corona/solar wind from 5°
  to 45° elongation in visible wavelengths and will provide a coupling
  between remote sensing and in situ observations. It is very similar
  to the HI-1 instrument on STEREO/SECCHI except that the FOV is twice
  the size at 40o. We present our efforts to prepare for the mission
  including our observing plans, quick-look plans and some results of
  the calibration activities. We gratefully acknowledge the support of
  the NASA Solar Orbiter Collaboration project.

---------------------------------------------------------
Title: The Wide-Field Imager for the Parker Solar Probe Mission
    (WISPR)
Authors: Plunkett, S. P.; Howard, R.; Chua, D. H.; Crump, N. A.;
   Dennison, H.; Korendyke, C.; Linton, M.; Rich, N.; Socker, D. G.;
   Thernisien, A. F.; Wang, D.; Vourlidas, A.; Baugh, R.; Van Duyne,
   J. P.; Liewer, P. C.; De Jong, E.; Boies, M. T.; Mikic, Z.; Bothmer,
   V.; Rochus, P.; Halain, J. P.
2017AGUFMSH23D2693P    Altcode:
  The Parker Solar Probe (PSP) mission will be humanity's first visit
  to the atmosphere of our nearest star, the Sun, when it is launched
  in July 2018. PSP will complete 24 orbits between the Sun and Venus
  with diminishing perihelia reaching as close as 7 million km (9.86
  solar radii) from Sun center. In addition to a suite of in-situ probes
  for the magnetic field, plasma, and energetic particles, the payload
  includes the Wide Field Imager for Solar Probe (WISPR) that will
  record unprecedented visible light images of the solar corona and the
  inner heliosphere. WISPR is the smallest heliospheric imager to date,
  and comprises two nested wide-field telescopes with large-format (2K
  x 2K) APS CMOS detectors to optimize the performance over a combined
  95º radial by 58º transverse field of view and to minimize the risk
  of dust damage, which may be considerable close to the Sun. WISPR will
  discover - in this never-before explored region of the heliosphere - the
  fundamental nature of coronal structures and the source regions of the
  solar wind as the PSP flies through them, and will determine whether a
  dust-free zone exists near the Sun. WISPR has completed its development
  effort and has been integrated onto the PSP spacecraft. In this paper,
  we will present our efforts to prepare for the mission including our
  observing plans and some results of the calibration activities.

---------------------------------------------------------
Title: The Heliospheric Cataloguing, Analysis and Techniques Service
    (HELCATS) project
Authors: Barnes, D.; Harrison, R. A.; Davies, J. A.; Perry, C. H.;
   Moestl, C.; Rouillard, A.; Bothmer, V.; Rodriguez, L.; Eastwood,
   J. P.; Kilpua, E.; Gallagher, P.; Odstrcil, D.
2017AGUFMSH31A2713B    Altcode:
  Understanding solar wind evolution is fundamental to advancing our
  knowledge of energy and mass transport in the solar system, whilst
  also being crucial to space weather and its prediction. The advent of
  truly wide-angle heliospheric imaging has revolutionised the study of
  solar wind evolution, by enabling direct and continuous observation
  of both transient and background components of the solar wind as they
  propagate from the Sun to 1 AU and beyond. The recently completed,
  EU-funded FP7 Heliospheric Cataloguing, Analysis and Techniques
  Service (HELCATS) project (1st May 2014 - 30th April 2017) combined
  European expertise in heliospheric imaging, built up over the last
  decade in particular through leadership of the Heliospheric Imager
  (HI) instruments aboard NASA's STEREO mission, with expertise in
  solar and coronal imaging as well as the interpretation of in-situ
  and radio diagnostic measurements of solar wind phenomena. HELCATS
  involved: (1) the cataloguing of transient (coronal mass ejections)
  and background (stream/corotating interaction regions) solar wind
  structures observed by the STEREO/HI instruments, including estimates of
  their kinematic properties based on a variety of modelling techniques;
  (2) the verification of these kinematic properties through comparison
  with solar source observations and in-situ measurements at multiple
  points throughout the heliosphere; (3) the assessment of the potential
  for initialising numerical models based on the derived kinematic
  properties of transient and background solar wind components; and (4)
  the assessment of the complementarity of radio observations (Type II
  radio bursts and interplanetary scintillation) in the detection and
  analysis of heliospheric structure in combination with heliospheric
  imaging observations. In this presentation, we provide an overview
  of the HELCATS project emphasising, in particular, the principal
  achievements and legacy of this unprecedented project.

---------------------------------------------------------
Title: Comparison of CME and ICME Structures Derived from
    Remote-Sensing and In Situ Observations
Authors: Bothmer, V.; Mrotzek, N.
2017SoPh..292..157B    Altcode:
  We present results from the comparison of the near-Sun and in situ
  analysis of two Earth-directed coronal mass ejections (CMEs) with
  different 3D orientations and solar source region characteristics. The
  CME on 14 July 2000, the so-called Bastille Day storm, a well-studied
  event, was observed from a single-point perspective by the Large Angle
  and Spectrometric Coronagraph (LASCO) onboard the Solar and Heliospheric
  Observatory (SOHO). It caused a major geomagnetic storm with a peak Kp
  of 9. The CME originated from a magnetic bipolar photospheric source
  region with the polarity inversion line being oriented rather parallel
  to the heliographic equator. In contrast, the CME on 29 September
  2013, which caused a geomagnetic storm with a peak Kp intensity of 8-,
  originated from a magnetic quadrupolar photospheric source region with
  the polarity inversion line between the two bipoles almost vertically
  oriented with respect to the heliographic equator. The results of a
  graduated cylindrical shell (GCS) analysis of the CMEs near the Sun
  are compared with the minimum variance analysis (MVA) of the magnetic
  field structure of the interplanetary CME (ICME) measured in situ near
  Earth's orbit. The results are in good agreement for the September
  2013 CME and ICME, whereas the July 2000 ICME appears substantially
  inclined near Earth's orbit. The discrepancy can likely be explained
  taking into account kinks in the CME's near-Sun structure of the CME
  that expands into the interplanetary medium.

---------------------------------------------------------
Title: CME Dynamics Using STEREO and LASCO Observations: The Relative
    Importance of Lorentz Forces and Solar Wind Drag
Authors: Sachdeva, Nishtha; Subramanian, Prasad; Vourlidas, Angelos;
   Bothmer, Volker
2017SoPh..292..118S    Altcode: 2017arXiv170504871S
  We seek to quantify the relative contributions of Lorentz forces and
  aerodynamic drag on the propagation of solar coronal mass ejections
  (CMEs). We use Graduated Cylindrical Shell (GCS) model fits to a
  representative set of 38 CMEs observed with the Solar and Heliospheric
  Observatory (SOHO) and the Solar and Terrestrial Relations Observatory
  (STEREO) spacecraft. We find that the Lorentz forces generally peak
  between 1.65 and 2.45 R<SUB>⊙</SUB> for all CMEs. For fast CMEs,
  Lorentz forces become negligible in comparison to aerodynamic drag as
  early as 3.5 - 4 R<SUB>⊙</SUB>. For slow CMEs, however, they become
  negligible only by 12 - 50 R<SUB>⊙</SUB>. For these slow events,
  our results suggest that some of the magnetic flux might be expended in
  CME expansion or heating. In other words, not all of it contributes to
  the propagation. Our results are expected to be important in building
  a physical model for understanding the Sun-Earth dynamics of CMEs.

---------------------------------------------------------
Title: Modeling observations of solar coronal mass ejections with
    heliospheric imagers verified with the Heliophysics System Observatory
Authors: Möstl, C.; Isavnin, A.; Boakes, P. D.; Kilpua, E. K. J.;
   Davies, J. A.; Harrison, R. A.; Barnes, D.; Krupar, V.; Eastwood,
   J. P.; Good, S. W.; Forsyth, R. J.; Bothmer, V.; Reiss, M. A.;
   Amerstorfer, T.; Winslow, R. M.; Anderson, B. J.; Philpott, L. C.;
   Rodriguez, L.; Rouillard, A. P.; Gallagher, P.; Nieves-Chinchilla,
   T.; Zhang, T. L.
2017SpWea..15..955M    Altcode: 2017arXiv170300705M
  We present an advance toward accurately predicting the arrivals of
  coronal mass ejections (CMEs) at the terrestrial planets, including
  Earth. For the first time, we are able to assess a CME prediction model
  using data over two thirds of a solar cycle of observations with the
  Heliophysics System Observatory. We validate modeling results of 1337
  CMEs observed with the Solar Terrestrial Relations Observatory (STEREO)
  heliospheric imagers (HI) (science data) from 8 years of observations
  by five in situ observing spacecraft. We use the self-similar expansion
  model for CME fronts assuming 60° longitudinal width, constant speed,
  and constant propagation direction. With these assumptions we find that
  23%-35% of all CMEs that were predicted to hit a certain spacecraft
  lead to clear in situ signatures, so that for one correct prediction,
  two to three false alarms would have been issued. In addition, we find
  that the prediction accuracy does not degrade with the HI longitudinal
  separation from Earth. Predicted arrival times are on average within 2.6
  ± 16.6 h difference of the in situ arrival time, similar to analytical
  and numerical modeling, and a true skill statistic of 0.21. We also
  discuss various factors that may improve the accuracy of space weather
  forecasting using wide-angle heliospheric imager observations. These
  results form a first-order approximated baseline of the prediction
  accuracy that is possible with HI and other methods used for data by
  an operational space weather mission at the Sun-Earth L5 point.

---------------------------------------------------------
Title: Radio triangulation of solar radio emissions associated with
    the 2012 July 23 CME
Authors: Krupar, Vratislav; Kruparova, Oksana; Santolik, Ondrej;
   Bothmer, Volker; Mrotzek, Niclas; Eastwood, Jonathan P.
2017EGUGA..19.8836K    Altcode:
  Coronal mass ejections (CMEs) are large-scale eruptions of magnetized
  plasma that may cause severe geomagnetic storms if Earth directed. The
  backside CME from 2012 July 23 belongs among historical extreme solar
  events due to associated solar energetic particle fluxes and the
  CME-driven shock speed above 2000 kms-1. Here, we focus on analysis of
  associated interplanetary (IP) radio emissions. The frequency drift
  of the IP type II burst provides us with a reasonable speed of the
  CME-driven shock. We have successfully applied a radio direction-finding
  technique to IP type II and type III bursts observed by the two
  identical radio receivers aboard the two STEREO spacecraft. The radio
  triangulation technique allows us to localize radio sources in the
  IP medium. The obtained locations of the type II and type III bursts
  are in a very good agreement with the CME direction. We demonstrate
  the complementarity between radio triangulation and 3D reconstruction
  techniques for space weather applications.

---------------------------------------------------------
Title: CME properties and solar source region characteristics -
    HELCATS results
Authors: Bothmer, Volker; Mrotzek, Niclas; Murray, Sophie; Gallagher,
   Peter; Barnes, David; Davies, Jackie; Harrison, Richard
2017EGUGA..19.5107B    Altcode:
  One objective of the EU FP7 project HELCATS is to derive and
  catalogue the characteristics of CMEs observed with the STEREO/COR2
  &amp; HI imagers based on geometrical and forward modelling. Here
  we present the results of the analysis of a subset of the 122 CME
  events that have been dynamically modelled with the GCS-method in
  the COR2 field of view and which are compiled in the KINCAT database
  at http://www.affects-fp7.eu/helcats-database/database.php. The
  CME properties, such as speeds, masses, angular widths, as derived
  from modelling, are compared with magnetic field properties of the
  corresponding solar source active region, such as magnetic flux,
  area, and polarity line characteristics. The results show which solar
  parameters define the structure of CMEs at distances around 12 solar
  radii and how they can be used for space weather forecast services.

---------------------------------------------------------
Title: Using helispheric imager observations in predicting the impact
    of coronal mass ejections (CMEs) at planets
Authors: Kilpua, Emilia; Möstl, Christian; Bothmer, Volker; Isavnin,
   Alexey; Harrison, Richard; Davies, Jackie; Palmerio, Erika; Boakes,
   Peter; Mrotzek, Niclas
2017EGUGA..19.9051K    Altcode:
  Connecting coronal mass ejections (CMEs) in remote-sensing and in-situ
  observations can be surprisingly difficult. Coronagraphs can detect
  CMEs only about 10% of their journey from Sun to 1 AU. One viable
  way to track CMEs through the inner heliosphere is using heliospheric
  imaging. HELCATS (Heliospheric Cataloguing, Analysis And Techniques
  Service) LINKCAT catalogue is the first concerted effort to establish
  such linkage automatically by the systematic use of STEREO Heliospheric
  Imager (HI) observations and related modelling. This presentation gives
  and overview of how the LINKCAT catalogue is generated and evaluates
  the potential of HI-based imagining in connecting CMEs near the Sun
  and in-situ. We will also discuss the possible problems in our approach
  and the key future improvements.

---------------------------------------------------------
Title: Impacts of Space Weather Effects on the Ionospheric Vertical
    Total Electron Content
Authors: Hinrichs, Johannes; Bothmer, Volker; Mrotzek, Niclas;
   Venzmer, Malte; Erdogan, Eren; Dettmering, Denise; Goss, Andreas;
   Schmidt, Michael; Seitz, Florian; Börger, Klaus; Brandert, Sylvia;
   Görres, Barbara; Kersten, Wilhelm F.
2017EGUGA..19.5229H    Altcode:
  In the space weather project OPTIMAP (OPerational Tool for Ionosphere
  Mapping And Prediction) we investigate and analyse the solar influences
  on the Earth's ionosphere, to help establish an improved forecast
  for global VTEC maps, taking into account space weather effects. The
  resulting service will be implemented at the German Space Situational
  Awareness Centre. Here we present results from the analysis of a time
  series of global ionospheric VTEC-maps provided through computations at
  DGFI-TUM and the IGS analysis center CODE, in conjunction with EUV and
  X-ray radiation and solar wind parameters measured by space missions
  in operation (GOES, SDO, ACE, SOHO and STEREO). The individual impacts
  of radiation and different solar wind structures, such as coronal mass
  ejections, high speed streams and CIRs, are described. This includes
  an analysis of the strongest geomagnetic storms measured since the
  launch of ACE.

---------------------------------------------------------
Title: A Catalogue of Coronal Mass Ejections Observed by the STEREO
Heliospheric Imagers: Results from HELCATS
Authors: Barnes, David; Davies, Jackie; Harrison, Richard; Perry,
   Chris; Möstl, Christian; Rouillard, Alexis; Bothmer, Volker;
   Rodriguez, Luciano; Eastwood, Jonathan; Kilpua, Emilia; Gallagher,
   Peter
2017EGUGA..19.8160B    Altcode:
  The wide fields of view provided by the STEREO Heliospheric Imagers
  (HIs) allow far greater coverage of Coronal Mass Ejections (CMEs) than
  are typically available from coronagraph observations. As part of the EU
  FP7 HELCATS (Heliospheric Cataloguing, Analysis and Techniques Service)
  project we present a comprehensive catalogue of CMEs that are observed
  in HI data, throughout the lifetime of the instruments. This spans
  the period from April 2007 to September 2014 for both STEREO-A and -B,
  with additional STEREO-A observations continuing from October 2015 to
  present, covering the majority of solar cycle 24. A subset of these
  CMEs are tracked through the HI fields of view, to which we apply both
  single-spacecraft and stereoscopic models to determine CME kinematic
  properties such as propagation directions, speeds and accelerations. The
  statistical properties of these results are discussed and they are
  compared with coronagraph observations during the same period.

---------------------------------------------------------
Title: A Multi-Model Approach to the Analysis of the Kinematics of
    CMEs Based on Multi-point Space Observations
Authors: Mrotzek, Niclas; Bothmer, Volker; Davies, Jackie; Harrison,
   Richard
2017EGUGA..19.3532M    Altcode:
  The interaction between Coronal Mass Ejections (CMEs) and the
  ambient solar wind is a crucial factor affecting their interplanetary
  evolution. It is believed that acceleration due to the Lorenz force
  dominates CME evolution near the Sun and that the aerodynamic drag force
  becomes dominant further away. In this study, we present results of a
  distance-dependent aerodynamic drag force model taking into account
  solar wind measurements from the Helios spacecraft over the spatial
  range 0.3 to 0.9 AU. We undertake GCS modelling of the investigated CMEs
  based on observations from the coronagraphs on SOHO and STEREO as well
  as observations from the STEREO heliospheric imagers (HIs). Application
  of the CGS modelling to the HI data enables the height-time profiles of
  the CMEs to be extended further from the Sun. To derive transit times
  to 1 AU, the height-time profiles are then fitted using a kinematic
  drag model and compared with in-situ solar wind measurements. The
  study is carried out in the framework of the EU FP7 project HELCATS
  (Heliospheric Cataloguing, Analysis and Techniques Service).

---------------------------------------------------------
Title: Modeling of coronal mass ejections with the STEREO heliospheric
    imagers verified with in situ observations by the Heliophysics
    System Observatory
Authors: Möstl, Christian; Isavnin, Alexey; Kilpua, Emilia; Bothmer,
   Volker; Mrotzek, Nicolas; Boakes, Peter; Rodriguez, Luciano; Krupar,
   Vratislav; Eastwood, Jonathan; Davies, Jackie; Harrison, Richard;
   Barnes, David; Winslow, Reka; Helcats Team
2017EGUGA..19.4536M    Altcode:
  We present the first study to verify modeling of CMEs as observed by
  the heliospheric imagers on the two STEREO spacecraft with a large
  scale dataset of in situ plasma and magnetic field observations from
  the Heliophysics System Observatory, including MESSENGER, VEX, Wind,
  and the in situ measurements on the two STEREO spacecraft. To this end,
  we have established a new interplanetary CME catalog (ICMECAT) for these
  spacecraft by gathering and updating individual ICME lists. In addition,
  we have re-calculated the in situ parameters in a consistent way,
  resulting in 668 events observed between 2007-2015. We then calculated
  the efficacy of the STEREO/HI instruments for predicting (in hindsight)
  with the SSEF30 model the arrival time and speed of CMEs as well as
  hit/miss ratios. We also show how ICMECAT gives decent statistics
  concerning CME impacts on all of the terrestrial planets, including
  Mars. The results show some major implications for future heliospheric
  imagers which may be used for space weather forecasting. Our effort
  should also serve as a baseline for the upcoming new era in heliospheric
  science with Solar Orbiter, Solar Probe Plus, BepiColombo returning
  partly comparable observations in the next decade. The presented work
  has received funding from the European Union Seventh Framework Programme
  (FP7/ 2007-2013) under grant agreement No. 606692 [HELCATS].

---------------------------------------------------------
Title: Regional Densification of a Global VTEC Model Based on
    B-Spline Representations
Authors: Erdogan, Eren; Schmidt, Michael; Dettmering, Denise; Goss,
   Andreas; Seitz, Florian; Börger, Klaus; Brandert, Sylvia; Görres,
   Barbara; Kersten, Wilhelm F.; Bothmer, Volker; Hinrichs, Johannes;
   Mrotzek, Niclas
2017EGUGA..19.8860E    Altcode:
  The project OPTIMAP is a joint initiative of the Bundeswehr
  GeoInformation Centre (BGIC), the German Space Situational Awareness
  Centre (GSSAC), the German Geodetic Research Institute of the Technical
  University Munich (DGFI-TUM) and the Institute for Astrophysics at
  the University of Göttingen (IAG). The main goal of the project
  is the development of an operational tool for ionospheric mapping
  and prediction (OPTIMAP). Two key features of the project are the
  combination of different satellite observation techniques (GNSS,
  satellite altimetry, radio occultations and DORIS) and the regional
  densification as a remedy against problems encountered with the
  inhomogeneous data distribution. Since the data from space-geoscientific
  mission which can be used for modeling ionospheric parameters, such
  as the Vertical Total Electron Content (VTEC) or the electron density,
  are distributed rather unevenly over the globe at different altitudes,
  appropriate modeling approaches have to be developed to handle this
  inhomogeneity. Our approach is based on a two-level strategy. To be
  more specific, in the first level we compute a global VTEC model with
  a moderate regional and spectral resolution which will be complemented
  in the second level by a regional model in a densification area. The
  latter is a region characterized by a dense data distribution to obtain
  a high spatial and spectral resolution VTEC product. Additionally,
  the global representation means a background model for the regional
  one to avoid edge effects at the boundaries of the densification
  area. The presented approach based on a global and a regional model
  part, i.e. the consideration of a regional densification is called
  the Two-Level VTEC Model (TLVM). The global VTEC model part is based
  on a series expansion in terms of polynomial B-Splines in latitude
  direction and trigonometric B-Splines in longitude direction. The
  additional regional model part is set up by a series expansion in terms
  of polynomial B-splines for both directions. The spectral resolution of
  both model parts is defined by the number of B-spline basis functions
  introduced for longitude and latitude directions related to appropriate
  coordinate systems. Furthermore, the TLVM has to be developed under the
  postulation that the global model part will be computed continuously
  in near real-time (NRT) and routinely predicted into the future by an
  algorithm based on deterministic and statistical forecast models. Thus,
  the additional regional densification model part, which will be computed
  also in NRT, but possibly only for a specified time duration, must be
  estimated independently from the global one. For that purpose a data
  separation procedure has to be developed in order to estimate the
  unknown series coefficients of both model parts independently. This
  procedure must also consider additional technique-dependent unknowns
  such as the Differential Code Biases (DCBs) within GNSS and intersystem
  biases. In this contribution we will present the concept to set up the
  TLVM including the data combination and the Kalman filtering procedure;
  first numerical results will be presented.

---------------------------------------------------------
Title: Overview of the HELCATS project
Authors: Harrison, Richard; Davies, Jackie; Perry, Chris; Moestl,
   Christian; Rouillard, Alexis; Bothmer, Volker; Rodriguez, Luciano;
   Eastwood, Jonathan; Kilpua, Emilia; Gallagher, Peter; Odstrcil, Dusan
2017EGUGA..19.5296H    Altcode:
  Understanding solar wind evolution is fundamental to advancing our
  knowledge of energy and mass transport in the solar system, whilst
  also being crucial to space weather and its prediction. The advent of
  truly wide-angle heliospheric imaging has revolutionised the study of
  solar wind evolution, by enabling direct and continuous observation
  of both transient and background components of the solar wind as
  they propagate from the Sun to 1 AU and beyond. The EU-funded FP7
  Heliospheric Cataloguing, Analysis and Techniques Service (HELCATS)
  project combines European expertise in heliospheric imaging, built up
  over the last decade in particular through lead involvement in NASA's
  STEREO mission, with expertise in solar and coronal imaging as well
  as the interpretation of in-situ and radio diagnostic measurements of
  solar wind phenomena. HELCATS involves: (1) cataloguing of transient
  (coronal mass ejections) and background (stream/corotating interaction
  regions) solar wind structures observed by the STEREO/Heliospheric
  Imagers, including estimates of their kinematic properties based on
  a variety of modelling techniques; (2) verifying these kinematic
  properties through comparison with solar source observations and
  in-situ measurements at multiple points throughout the heliosphere;
  (3) assessing the potential for initialising numerical models based
  on the derived kinematic properties of transient and background
  solar wind components; (4) assessing the complementarity of radio
  observations (Type II radio bursts and interplanetary scintillation)
  in the detection and analysis of heliospheric structure in combination
  with heliospheric imaging observations. We provide an overview of the
  achievements of the HELCATS project, as it reaches its conclusion, and
  present selected results that seek to illustrate the value and legacy of
  this unprecedented, coordinated study of structures in the heliosphere.

---------------------------------------------------------
Title: Magnetic structure of Earth-directed events in the HELCATS
    LINKCAT catalog during 2011-2013
Authors: Palmerio, Erika; Kilpua, Emilia; Bothmer, Volker; Isavnin,
   Alexey; Möstl, Christian; Green, Lucie; James, Alexander; Davies,
   Jackie; Harrison, Richard
2017EGUGA..19.3874P    Altcode:
  Coronal mass ejections (CMEs) are the main drivers of intense magnetic
  storms and various subsequent space weather phenomena at Earth. The
  parameter that defines the ability of a CME to drive geomagnetic
  storms is the north-south magnetic field component. One of the most
  significant problems in current long-term space weather forecasts is
  that there is no practical method to measure the magnetic structure
  of CMEs routinely in the outer corona. The magnetic structure of CME
  flux ropes can however be inferred based on the properties of the
  CME's source region characteristics, such as filament details, coronal
  EUV arcades, X-ray sigmoids, taking into account nearby coronal and
  photospheric features. The linked catalogue (LINKCAT) of solar CMEs
  during the STEREO era is part of the HELCATS project. It aims at
  connecting CME observations at the Sun and in interplanetary space,
  using heliospheric imager observations from the HI1 cameras onboard the
  two STEREO spacecraft to connect the different datasets. The HELCATS
  LINKCAT catalogue contains 45 Earth-directed events in the period
  2011-2013 (https://www.helcats-fp7.eu/catalogues/wp4_cat.html). Here we
  present a statistical study based on the LINKCAT Earth-directed events
  during 2011-2013 in which we determine the magnetic properties of
  the erupting CMEs, i.e. their magnetic helicity sign, flux rope tilt,
  and flux rope axial field direction, by using a synthesis of indirect
  proxies based on multi-wavelength remote sensing observations from the
  STEREO, SOHO, Hinode, and SDO satellites. These parameters define the
  “intrinsic” flux rope configuration at the time of the eruption which
  is compared with the magnetic structures detected in situ near Earth.

---------------------------------------------------------
Title: The Wide-Field Imager for Solar Probe Plus (WISPR)
Authors: Vourlidas, Angelos; Howard, Russell A.; Plunkett, Simon P.;
   Korendyke, Clarence M.; Thernisien, Arnaud F. R.; Wang, Dennis; Rich,
   Nathan; Carter, Michael T.; Chua, Damien H.; Socker, Dennis G.; Linton,
   Mark G.; Morrill, Jeff S.; Lynch, Sean; Thurn, Adam; Van Duyne, Peter;
   Hagood, Robert; Clifford, Greg; Grey, Phares J.; Velli, Marco; Liewer,
   Paulett C.; Hall, Jeffrey R.; DeJong, Eric M.; Mikic, Zoran; Rochus,
   Pierre; Mazy, Emanuel; Bothmer, Volker; Rodmann, Jens
2016SSRv..204...83V    Altcode: 2015SSRv..tmp....8V; 2015SSRv..tmp...66B
  The Wide-field Imager for Solar PRobe Plus (WISPR) is the sole imager
  aboard the Solar Probe Plus (SPP) mission scheduled for launch in
  2018. SPP will be a unique mission designed to orbit as close as
  7 million km (9.86 solar radii) from Sun center. WISPR employs a
  95<SUP>∘</SUP> radial by 58<SUP>∘</SUP> transverse field of view
  to image the fine-scale structure of the solar corona, derive the 3D
  structure of the large-scale corona, and determine whether a dust-free
  zone exists near the Sun. WISPR is the smallest heliospheric imager to
  date yet it comprises two nested wide-field telescopes with large-format
  (2 K × 2 K) APS CMOS detectors to optimize the performance for their
  respective fields of view and to minimize the risk of dust damage,
  which may be considerable close to the Sun. The WISPR electronics are
  very flexible allowing the collection of individual images at cadences
  up to 1 second at perihelion or the summing of multiple images to
  increase the signal-to-noise when the spacecraft is further from the
  Sun. The dependency of the Thomson scattering emission of the corona
  on the imaging geometry dictates that WISPR will be very sensitive
  to the emission from plasma close to the spacecraft in contrast to
  the situation for imaging from Earth orbit. WISPR will be the first
  `local' imager providing a crucial link between the large-scale corona
  and the in-situ measurements.

---------------------------------------------------------
Title: A Catalogue of Geometrically-Modelled Coronal Mass Ejections
    Observed by the STEREO Heliospheric Imagers
Authors: Barnes, D.; Davies, J. A.; Harrison, R. A.; Perry, C. H.;
   Moestl, C.; Rouillard, A.; Bothmer, V.; Rodriguez, L.; Eastwood,
   J. P.; Kilpua, E.; Gallagher, P.
2016AGUFMSH31B2588B    Altcode:
  We present a catalogue of Coronal Mass Ejections (CMEs) observed by the
  Heliospheric Imagers (HIs) onboard the two NASA STEREO spacecraft. This
  catalogue contains all CMEs observed during the operational phase of the
  STEREO mission, April 2007 to September 2014, for both spacecraft and
  resumes from November 2015 for STEREO-A. These CMEs are tracked using
  time-elongation plots through the HI-1 and HI-2 fields of view and to
  them we apply geometric models to determine their kinematic properties,
  such as speed, propagation direction and launch time. A subset of
  these CMEs, which are observed simultaneously by both spacecraft,
  are identified and to which stereoscopic modelling techniques are
  applied. The statistical properties of these catalogues are discussed
  as are their results compared to existing CME catalogues covering the
  same periods. This work is carried out as part of the EU FP7 HELCATS
  (Heliospheric Cataloguing, Analysis and Techniques Service) project.

---------------------------------------------------------
Title: A small mission concept to the Sun-Earth Lagrangian L5 point
    for innovative solar, heliospheric and space weather science
Authors: Lavraud, B.; Liu, Y.; Segura, K.; He, J.; Qin, G.; Temmer,
   M.; Vial, J. -C.; Xiong, M.; Davies, J. A.; Rouillard, A. P.; Pinto,
   R.; Auchère, F.; Harrison, R. A.; Eyles, C.; Gan, W.; Lamy, P.;
   Xia, L.; Eastwood, J. P.; Kong, L.; Wang, J.; Wimmer-Schweingruber,
   R. F.; Zhang, S.; Zong, Q.; Soucek, J.; An, J.; Prech, L.; Zhang,
   A.; Rochus, P.; Bothmer, V.; Janvier, M.; Maksimovic, M.; Escoubet,
   C. P.; Kilpua, E. K. J.; Tappin, J.; Vainio, R.; Poedts, S.; Dunlop,
   M. W.; Savani, N.; Gopalswamy, N.; Bale, S. D.; Li, G.; Howard, T.;
   DeForest, C.; Webb, D.; Lugaz, N.; Fuselier, S. A.; Dalmasse, K.;
   Tallineau, J.; Vranken, D.; Fernández, J. G.
2016JASTP.146..171L    Altcode:
  We present a concept for a small mission to the Sun-Earth Lagrangian L5
  point for innovative solar, heliospheric and space weather science. The
  proposed INvestigation of Solar-Terrestrial Activity aNd Transients
  (INSTANT) mission is designed to identify how solar coronal magnetic
  fields drive eruptions, mass transport and particle acceleration that
  impact the Earth and the heliosphere. INSTANT is the first mission
  designed to (1) obtain measurements of coronal magnetic fields from
  space and (2) determine coronal mass ejection (CME) kinematics with
  unparalleled accuracy. Thanks to innovative instrumentation at a vantage
  point that provides the most suitable perspective view of the Sun-Earth
  system, INSTANT would uniquely track the whole chain of fundamental
  processes driving space weather at Earth. We present the science
  requirements, payload and mission profile that fulfill ambitious science
  objectives within small mission programmatic boundary conditions.

---------------------------------------------------------
Title: Long-Term Tracking of Corotating Density Structures Using
    Heliospheric Imaging
Authors: Plotnikov, I.; Rouillard, A. P.; Davies, J. A.; Bothmer,
   V.; Eastwood, J. P.; Gallagher, P.; Harrison, R. A.; Kilpua, E.;
   Möstl, C.; Perry, C. H.; Rodriguez, L.; Lavraud, B.; Génot, V.;
   Pinto, R. F.; Sanchez-Diaz, E.
2016SoPh..291.1853P    Altcode: 2016SoPh..tmp..118P; 2016arXiv160601127P
  The systematic monitoring of the solar wind in high-cadence and
  high-resolution heliospheric images taken by the Solar-Terrestrial
  Relation Observatory (STEREO) spacecraft permits the study of the
  spatial and temporal evolution of variable solar wind flows from
  the Sun out to 1 AU, and beyond. As part of the EU Framework 7 (FP7)
  Heliospheric Cataloguing, Analysis and Techniques Service (HELCATS)
  project, we have generated a catalog listing the properties of 190
  corotating structures well-observed in images taken by the Heliospheric
  Imager (HI) instruments onboard STEREO-A (ST-A). Based on this catalog,
  we present here one of very few long-term analyses of solar wind
  structures advected by the background solar wind. We concentrate on the
  subset of plasma density structures clearly identified inside corotating
  structures. This analysis confirms that most of the corotating density
  structures detected by the heliospheric imagers comprises a series
  of density inhomogeneities advected by the slow solar wind that
  eventually become entrained by stream interaction regions. We have
  derived the spatial-temporal evolution of each of these corotating
  density structures by using a well-established fitting technique. The
  mean radial propagation speed of the corotating structures is found
  to be 311 ±31 kms−<SUP>1</SUP>. Such a low mean value corresponds
  to the terminal speed of the slow solar wind rather than the speed of
  stream interfaces, which is typically intermediate between the slow and
  fast solar wind speeds (∼400 kms−<SUP>1</SUP>). Using our fitting
  technique, we predicted the arrival time of each corotating density
  structure at different probes in the inner heliosphere. We find that our
  derived speeds are systematically lower by ∼100 kms−<SUP>1</SUP>
  than those measured in situ at the predicted impact times. Moreover,
  for cases when a stream interaction region is clearly detected in situ
  at the estimated impact time, we find that our derived speeds are lower
  than the speed of the stream interface measured in situ by an average
  of 55 kms−<SUP>1</SUP> at ST-A and 84 kms−<SUP>1</SUP> at STEREO-B
  (ST-B). We show that the speeds of the corotating density structures
  derived using our fitting technique track well the long-term variation
  of the radial speed of the slow solar wind during solar minimum years
  (2007 - 2008). Furthermore, we demonstrate that these features originate
  near the coronal neutral line that eventually becomes the heliospheric
  current sheet.

---------------------------------------------------------
Title: An Analysis of Interplanetary Solar Radio Emissions Associated
    with a Coronal Mass Ejection
Authors: Krupar, V.; Eastwood, J. P.; Kruparova, O.; Santolik, O.;
   Soucek, J.; Magdalenić, J.; Vourlidas, A.; Maksimovic, M.; Bonnin,
   X.; Bothmer, V.; Mrotzek, N.; Pluta, A.; Barnes, D.; Davies, J. A.;
   Martínez Oliveros, J. C.; Bale, S. D.
2016ApJ...823L...5K    Altcode: 2016arXiv160604301K
  Coronal mass ejections (CMEs) are large-scale eruptions of magnetized
  plasma that may cause severe geomagnetic storms if Earth directed. Here,
  we report a rare instance with comprehensive in situ and remote
  sensing observations of a CME combining white-light, radio, and plasma
  measurements from four different vantage points. For the first time,
  we have successfully applied a radio direction-finding technique
  to an interplanetary type II burst detected by two identical widely
  separated radio receivers. The derived locations of the type II and
  type III bursts are in general agreement with the white-light CME
  reconstruction. We find that the radio emission arises from the flanks
  of the CME and are most likely associated with the CME-driven shock. Our
  work demonstrates the complementarity between radio triangulation and
  3D reconstruction techniques for space weather applications.

---------------------------------------------------------
Title: The combination of satellite observation techniques for
    sequential ionosphere VTEC modeling
Authors: Erdogan, Eren; Limberger, Marco; Schmidt, Michael; Seitz,
   Florian; Dettmering, Denise; Börger, Klaus; Brandert, Sylvia; Görres,
   Barbara; Kersten, Wilhelm F.; Bothmer, Volker; Hinrichs, Johannes;
   Venzmer, Malte; Mrotzek, Niclas
2016EGUGA..1812685E    Altcode:
  The project OPTIMAP is a joint initiative by the Bundeswehr
  GeoInformation Centre (BGIC), the German Space Situational Awareness
  Centre (GSSAC), the German Geodetic Research Institute of the
  Technical University of Munich (DGFI-TUM) and the Institute for
  Astrophysics at the University of Göttingen (IAG). The main goal is
  to develop an operational tool for ionospheric mapping and prediction
  (OPTIMAP). A key feature of the project is the combination of different
  satellite observation techniques to improve the spatio-temporal data
  coverage and the sensitivity for selected target parameters. In the
  current status, information about the vertical total electron content
  (VTEC) is derived from the dual frequency signal processing of four
  techniques: (1) Terrestrial observations of GPS and GLONASS ensure the
  high-resolution coverage of continental regions, (2) the satellite
  altimetry mission Jason-2 is taken into account to provide VTEC in
  nadir direction along the satellite tracks over the oceans, (3) GPS
  radio occultations to Formosat-3/COSMIC are exploited for the retrieval
  of electron density profiles that are integrated to obtain VTEC and
  (4) Jason-2 carrier-phase observations tracked by the on-board DORIS
  receiver are processed to determine the relative VTEC. All measurements
  are sequentially pre-processed in hourly batches serving as input data
  of a Kalman filter (KF) for modeling the global VTEC distribution. The
  KF runs in a predictor-corrector mode allowing for the sequential
  processing of the measurements where update steps are performed with
  one-minute sampling in the current configuration. The spatial VTEC
  distribution is represented by B-spline series expansions, i.e., the
  corresponding B-spline series coefficients together with additional
  technique-dependent unknowns such as Differential Code Biases and
  Intersystem Biases are estimated by the KF. As a preliminary solution,
  the prediction model to propagate the filter state through time is
  defined by a random walk.

---------------------------------------------------------
Title: Deriving CME kinematics from multipoint space observations
Authors: Mrotzek, Niclas; Pluta, Adam; Bothmer, Volker; Davies,
   Jackie; Harrison, Richard
2016EGUGA..18.8058M    Altcode:
  It is commonly believed that the kinematics of CMEs consist of an early
  Lorentz acceleration phase near the Sun followed by a decelerating
  drag-force phase at distances further out. To better understand
  the physical processes of CME evolution, and also to predict more
  accurately their arrival times at other heliospheric locations,
  we have analysed CMEs using multipoint coronagraph observations
  from STEREO and SOHO. The CME speed evolution is analysed by applying
  time-series GCS-modelling. The analysis is extended to distances further
  away from the Sun through analysis of observations from the STEREO
  heliospheric imagers. The results are compared to those obtained from
  the geometrical modelling of time-elongation profiles of CMEs extracted
  from J-maps. We discuss the implications of our results in the context
  of state-of-the-art space weather predictions. The studies are carried
  out in the EU FP7 project HELCATS (Heliospheric Cataloguing, Analysis
  and Techniques Service).

---------------------------------------------------------
Title: HELCATS - Heliospheric Cataloguing, Analysis and Techniques
    Service
Authors: Harrison, Richard; Davies, Jackie; Perry, Chris; Moestl,
   Christian; Rouillard, Alexis; Bothmer, Volker; Rodriguez, Luciano;
   Eastwood, Jonathan; Kilpua, Emilia; Gallagher, Peter
2016EGUGA..1810220H    Altcode:
  Understanding the evolution of the solar wind is fundamental to
  advancing our knowledge of energy and mass transport in the solar
  system, rendering it crucial to space weather and its prediction. The
  advent of truly wide-angle heliospheric imaging has revolutionised the
  study of both transient (CMEs) and background (SIRs/CIRs) solar wind
  plasma structures, by enabling their direct and continuous observation
  out to 1 AU and beyond. The EU-funded FP7 HELCATS project combines
  European expertise in heliospheric imaging, built up in particular
  through lead involvement in NASA's STEREO mission, with expertise in
  solar and coronal imaging as well as in-situ and radio measurements
  of solar wind phenomena, in a programme of work that will enable a
  much wider exploitation and understanding of heliospheric imaging
  observations. With HELCATS, we are (1.) cataloguing transient and
  background solar wind structures imaged in the heliosphere by STEREO/HI,
  since launch in late October 2006 to date, including estimates of their
  kinematic properties based on a variety of established techniques
  and more speculative, approaches; (2.) evaluating these kinematic
  properties, and thereby the validity of these techniques, through
  comparison with solar source observations and in-situ measurements
  made at multiple points throughout the heliosphere; (3.) appraising
  the potential for initialising advanced numerical models based on
  these kinematic properties; (4.) assessing the complementarity of radio
  observations (in particular of Type II radio bursts and interplanetary
  scintillation) in combination with heliospheric imagery. We will,
  in this presentation, provide an overview of progress from the first
  18 months of the HELCATS project.

---------------------------------------------------------
Title: Impacts of Space Weather Effects on the Ionospheric Vertical
    Total Electron Content
Authors: Hinrichs, Johannes; Bothmer, Volker; Mrotzek, Niclas; Venzmer,
   Malte; Erdogan, Eren; Dettmering, Denise; Limberger, Marco; Schmidt,
   Michael; Seitz, Florian; Börger, Klaus; Brandert, Sylvia; Görres,
   Barbara; Kersten, Wilhelm F.
2016EGUGA..18.7375H    Altcode:
  Space weather effects on the terrestrial ionospheric vertical total
  electron content (VTEC) are caused by solar EUV- and X-Ray emissions,
  solar wind streams and coronal mass ejections (CMEs), amongst other
  processes. They can lead to major disturbances of telecommunication and
  navigation systems. Accurately predicting the global VTEC distribution
  is thus of utmost importance for our societal infrastructure. Here
  we present results obtained within the German space situational
  awareness project OPTIMAP (OPerational Tool for Ionosphere Mapping
  And Prediction) through analyzing the solar effects on the global and
  regional distribution as well as on the temporal variation of the
  ionospheric VTEC. For the state-of-the-art analysis in the OPTIMAP
  project, key data from the GOES, SDO, ACE, SOHO, Proba2 and STEREO
  missions are analysed together with ground based parameters such as
  the F10.7 index. The ionospheric data are taken from global VTEC-maps
  provided by the International GNSS Service (IGS). The results will
  be used as input for the development of an improved operational VTEC
  forecast service providing forecasts up to five days in advance.

---------------------------------------------------------
Title: Global VTEC-modelling in near real-time based on space geodetic
    techniques, adapted B-spline expansions and Kalman-filtering including
    observations of the Sun's radiation
Authors: Börger, Klaus; Schmidt, Michael; Dettmering, Denise;
   Limberger, Marco; Erdogan, Eren; Seitz, Florian; Brandert, Sylvia;
   Görres, Barbara; Kersten, Wilhelm; Bothmer, Volker; Hinrichs,
   Johannes; Venzmer, Malte; Mrotzek, Niclas
2016EGUGA..1812905B    Altcode:
  Today, the observations of space geodetic techniques are usually
  available with a rather low latency which applies to space missions
  observing the solar terrestrial environment, too. Therefore, we
  can use all these measurements in near real-time to compute and to
  provide ionosphere information, e.g. the vertical total electron
  content (VTEC). GSSAC and BGIC support a project aiming at a service
  for providing ionosphere information. This project is called OPTIMAP,
  meaning "Operational Tool for Ionosphere Mapping and Prediction"; the
  scientific work is mainly done by the German Geodetic Research Institute
  of the Technical University Munich (DGFI-TUM) and the Institute for
  Astrophysics of the University of Goettingen (IAG). The OPTIMAP strategy
  for providing ionosphere target quantities of high quality, such as VTEC
  or the electron density, includes mathematical approaches and tools
  allowing for the model adaptation to the real observational scenario
  as a significant improvement w.r.t. the traditional well-established
  methods. For example, OPTIMAP combines different observation types
  such as GNSS (GPS, GLONASS), Satellite Altimetry (Jason-2), DORIS as
  well as radio-occultation measurements (FORMOSAT#3/COSMIC). All these
  observations run into a Kalman-filter to compute global ionosphere
  maps, i.e. VTEC, for the current instant of time and as a forecast for
  a couple of subsequent days. Mathematically, the global VTEC is set
  up as a series expansion in terms of two-dimensional basis functions
  defined as tensor products of trigonometric B-splines for longitude and
  polynomial B-splines for latitude. Compared to the classical spherical
  harmonics, B-splines have a localizing character and, therefore, can
  handle an inhomogeneous data distribution properly. Finally, B-splines
  enable a so-called multi-resolution-representation (MRR) enabling the
  combination of global and regional modelling approaches. In addition
  to the geodetic measurements, Sun observations are pre-processed and
  integrated in the data analysis. Sun observations provide very important
  and useful information that is passed into the Kalman-filter to improve
  the ionosphere predictions.

---------------------------------------------------------
Title: First Results on Visualization and Verification of the
    STEREO Heliospheric Imager CME Catalogue with In Situ Data from the
    Heliophysics System Observatory
Authors: Rollett, T.; Moestl, C.; Boakes, P. D.; Isavnin, A.; Davies,
   J. A.; Byrne, J.; Barnes, D.; Good, S. W.; Perry, C. H.; Kubicka,
   M.; Harrison, R. A.; Kilpua, E.; Forsyth, R. J.; Bothmer, V.
2015AGUFMSH53A2466R    Altcode:
  The space weather community has recently seen major advances in the
  prediction of the speed and arrival time of solar coronal mass ejections
  at Earth and other planets. Since the start of the STEREO mission
  in 2006, each of the heliospheric imagers (HIs) onboard the Ahead
  and Behind spacecraft has successfully tracked hundreds of CMEs. The
  advantage of HI is that CMEs can be followed for a significant part of
  the inner heliosphere, and the CME evolution in direction and speed
  is better constrained than by coronagraphs alone. By tracking and
  cataloguing each of those CMEs in the EU HELCATS project, we can apply
  geometrical modeling (FPF, HMF, SSEF) techniques on single-spacecraft
  HI observations to extract the expected planetary impacts of each
  CME. These arrivals are then verified or refuted by in situ solar wind
  plasma and magnetic field observations provided by the spacecraft
  forming the Heliophysics System Observatory (HSO), such as Wind,
  ACE, Venus Express, MESSENGER, and STEREO-A/B, for which various ICME
  catalogues are gathered and updated in the course of HELCATS.A first
  assessment on the relationship between CME HI and in situ observations
  is discussed, such as occurrence rates, speeds and arrival times and
  magnetic field strength. We also present visualizations of the HI CME
  catalogue and the corresponding in situ observations. The presented
  work has received funding from the European Union Seventh Framework
  Programme (FP7/ 2007-2013) under grant agreement No. 606692 [HELCATS].

---------------------------------------------------------
Title: Radio Triangulation of Type II Bursts Associated with a CME -
    CME Interaction
Authors: Krupar, V.; Bothmer, V.; Davies, J. A.; Eastwood, J. P.;
   Forsyth, R. J.; Kruparova, O.; Magdalenic, J.; Maksimovic, M.;
   Santolik, O.; Soucek, J.; Vourlidas, A.
2015AGUFMSH53B2498K    Altcode:
  Coronal Mass Ejections (CMEs) are large-scale magnetized plasma
  disturbances propagating through the corona and the interplanetary
  (IP) medium. Along their path, some CMEs can drive shock waves, which
  accelerate ions and electrons. These fast electrons can generate
  type II radio bursts at the local plasma frequency and/or its first
  harmonic. In this study we use data from the two STEREO spacecraft
  which carry both imaging and radio instruments with direction-finding
  capabilities allowing us to track energetic electrons responsible
  for radio bursts. We present an analysis of type II bursts observed
  on the November 29 - 30, 2013. The shock wave signatures were
  possibly generated by an interaction of two consecutive CMEs. We have
  investigated three time-frequency intervals when received radio waves
  were sufficiently intense for direction-finding analysis. The obtained
  positions of triangulated radio sources suggest that the CMEs propagate
  towards the STEREO-A. The IP shock associated with this event has been
  also observed in situ by the MESSENGER and STEREO-A spacecraft.

---------------------------------------------------------
Title: HELCATS - Heliospheric Cataloguing, Analysis and Techniques
    Service
Authors: Barnes, D.; Harrison, R. A.; Davies, J. A.; Byrne, J.;
   Perry, C. H.; Moestl, C.; Rouillard, A. P.; Bothmer, V.; Rodriguez,
   L.; Eastwood, J. P.; Kilpua, E.; Odstrcil, D.; Gallagher, P.
2015AGUFMSH21B2410B    Altcode:
  Understanding the evolution of the solar wind is fundamental to
  advancing our knowledge of energy and mass transport in the Solar
  System, making it crucial to space weather and its prediction. The
  advent of truly wide-angle heliospheric imaging has revolutionised
  the study of both transient (CMEs) and background (IRs) solar wind
  plasma structures, by enabling their direct and continuous observation
  out to 1 AU and beyond. The EU-funded FP7 HELCATS project combines
  European expertise in heliospheric imaging, built up in particular
  through lead involvement in NASA's STEREO mission, with expertise in
  solar and coronal imaging as well as in-situ and radio measurements
  of solar wind phenomena, in a programme of work that will enable
  a much wider exploitation and understanding of heliospheric imaging
  observations. The HELCATS project endeavors to catalogue transient and
  background solar wind structures imaged by STEREO/HI throughout the
  duration of the mission. This catalogue will include estimates of their
  kinematic properties using a variety of established and more speculative
  approaches, which are to be evaluated through comparisons with solar
  source and in-situ measurements. The potential for driving numerical
  models from these kinematic properties is to be assessed, as is their
  complementarity to radio observations, specifically Type II bursts and
  interplanetary scintillation. This presentation provides an overview of
  the HELCATS project and its progress in first 18 months of operations.

---------------------------------------------------------
Title: North-south asymmetry in the magnetic deflection of polar
    coronal hole jets
Authors: Nisticò, G.; Zimbardo, G.; Patsourakos, S.; Bothmer, V.;
   Nakariakov, V. M.
2015A&A...583A.127N    Altcode: 2015arXiv150801072N
  Context. Measurements of the sunspots area, of the magnetic field in
  the interplanetary medium, and of the heliospheric current sheet (HCS)
  position, reveal a possible north-south (N-S) asymmetry in the magnetic
  field of the Sun. This asymmetry could cause the bending of the HCS of
  the order of 5-10 deg in the southward direction, and it appears to
  be a recurrent characteristic of the Sun during the minima of solar
  activity. <BR /> Aims: We study the N-S asymmetry as inferred from
  measurements of the deflection of polar coronal hole jets when they
  propagate throughout the corona. <BR /> Methods: Since the corona is
  an environment where the magnetic pressure is greater than the kinetic
  pressure (β ≪ 1), we can assume that the magnetic field controls the
  dynamics of plasma. On average, jets follow magnetic field lines during
  their propagation, highlighting their local direction. We measured
  the position angles at 1 R<SUB>⊙</SUB> and at 2 R<SUB>⊙</SUB> of
  79 jets, based on the Solar TErrestrial RElations Observatory (STEREO)
  ultraviolet and white-light coronagraph observations during the solar
  minimum period March 2007-April 2008. The average jet deflection is
  studied both in the plane perpendicular to the line of sight and, for
  a reduced number of jets, in 3D space. The observed jet deflection is
  studied in terms of an axisymmetric magnetic field model comprising
  dipole (g<SUB>1</SUB>), quadrupole (g<SUB>2</SUB>), and esapole
  (g<SUB>3</SUB>) moments. <BR /> Results: We found that the propagation
  of the jets is not radial, which is in agreement with the deflection
  due to magnetic field lines. Moreover, the amount of the deflection is
  different between jets over the north and those from the south pole. A
  comparison of jet deflections and field line tracing shows that a ratio
  g<SUB>2</SUB>/g<SUB>1</SUB> ≃ -0.5 for the quadrupole and a ratio
  g<SUB>3</SUB>/g<SUB>1</SUB> ≃ 1.6-2.0 for the esapole can describe
  the field. The presence of a non-negligible quadrupole moment confirms
  the N-S asymmetry of the solar magnetic field for the considered
  period. <BR /> Conclusions: We find that the magnetic deflection of
  jets is larger in the north than in the south of the order of 25-40%,
  with an asymmetry that is consistent with a southward deflection of
  the heliospheric current sheet of the order of 10 deg, consistent with
  that inferred from other independent datasets and instruments.

---------------------------------------------------------
Title: Where does the Thermospheric Ionospheric GEospheric Research
    (TIGER) Program go?
Authors: Schmidtke, G.; Avakyan, S. V.; Berdermann, J.; Bothmer,
   V.; Cessateur, G.; Ciraolo, L.; Didkovsky, L.; Dudok de Wit, T.;
   Eparvier, F. G.; Gottwald, A.; Haberreiter, M.; Hammer, R.; Jacobi,
   Ch.; Jakowski, N.; Kretzschmar, M.; Lilensten, J.; Pfeifer, M.;
   Radicella, S. M.; Schäfer, R.; Schmidt, W.; Solomon, S. C.; Thuillier,
   G.; Tobiska, W. K.; Wieman, S.; Woods, T. N.
2015AdSpR..56.1547S    Altcode:
  At the 10th Thermospheric Ionospheric GEospheric Research (TIGER/COSPAR)
  symposium held in Moscow in 2014 the achievements from the start of
  TIGER in 1998 were summarized. During that period, great progress was
  made in measuring, understanding, and modeling the highly variable
  UV-Soft X-ray (XUV) solar spectral irradiance (SSI), and its effects
  on the upper atmosphere. However, after more than 50 years of work the
  radiometric accuracy of SSI observation is still an issue and requires
  further improvement. Based on the extreme ultraviolet (EUV) data from
  the SOLAR/SolACES, and SDO/EVE instruments, we present a combined data
  set for the spectral range from 16.5 to 105.5 nm covering a period
  of 3.5 years from 2011 through mid of 2014. This data set is used
  in ionospheric modeling of the global Total Electron Content (TEC),
  and in validating EUV SSI modeling. For further investigations the
  period of 3.5 years is being extended to about 12 years by including
  data from SOHO/SEM and TIMED/SEE instruments. Similarly, UV data are
  used in modeling activities. After summarizing the results, concepts
  are proposed for future real-time SSI measurements with in-flight
  calibration as experienced with the ISS SOLAR payload, for the
  development of a space weather camera for observing and investigating
  space weather phenomena in real-time, and for providing data sets for
  SSI and climate modeling. Other planned topics are the investigation
  of the relationship between solar EUV/UV and visible/near-infrared
  emissions, the impact of X-rays on the upper atmosphere, the development
  of solar EUV/UV indices for different applications, and establishing a
  shared TIGER data system for EUV/UV SSI data distribution and real-time
  streaming, also taking into account the achievements of the FP7 SOLID
  (First European SOLar Irradiance Data Exploitation) project. For further
  progress it is imperative that coordinating activities in this special
  field of solar-terrestrial relations and solar physics is emphasized.

---------------------------------------------------------
Title: An Application of the Stereoscopic Self-similar-Expansion
    Model to the Determination of CME-Driven Shock Parameters
Authors: Volpes, L.; Bothmer, V.
2015SoPh..290.3005V    Altcode: 2015SoPh..tmp..121V; 2015arXiv150903181V
  We present an application of the stereoscopic self-similar-expansion
  model (SSSEM) to Solar Terrestrial Relations Observatory
  (STEREO)/Sun-Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) observations of the CME on 3 April 2010 and its associated
  shock. The aim is to verify whether CME-driven shock parameters can
  be inferred from the analysis of j-maps. For this purpose, we used
  the SSSEM to derive the CME and the shock kinematics. Arrival times
  and speeds, inferred assuming either propagation at constant speed
  or with uniform deceleration, agree well with Advanced Composition
  Explorer (ACE) measurements. The shock standoff distance [Δ ], the
  density compression [ρ/<SUB>d</SUB>ρ<SUB>u</SUB>], and the Mach
  number [M ] were calculated by combining the results obtained for the
  CME and shock kinematics with models for the shock location. Their
  values were extrapolated to L<SUB>1</SUB> and compared to in-situ
  data. The in-situ standoff distance was obtained from ACE solar-wind
  measurements, and the Mach number and compression ratio were provided by
  the interplanetary shock database of the Harvard-Smithsonian Center
  for Astrophysics. They are ρ/<SUB>d</SUB>ρ<SUB>u</SUB>=2.84 and
  M =2.2 . The best fit to observations was obtained when the SSSEM
  half-width λ =40<SUP>∘</SUP>, and the CME and shock propagate with
  uniform deceleration. In this case we found Δ =23 R<SUB>⊙</SUB>,
  ρ/<SUB>d</SUB>ρ<SUB>u</SUB>=2.61 , and M =2.93 . The study shows
  that CME-driven shock parameters can be estimated from the analysis of
  time-elongation plots and can be used to predict their in-situ values.

---------------------------------------------------------
Title: On the interplanetary evolution of CME-driven shocks: a
    comparison between remote sensing observations and in-situ data
Authors: Volpes, Laura; Bothmer, Volker
2015IAUGA..2256648V    Altcode:
  Fast coronal mass ejections (CMEs) are a prime driver of major space
  weather effects and strong geomagnetic storms. When the CME propagation
  speed is higher than the Alfvén speed a shock forms in front of the CME
  leading edge. CME-driven shocks are observed in in-situ data and, with
  the advent of increasingly sensitive imaging instruments, also in remote
  sensing observations in the form of bright fronts ahead of the CMEs.In
  this work we present the study of 4 Earth-directed CMEs which drove
  shocks detected in STEREO COR 2 and HI observations. For each event we
  identify the source region and the signatures of CME eruption such as
  waves, EUV dimmings, flare and prominence eruptions. The shock and CME
  interplanetary evolution is determined from COR2 and HI observations via
  an application of triangulation techniques. Furthermore, propagation
  speed and arrival times are inferred. The CME geometry is modelled in
  COR2 via the graduated cylindrical shell (GCS) model and the assumption
  on self-similar expansion is tested by expanding the flux rope to the
  HI1 field of view. A combination of these results with models for the
  shock location allows to infer the time evolution of the compression
  ratio ρ<SUB>d</SUB>/ρ<SUB>u</SUB> across the shock and of the upstream
  Mach number M at locations where no direct plasma measurements are
  available. These values, as well as the arrival time and speed, are
  compared to ACE in-situ measurements to validate the results. For
  the 03 April 2010 event, e.g., the values of the Mach number and the
  compression ratio extrapolated to the position of ACE are respectively
  2.1 &lt; ρ<SUB>d</SUB>/ρ<SUB>u</SUB> &lt; 2.4 and 2.3 &lt; M &lt;
  2.5, in good agreement with the in-situ values found in literature,
  ρ<SUB>d</SUB>/ρ<SUB>u</SUB> = 2.84 and M = 2.2. This study is carried
  out in conjunction to simulations of CME initiation. Combined results
  from observations and simulations allow to connect the interplanetary
  and near-Earth properties of CMEs to those of their source regions,
  and to the mechanisms of CME onset.

---------------------------------------------------------
Title: On the interplanetary evolution of CME-driven shocks: a
    comparison between remote sensing observations and in-situ data
Authors: Volpes, Laura; Bothmer, Volker
2015IAUGA..2254866V    Altcode:
  Fast coronal mass ejections (CMEs) are a prime driver of major space
  weather effects and strong geomagnetic storms. When the CME propagation
  speed is higher than the Alfvén speed a shock forms in front of the CME
  leading edge. CME-driven shocks are observed in in-situ data and, with
  the advent of increasingly sensitive imaging instruments, also in remote
  sensing observations in the form of bright fronts ahead of the CMEs.In
  this work we present the study of 4 Earth-directed CMEs which drove
  shocks detected in STEREO COR 2 and HI observations. For each event we
  identify the source region and the signatures of CME eruption such as
  waves, EUV dimmings, flare and prominence eruptions. The shock and CME
  interplanetary evolution is determined from COR2 and HI observations via
  an application of triangulation techniques. Furthermore, propagation
  speed and arrival times are inferred. The CME geometry is modelled in
  COR2 via the graduated cylindrical shell (GCS) model and the assumption
  on self-similar expansion is tested by expanding the flux rope to the
  HI1 field of view. A combination of these results with models for the
  shock location allows to infer the time evolution of the compression
  ratio ρ<SUB>d</SUB>/ρ<SUB>u</SUB> across the shock and of the upstream
  Mach number M at locations where no direct plasma measurements are
  available. These values, as well as the arrival time and speed, are
  compared to ACE in-situ measurements to validate the results. For
  the 03 April 2010 event, e.g., the values of the Mach number and the
  compression ratio extrapolated to the position of ACE are respectively
  2.1 &lt; ρ<SUB>d</SUB>/ρ<SUB>u</SUB> &lt; 2.4 and 2.3 &lt; M &lt;
  2.5, in good agreement with the in-situ values found in literature,
  ρ<SUB>d</SUB>/ρ<SUB>u</SUB> = 2.84 and M = 2.2. This study is carried
  out in conjunction to simulations of CME initiation. Combined results
  from observations and simulations allow to connect the interplanetary
  and near-Earth properties of CMEs to those of their source regions,
  and to the mechanisms of CME onset.

---------------------------------------------------------
Title: Where no dust instrument has gone before: Dust science with
    Solar Probe Plus
Authors: Rodmann, Jens; Bothmer, Volker; Thernisien, Arnaud
2015EGUGA..1712390R    Altcode:
  Solar Probe Plus will be a ground-breaking mission to explore the
  innermost regions of the solar system. By flying down to less than 10
  solar radii (~0.05 AU), the mission will greatly enhance our knowledge
  of the Near-Sun dust environment. This region is governed by a poorly
  understood interplay of dust delivery by sungrazing comets and radiation
  forces, the destruction of dust by sublimation, and interactions of dust
  particles with the ambient coronal plasma. We will focus on two Solar
  Probe Plus instruments relevant for dust: (1) the Wide-field Imager
  for SolarPRobe (WISPR), a white-light heliospheric imager dedicated
  to study the solar wind, coronal mass ejections, and dust-plasma
  interactions; (2) the FIELDS Experiment aimed at electric and magnetic
  field measurements in the solar wind, that can also detect telltale
  voltage signatures of dust-particle impacts on the spacecraft. We
  will highlight recent simulations of the scattered-light emission
  from dust particles (F-corona) in order to assess the capabilities of
  the WISPR instrument to image the dust-free zone around the Sun. We
  will test whether dust density enhancements as predicted by dynamical
  simulations can be identified and resolved. Furthermore, we will discuss
  whether WISPR imagery will allow us to separate composition-dependent
  sublimation fronts, e.g. for silicates or carbonaceous dust. For FIELDS,
  we will present predictions for count rates and impact velocities of
  micron-sized dust particle hits expected over the 7-year mission.

---------------------------------------------------------
Title: The HELCATS Project: Characterising the Evolution of Coronal
    Mass Ejections Observed During Solar Cycle 24
Authors: Bisi, M. M.; Harrison, R. A.; Davies, J. A.; Perry, C. H.;
   Moestl, C.; Rouillard, A. P.; Bothmer, V.; Rodriguez, L.; Eastwood,
   J. P.; Kilpua, E.; Gallagher, P.; Odstrcil, D.
2014AGUFMSH43B4214B    Altcode:
  Understanding the evolution of coronal mass ejections (CMEs) is
  fundamental to advancing our knowledge of energy and mass transport in
  the solar system, thus also rendering it crucial to space weather and
  its prediction. The advent of truly wide-angle heliospheric imaging
  has revolutionised the study of CMEs, by enabling their direct and
  continuous observation as they propagate from the Sun out to 1 AU and
  beyond. The recently initiated EU-funded FP7 Heliospheric Cataloguing,
  Analysis and Technique Service (HELCATS) project combines European
  expertise in the field of heliospheric imaging, built up over the last
  decade in particular through lead involvement in NASA's STEREO mission,
  with expertise in such areas as solar and coronal imaging as well as
  the interpretation of in-situ and radio diagnostic measurements of
  solar wind phenomena. The goals of HELCATS include the cataloguing
  of CMEs observed in the heliosphere by the Heliospheric Imager
  (HI) instruments on the STEREO spacecraft, since their launch in
  late October 2006 to date, an interval that covers much of the
  historically weak solar cycle 24. Included in the catalogue will be
  estimates of the kinematic properties of the imaged CMEs, based on a
  variety of established, and some more speculative, modelling approaches
  (geometrical, forward, inverse, magneto-hydrodynamic); these kinematic
  properties will be verified through comparison with solar disc and
  coronal imaging observations, as well as through comparison with radio
  diagnostic and in-situ measurements made at multiple points throughout
  the heliosphere. We will provide an overview of the HELCATS project,
  and present initial results that will seek to illuminate the unusual
  nature of solar cycle 24.

---------------------------------------------------------
Title: North-South Asymmetry in the Magnetic Deflection of Polar
    Coronal Jets
Authors: Nisticò, Giuseppe; Zimbardo, Gaetano; Bothmer, Volker;
   Patsourakos, Spiros
2014cosp...40E2295N    Altcode:
  Solar jets observed with the Extreme Ultra-Violet Imager (EUVI) and
  CORonagraphs (COR) instruments aboard the STEREO mission provide a tool
  to probe and understand the magnetic structure of the corona. Since
  the corona is an environment where the magnetic pressure is greater
  than the kinetic pressure, the magnetic field controls the dynamics
  of plasma and, on average, jets during their propagation trace
  the magnetic field lines. We discuss the North-South asymmetry of
  the magnetic field of the Sun as inferred from measurements of the
  deflection of polar coronal hole jets when they propagate throughout
  the corona. We measured the position angle at 1 and at 2 solar radii
  for the 79 jets of the catalogue of Nisticò et al. (2009), based on
  the STEREO ultraviolet and visible observations, and we found that the
  propagation is not radial. The average jet deflection is studied both in
  the plane perpendicular to the line of sight, and, for a reduced number
  of jets in the three dimensional (3D) space. We find that the magnetic
  deflection of jets is larger in the North than in the South, with an
  asymmetry which is consistent with the N-S asymmetry of the heliospheric
  magnetic field inferred from the Ulysses in situ measurements, and
  gives clues to the study of the large scale solar magnetic field.

---------------------------------------------------------
Title: 3D forecast of major geomagnetic storms
Authors: Bosman, Eckhard; Odstrcil, Dusan; Hesemann, Jonas; Milward,
   George; Venzmer, Malte; Volpes, Laura; Bothmer, Volker; Viereck, Rodney
2013EGUGA..1511840B    Altcode:
  A 3D analysis of coronal mass ejection events leading to major
  geomagnetic storms in solar cycle 24 has been carried out with help
  of STEREO and SOHO multipoint observations. The results from the CME
  modeling through application of the GCS and CAT methods were used as
  inner boundary conditions for the ENLIL simulations. Comparison of
  multipoint in situ CME measurements with the ENLIL results provides
  information on the 3D accuracy of the space weather forecasts and
  implications for future mission plannings near L5 or sub L1 orbits.

---------------------------------------------------------
Title: AFFECTS - Advanced Forecast For Ensuring Communications
    Through Space
Authors: Bothmer, Volker
2013EGUGA..1511752B    Altcode:
  Through the AFFECTS project funded by the European Union's 7th
  Framework Programme, European and US scientists develop an advanced
  proto-type space weather warning system to safeguard the operation of
  telecommunication and navigation systems on Earth to the threat of solar
  storms. The project is led by the University of Göttingen's Institute
  for Astrophysics and comprises worldwide leading research and academic
  institutions and industrial enterprises from Germany, Belgium, Ukraine,
  Norway and the United States. The key objectives of the AFFECTS project
  are: State-of-the-art analysis and modelling of the Sun-Earth chain
  of effects on the Earth's ionosphere and their subsequent impacts
  on communication systems based on multipoint space observations and
  complementary ground-based data. Development of a prototype space
  weather early warning system and reliable space weather forecasts,
  with specific emphasis on ionospheric applications. Dissemination of
  new space weather products and services to end users, the scientific
  community and general public. The presentation summarizes the project
  highlights, with special emphasis on the developed space weather
  forecast tools.

---------------------------------------------------------
Title: Three-Dimensional Properties of Coronal Mass Ejections from
    STEREO/SECCHI Observations
Authors: Bosman, E.; Bothmer, V.; Nisticò, G.; Vourlidas, A.; Howard,
   R. A.; Davies, J. A.
2012SoPh..281..167B    Altcode: 2012SoPh..tmp..234B
  We identify 565 coronal mass ejections (CMEs) between January 2007
  and December 2010 in observations from the twin STEREO/SECCHI/COR2
  coronagraphs aboard the STEREO mission. Our list is in full
  agreement with the corresponding SOHO/LASCO CME Catalog
  (http://cdaw.gsfc.nasa.gov/CME_list/) for events with angular
  widths of 45<SUP>∘</SUP> and up. The monthly event rates behave
  similarly to sunspot rates showing a three- to fourfold rise between
  September 2009 and March 2010. We select 51 events with well-defined
  white-light structure and model them as three-dimensional (3D) flux
  ropes using a forward-modeling technique developed by Thernisien,
  Howard and Vourlidas (Astrophys. J. 652, 763 - 773, 2006). We derive
  their 3D properties and identify their source regions. We find that
  the majority of the CME flux ropes (82 %) lie within 30<SUP>∘</SUP>
  of the solar equator. Also, 82 % of the events are displaced from their
  source region, to a lower latitude, by 25<SUP>∘</SUP> or less. These
  findings provide strong support for the deflection of CMEs towards
  the solar equator reported in earlier observations, e.g. by Cremades
  and Bothmer (Astron. Astrophys.422, 307 - 322, 2004).

---------------------------------------------------------
Title: Observational Tracking of the 2D Structure of Coronal Mass
    Ejections Between the Sun and 1 AU
Authors: Savani, N. P.; Davies, J. A.; Davis, C. J.; Shiota, D.;
   Rouillard, A. P.; Owens, M. J.; Kusano, K.; Bothmer, V.; Bamford,
   S. P.; Lintott, C. J.; Smith, A.
2012SoPh..279..517S    Altcode: 2015arXiv150308774S
  The Solar TErrestrial RElations Observatory (STEREO) provides high
  cadence and high resolution images of the structure and morphology of
  coronal mass ejections (CMEs) in the inner heliosphere. CME directions
  and propagation speeds have often been estimated through the use of
  time-elongation maps obtained from the STEREO Heliospheric Imager (HI)
  data. Many of these CMEs have been identified by citizen scientists
  working within the SolarStormWatch project (www.solarstormwatch.com)
  as they work towards providing robust real-time identification of
  Earth-directed CMEs. The wide field of view of HI allows scientists
  to directly observe the two-dimensional (2D) structures, while the
  relative simplicity of time-elongation analysis means that it can be
  easily applied to many such events, thereby enabling a much deeper
  understanding of how CMEs evolve between the Sun and the Earth. For
  events with certain orientations, both the rear and front edges of the
  CME can be monitored at varying heliocentric distances (R) between
  the Sun and 1 AU. Here we take four example events with measurable
  position angle widths and identified by the citizen scientists. These
  events were chosen for the clarity of their structure within the HI
  cameras and their long track lengths in the time-elongation maps. We
  show a linear dependency with R for the growth of the radial width
  (W) and the 2D aspect ratio (χ) of these CMEs, which are measured
  out to ≈ 0.7 AU. We estimated the radial width from a linear best
  fit for the average of the four CMEs. We obtained the relationships
  W=0.14R+0.04 for the width and χ=2.5R+0.86 for the aspect ratio
  (W and R in units of AU).

---------------------------------------------------------
Title: Solar and Interplanetary Data availability for space weather
Authors: Bothmer, Volker
2012cosp...39..227B    Altcode: 2012cosp.meet..227B
  Multi-point space missions, such as STEREO, SDO, SOHO, ACE and
  Proba2, with dedicated instrumentations operating in the Sun-Earth
  system currently provide a huge amount of unprecedented solar and
  interplanetary observations. The data from these missions as well as
  unique other long-term datasets already established provide to date
  unique input resources for quantification of space weather processes and
  the development of reliable space weather models. In this presentation
  I will give an overview on the availability of these datasets to the
  scientific community, the tools required for access of these datasets,
  namely the VOs and website resources, and brief comments on their
  individual importance for the various fields of space weather research.

---------------------------------------------------------
Title: Observing Space Weather towards building Predictive
    Capabilities
Authors: Bothmer, Volker
2012cosp...39..226B    Altcode: 2012cosp.meet..226B
  Simultaneous data from multi-point space missions operating in
  the Sun-Earth system in conjunction with dedicated ground- based
  networks have facilitated major steps towards the quantification of
  space weather processes, better understandings of their impacts on
  the various high level systems of modern societal infrastructure and
  fundamental developments in space weather forecasting. Through the
  EU FP7 program and the ESA Space Situational Awareness (SSA) program
  several dedicated space weather projects and studies have currently
  been initiated, such as the AFFECTS (Advanced Forecast For Ensuring
  Communications Through Space), aiming in establishing prototype
  space weather services, instruments and missions as precursors of a
  future space weather operational system. This presentation provides
  an overview of the ongoing European activities, upcoming challenges
  and opportunities for international collaborations.

---------------------------------------------------------
Title: 3D Modeling of CMEs observed with STEREO
Authors: Bosman, E.; Bothmer, V.
2012EGUGA..1411632B    Altcode:
  From January 2007 until end of 2010, 565 typical large-scale coronal
  mass ejections (CMEs) have been identified in the SECCHI/COR2 synoptic
  movies of the STEREO Mission. A subset comprising 114 CME events,
  selected based on the CME's brightness appearance in the SECCHI/COR2
  images, has been modeled through the Graduated Cylindrical Shell (GCS)
  Model developed by Thernisien et al. (2006). This study presents an
  overview of the GCS forward-modeling results and an interpretation of
  the CME characteristics in relationship to their solar source region
  properties and solar cycle appearances.

---------------------------------------------------------
Title: CME-CME interaction during the 2010 August 1 events
Authors: Temmer, M.; Vrsnak, B.; Rollett, T.; Bein, B.; deKoning,
   C. A.; Liu, Y.; Bosman, E.; Davies, J. A.; Möstl, C.; Zic, T.;
   Veronig, A. M.; Bothmer, V.; Harrison, R.; Nitta, N.; Bisi, M.; Flor,
   O.; Eastwood, J.; Odstrcil, D.; Forsyth, R.
2012EGUGA..14.1677T    Altcode:
  We study a CME-CME interaction that occurred during the 2010 August 1
  events using STEREO/SECCHI data (COR and HI). The CMEs were Earth
  directed where clear signatures of magnetic flux ropes could be
  measured from in situ Wind data. To give evidence of the actual
  interaction we derive the direction of motion for both CMEs applying
  several independent methods. From this we obtain that both CMEs head
  into similar directions enabling us to actually observe the merging
  in the HI1 field-of-view (and rule out the possibility that this is
  just a line of sight effect). The full de-projected kinematics of the
  faster CME from Sun to Earth is derived when combining data points from
  remote observations with in situ parameters of the ICME measured at
  1 AU. We study the evolution of the kinematical profile of the faster
  CME by applying a drag based model.

---------------------------------------------------------
Title: Characteristics of Kinematics of a Coronal Mass Ejection
    during the 2010 August 1 CME-CME Interaction Event
Authors: Temmer, Manuela; Vršnak, Bojan; Rollett, Tanja; Bein, Bianca;
   de Koning, Curt A.; Liu, Ying; Bosman, Eckhard; Davies, Jackie A.;
   Möstl, Christian; Žic, Tomislav; Veronig, Astrid M.; Bothmer, Volker;
   Harrison, Richard; Nitta, Nariaki; Bisi, Mario; Flor, Olga; Eastwood,
   Jonathan; Odstrcil, Dusan; Forsyth, Robert
2012ApJ...749...57T    Altcode: 2012arXiv1202.0629T
  We study the interaction of two successive coronal mass ejections (CMEs)
  during the 2010 August 1 events using STEREO/SECCHI COR and heliospheric
  imager (HI) data. We obtain the direction of motion for both CMEs by
  applying several independent reconstruction methods and find that the
  CMEs head in similar directions. This provides evidence that a full
  interaction takes place between the two CMEs that can be observed in the
  HI1 field of view. The full de-projected kinematics of the faster CME
  from Sun to Earth is derived by combining remote observations with in
  situ measurements of the CME at 1 AU. The speed profile of the faster
  CME (CME2; ~1200 km s<SUP>-1</SUP>) shows a strong deceleration over
  the distance range at which it reaches the slower, preceding CME (CME1;
  ~700 km s<SUP>-1</SUP>). By applying a drag-based model we are able
  to reproduce the kinematical profile of CME2, suggesting that CME1
  represents a magnetohydrodynamic obstacle for CME2 and that, after
  the interaction, the merged entity propagates as a single structure
  in an ambient flow of speed and density typical for quiet solar wind
  conditions. Observational facts show that magnetic forces may contribute
  to the enhanced deceleration of CME2. We speculate that the increase
  in magnetic tension and pressure, when CME2 bends and compresses the
  magnetic field lines of CME1, increases the efficiency of drag.

---------------------------------------------------------
Title: Observations of the White Light Corona from Solar Orbiter
    and Solar Probe Plus
Authors: Howard, R. A.; Thernisien, A. F.; Vourlidas, A.; Plunkett,
   S. P.; Korendyke, C. M.; Sheeley, N. R.; Morrill, J. S.; Socker,
   D. G.; Linton, M. G.; Liewer, P. C.; De Jong, E. M.; Velli, M. M.;
   Mikic, Z.; Bothmer, V.; Lamy, P. L.
2011AGUFMSH43F..06H    Altcode:
  The SoloHI instrument on Solar Orbiter and the WISPR instrument on Solar
  Probe+ will make white light coronagraphic images of the corona as the
  two spacecraft orbit the Sun. The minimum perihelia for Solar Orbiter
  is about 60 Rsun and for SP+ is 9.5 Rsun. The wide field of view of the
  WISPR instrument (about 105 degrees radially) corresponds to viewing
  the corona from 2.2 Rsun to 20 Rsun. Thus the entire Thomson hemisphere
  is contained within the telescope's field and we need to think of
  the instrument as being a traditional remote sensing instrument and
  then transitioning to a local in-situ instrument. The local behavior
  derives from the fact that the maximum Thomson scattering will favor
  the electron plasma close to the spacecraft - exactly what the in-situ
  instruments will be sampling. SoloHI and WISPR will also observe
  scattered light from dust in the inner heliosphere, which will be an
  entirely new spatial regime for dust observations from a coronagraph,
  which we assume to arise from dust in the general neighborhood of about
  half way between the observer and the Sun. As the dust grains approach
  the Sun, they evaporate and do not contribute to the scattering. A
  dust free zone has been postulated to exist somewhere inside of 5 Rsun
  where all dust is evaporated, but this has never been observed. The
  radial position where the evaporation occurs will depend on the
  precise molecular composition of the individual grains. The orbital
  plane of Solar Orbiter will gradually increase up to about 35 degrees,
  enabling a very different view through the zodiacal dust cloud to test
  the models generated from in-ecliptic observations. In this paper we
  will explore some of the issues associated with the observation of
  the dust and will present a simple model to explore the sensitivity
  of the instrument to observe such evaporations.

---------------------------------------------------------
Title: Determination of temperature maps of EUV coronal hole jets
Authors: Nisticò, Giuseppe; Patsourakos, Spiros; Bothmer, Volker;
   Zimbardo, Gaetano
2011AdSpR..48.1490N    Altcode:
  Coronal hole jets are fast ejections of plasma occurring within
  coronal holes, observed at Extreme-UltraViolet (EUV) and X-ray
  wavelengths. Recent observations of jets by the STEREO and Hinode
  missions show that they are transient phenomena which occur at much
  higher rates than large-scale impulsive phenomena like flares and
  Coronal Mass Ejections (CMEs). In this paper we describe some typical
  characteristics of coronal jets observed by the SECCHI instruments
  of STEREO spacecraft. We show an example of 3D reconstruction of
  the helical structure for a south pole jet, and present how the
  angular distribution of the jet position angles changes from the
  Extreme-UltraViolet-Imager (EUVI) field of view to the CORonagraph1
  (COR1) (height ∼2.0 R<SUB>⊙</SUB> heliocentric distance) field
  of view. Then we discuss a preliminary temperature determination for
  the jet plasma by using the filter ratio method at 171 and 195 Å and
  applying a technique for subtracting the EUV background radiation. The
  results show that jets are characterized by electron temperatures
  ranging between 0.8 and 1.3 MK. We present the thermal structure of
  the jet as temperature maps and we describe its thermal evolution.

---------------------------------------------------------
Title: Evolution of Coronal Mass Ejection Morphology with Increasing
    Heliocentric Distance. II. In Situ Observations
Authors: Savani, N. P.; Owens, M. J.; Rouillard, A. P.; Forsyth,
   R. J.; Kusano, K.; Shiota, D.; Kataoka, R.; Jian, L.; Bothmer, V.
2011ApJ...732..117S    Altcode:
  Interplanetary coronal mass ejections (ICMEs) are often observed to
  travel much faster than the ambient solar wind. If the relative speed
  between the two exceeds the fast magnetosonic velocity, then a shock
  wave will form. The Mach number and the shock standoff distance ahead
  of the ICME leading edge is measured to infer the vertical size of an
  ICME in a direction that is perpendicular to the solar wind flow. We
  analyze the shock standoff distance for 45 events varying between
  0.5 AU and 5.5 AU in order to infer their physical dimensions. We
  find that the average ratio of the inferred vertical size to measured
  radial width, referred to as the aspect ratio, of an ICME is 2.8 ±
  0.5. We also compare these results to the geometrical predictions from
  Paper I that forecast an aspect ratio between 3 and 6. The geometrical
  solution varies with heliocentric distance and appears to provide a
  theoretical maximum for the aspect ratio of ICMEs. The minimum aspect
  ratio appears to remain constant at 1 (i.e., a circular cross section)
  for all distances. These results suggest that possible distortions to
  the leading edge of ICMEs are frequent. But, these results may also
  indicate that the constants calculated in the empirical relationship
  correlating the different shock front need to be modified; or perhaps
  both distortions and a change in the empirical formulae are required.

---------------------------------------------------------
Title: Observational features of equatorial coronal hole jets
Authors: Nisticò, G.; Bothmer, V.; Patsourakos, S.; Zimbardo, G.
2010AnGeo..28..687N    Altcode: 2010arXiv1002.2181N
  Collimated ejections of plasma called "coronal hole jets" are commonly
  observed in polar coronal holes. However, such coronal jets are not only
  a specific features of polar coronal holes but they can also be found
  in coronal holes appearing at lower heliographic latitudes. In this
  paper we present some observations of "equatorial coronal hole jets"
  made up with data provided by the STEREO/SECCHI instruments during
  a period comprising March 2007 and December 2007. The jet events
  are selected by requiring at least some visibility in both COR1 and
  EUVI instruments. We report 15 jet events, and we discuss their main
  features. For one event, the uplift velocity has been determined as
  about 200 km s<SUP>-1</SUP>, while the deceleration rate appears to
  be about 0.11 km s<SUP>-2</SUP>, less than solar gravity. The average
  jet visibility time is about 30 min, consistent with jet observed in
  polar regions. On the basis of the present dataset, we provisionally
  conclude that there are not substantial physical differences between
  polar and equatorial coronal hole jets.

---------------------------------------------------------
Title: The nature of micro CMEs within coronal holes
Authors: Bothmer, Volker; Nistico, Giuseppe; Zimbardo, Gaetano;
   Patsourakos, Spiros; Bosman, Eckhard
2010cosp...38.2840B    Altcode: 2010cosp.meet.2840B
  Whilst investigating the origin and characteristics of coronal jets
  and large-scale CMEs identi-fied in data from the SECCHI (Sun Earth
  Connection Coronal and Heliospheric Investigation) instrument suites
  on board the two STEREO satellites, we discovered transient events
  that originated in the low corona with a morphology resembling that of
  typical three-part struc-tured coronal mass ejections (CMEs). However,
  the CMEs occurred on considerably smaller spatial scales. In this
  presentation we show evidence for the existence of small-scale CMEs
  from inside coronal holes and present quantitative estimates of their
  speeds and masses. We interprete the origin and evolution of micro
  CMEs as a natural consequence of the emergence of small-scale magnetic
  bipoles related to the Sun's ever changing photospheric magnetic flux
  on various scales and their interactions with the ambient plasma and
  magnetic field. The analysis of CMEs is performed within the framework
  of the EU Erasmus and FP7 SOTERIA projects.

---------------------------------------------------------
Title: Solar Observations -What is needed for Space Weather
    Monitoring ?
Authors: Bothmer, Volker
2010cosp...38.4182B    Altcode: 2010cosp.meet.4182B
  The Sun is our star and the prime source of space weather. Over the
  past decades, space missions with sophisticated payloads have led us
  to discover and explore the dynamics of our Sun and its impact on the
  heliosphere in unprecedented detail. A new level of understanding of the
  physics behind solar activity has been achieved and state-of-the-art
  missions like STEREO, Hinode, SDO, Proba2 and ACE, as well as future
  missions like Proba3, Solar Orbiter, Solar Probe Plus or Solar-C will
  close existing gaps in our knowledge. Accordingly, what was formerly
  known as the field of "solar-terrestrial research" has basically evolved
  into the field of "space weather", a highly interdisciplinary field of
  science that includes the impacts of space weather on those technical
  systems that are crucial to modern society. In order to proceed to the
  next stage, it is necessary to quantify the key physical processes
  in the Sun-Earth system and to define those space-and ground-based
  solar observations and measurements that are needed to provide
  operational space weather forecasts, given the technical and budgetary
  thresholds. This presentation summarises the state-of-the-art assets,
  near-term and future projects and identifies existing observational
  gaps. Based on these conclusions, dedicated concepts for Sun and
  interplanetary monitoring systems for space weather purposes are
  presented.

---------------------------------------------------------
Title: 3D structure of CMEs observed with STEREO/SECCHI
Authors: Bothmer, Volker; Bosman, Eckhard; Thernisien, Arnaud
2010cosp...38.1870B    Altcode: 2010cosp.meet.1870B
  Since launch in October 2006, the SECCHI remote sensing suites on
  board the two STEREO spacecraft have observed so far more than 300
  coronal mass ejections (CMEs) at increasing angular separation. Using
  SECCHI and additionally SOHO/MDI/EIT observations, we have studied
  the CME 3D structure and source regions for these events. Here we
  present a summary of first results of this analysis performed within
  the framework of the EU FP7 project SOTERIA.

---------------------------------------------------------
Title: Classification and Physical parameters EUV coronal jets with
    STEREO/SECCHI.
Authors: Nistico, Giuseppe; Bothmer, Volker; Patsourakos, Spiro;
   Zimbardo, Gaetano
2010cosp...38.1820N    Altcode: 2010cosp.meet.1820N
  In this work we present observations of EUV coronal jets, detected with
  the SECCHI (Sun Earth Connection Coronal and Heliospheric Investigation)
  imaging suites of the two STEREO spacecraft. Starting from catalogues of
  polar and equatorial coronal hole jets (Nistico' et al., Solar Phys.,
  259, 87, 2009; Ann. Geophys. in press), identified from simultaneous
  EUV and white-light coronagraph observations, taken during the time
  period March 2007 to April 2008 when solar activity was at minimum,
  we perfom a detailed study of some events. A basic char-acterisation of
  the magnetic morphology and identification of the presence of helical
  structure were established with respect to recently proposed models
  for their origin and temporal evo-lution. A classification of the
  events with respect to previous jet studies shows that amongst the 79
  events, identified into polar coronal holes, there were 37 Eiffel tower
  -type jet events commonly interpreted as a small-scale ( 35 arcsec)
  magnetic bipole reconnecting with the ambi-ent unipolar open coronal
  magnetic fields at its looptops, 12 lambda-type jet events commonly
  interpreted as reconnection with the ambient field happening at the
  bipoles footpoints. Five events were termed micro-CME type jet events
  because they resembled classical three-part structured coronal mass
  ejections (CMEs) but on much smaller scales. The remainig 25 cases
  could not be uniquely classified. Thirty-one of the total number of
  events exhibited a helical magnetic field structure, indicative for a
  torsional motion of the jet around its axis of propaga-tion. The jet
  events are found to be also present in equatorial coronal holes. We
  also present the 3-D reconstruction, temperature, velocity, and density
  measurements of a number of jets during their evolution.

---------------------------------------------------------
Title: Solar Weather Event Modelling and Prediction
Authors: Messerotti, Mauro; Zuccarello, Francesca; Guglielmino,
   Salvatore L.; Bothmer, Volker; Lilensten, Jean; Noci, Giancarlo;
   Storini, Marisa; Lundstedt, Henrik
2009SSRv..147..121M    Altcode:
  Key drivers of solar weather and mid-term solar weather are reviewed
  by considering a selection of relevant physics- and statistics-based
  scientific models as well as a selection of related prediction models,
  in order to provide an updated operational scenario for space weather
  applications. The characteristics and outcomes of the considered
  scientific and prediction models indicate that they only partially cope
  with the complex nature of solar activity for the lack of a detailed
  knowledge of the underlying physics. This is indicated by the fact that,
  on one hand, scientific models based on chaos theory and non-linear
  dynamics reproduce better the observed features, and, on the other
  hand, that prediction models based on statistics and artificial neural
  networks perform better. To date, the solar weather prediction success
  at most time and spatial scales is far from being satisfactory, but
  the forthcoming ground- and space-based high-resolution observations
  can add fundamental tiles to the modelling and predicting frameworks
  as well as the application of advanced mathematical approaches in the
  analysis of diachronic solar observations, that are a must to provide
  comprehensive and homogeneous data sets.

---------------------------------------------------------
Title: Characteristics of EUV Coronal Jets Observed with STEREO/SECCHI
Authors: Nisticò, G.; Bothmer, V.; Patsourakos, S.; Zimbardo, G.
2009SoPh..259...87N    Altcode: 2009arXiv0906.4407N
  In this paper we present the first comprehensive statistical study
  of EUV coronal jets observed with the SECCHI (Sun Earth Connection
  Coronal and Heliospheric Investigation) imaging suites of the two
  STEREO spacecraft. A catalogue of 79 polar jets is presented, identified
  from simultaneous EUV and white-light coronagraph observations, taken
  during the time period March 2007 to April 2008, when solar activity
  was at a minimum. The twin spacecraft angular separation increased
  during this time interval from 2 to 48 degrees. The appearances of
  the coronal jets were always correlated with underlying small-scale
  chromospheric bright points. A basic characterization of the morphology
  and identification of the presence of helical structure were established
  with respect to recently proposed models for their origin and temporal
  evolution. Though each jet appeared morphologically similar in the
  coronagraph field of view, in the sense of a narrow collimated outward
  flow of matter, at the source region in the low corona the jet showed
  different characteristics, which may correspond to different magnetic
  structures. A classification of the events with respect to previous
  jet studies shows that amongst the 79 events there were 37 Eiffel
  tower-type jet events, commonly interpreted as a small-scale (∼35
  arc sec) magnetic bipole reconnecting with the ambient unipolar open
  coronal magnetic fields at its loop tops, and 12 lambda-type jet events
  commonly interpreted as reconnection with the ambient field happening at
  the bipole footpoints. Five events were termed micro-CME-type jet events
  because they resembled the classical coronal mass ejections (CMEs) but
  on much smaller scales. The remaining 25 cases could not be uniquely
  classified. Thirty-one of the total number of events exhibited a helical
  magnetic field structure, indicative for a torsional motion of the jet
  around its axis of propagation. A few jets are also found in equatorial
  coronal holes. In this study we present sample events for each of
  the jet types using both, STEREO A and STEREO B, perspectives. The
  typical lifetimes in the SECCHI/EUVI (Extreme UltraViolet Imager)
  field of view between 1.0 to 1.7 R<SUB>⊙</SUB> and in SECCHI/COR1
  field of view between 1.4 to 4 R<SUB>⊙</SUB> are obtained, and the
  derived speeds are roughly estimated. In summary, the observations
  support the assumption of continuous small-scale reconnection as an
  intrinsic feature of the solar corona, with its role for the heating of
  the corona, particle acceleration, structuring and acceleration of the
  solar wind remaining to be explored in more detail in further studies.

---------------------------------------------------------
Title: Theoretical modeling for the stereo mission
Authors: Aschwanden, Markus J.; Burlaga, L. F.; Kaiser, M. L.; Ng,
   C. K.; Reames, D. V.; Reiner, M. J.; Gombosi, T. I.; Lugaz, N.;
   Manchester, W.; Roussev, I. I.; Zurbuchen, T. H.; Farrugia, C. J.;
   Galvin, A. B.; Lee, M. A.; Linker, J. A.; Mikić, Z.; Riley, P.;
   Alexander, D.; Sandman, A. W.; Cook, J. W.; Howard, R. A.; Odstrčil,
   D.; Pizzo, V. J.; Kóta, J.; Liewer, P. C.; Luhmann, J. G.; Inhester,
   B.; Schwenn, R. W.; Solanki, S. K.; Vasyliunas, V. M.; Wiegelmann, T.;
   Blush, L.; Bochsler, P.; Cairns, I. H.; Robinson, P. A.; Bothmer,
   V.; Kecskemety, K.; Llebaria, A.; Maksimovic, M.; Scholer, M.;
   Wimmer-Schweingruber, R. F.
2008SSRv..136..565A    Altcode: 2006SSRv..tmp...75A
  We summarize the theory and modeling efforts for the STEREO mission,
  which will be used to interpret the data of both the remote-sensing
  (SECCHI, SWAVES) and in-situ instruments (IMPACT, PLASTIC). The
  modeling includes the coronal plasma, in both open and closed magnetic
  structures, and the solar wind and its expansion outwards from the Sun,
  which defines the heliosphere. Particular emphasis is given to modeling
  of dynamic phenomena associated with the initiation and propagation
  of coronal mass ejections (CMEs). The modeling of the CME initiation
  includes magnetic shearing, kink instability, filament eruption, and
  magnetic reconnection in the flaring lower corona. The modeling of CME
  propagation entails interplanetary shocks, interplanetary particle
  beams, solar energetic particles (SEPs), geoeffective connections,
  and space weather. This review describes mostly existing models of
  groups that have committed their work to the STEREO mission, but is by
  no means exhaustive or comprehensive regarding alternative theoretical
  approaches.

---------------------------------------------------------
Title: Sun Earth Connection Coronal and Heliospheric Investigation
    (SECCHI)
Authors: Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.;
   Socker, D. G.; Plunkett, S. P.; Korendyke, C. M.; Cook, J. W.; Hurley,
   A.; Davila, J. M.; Thompson, W. T.; St Cyr, O. C.; Mentzell, E.;
   Mehalick, K.; Lemen, J. R.; Wuelser, J. P.; Duncan, D. W.; Tarbell,
   T. D.; Wolfson, C. J.; Moore, A.; Harrison, R. A.; Waltham, N. R.;
   Lang, J.; Davis, C. J.; Eyles, C. J.; Mapson-Menard, H.; Simnett,
   G. M.; Halain, J. P.; Defise, J. M.; Mazy, E.; Rochus, P.; Mercier,
   R.; Ravet, M. F.; Delmotte, F.; Auchere, F.; Delaboudiniere, J. P.;
   Bothmer, V.; Deutsch, W.; Wang, D.; Rich, N.; Cooper, S.; Stephens,
   V.; Maahs, G.; Baugh, R.; McMullin, D.; Carter, T.
2008SSRv..136...67H    Altcode: 2008SSRv..tmp...64H
  The Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) is a five telescope package, which has been developed for
  the Solar Terrestrial Relation Observatory (STEREO) mission by the
  Naval Research Laboratory (USA), the Lockheed Solar and Astrophysics
  Laboratory (USA), the Goddard Space Flight Center (USA), the University
  of Birmingham (UK), the Rutherford Appleton Laboratory (UK), the
  Max Planck Institute for Solar System Research (Germany), the Centre
  Spatiale de Leige (Belgium), the Institut d’Optique (France) and the
  Institut d’Astrophysique Spatiale (France). SECCHI comprises five
  telescopes, which together image the solar corona from the solar disk to
  beyond 1 AU. These telescopes are: an extreme ultraviolet imager (EUVI:
  1 1.7 R<SUB>⊙</SUB>), two traditional Lyot coronagraphs (COR1: 1.5 4
  R<SUB>⊙</SUB> and COR2: 2.5 15 R<SUB>⊙</SUB>) and two new designs
  of heliospheric imagers (HI-1: 15 84 R<SUB>⊙</SUB> and HI-2: 66 318
  R<SUB>⊙</SUB>). All the instruments use 2048×2048 pixel CCD arrays
  in a backside-in mode. The EUVI backside surface has been specially
  processed for EUV sensitivity, while the others have an anti-reflection
  coating applied. A multi-tasking operating system, running on a PowerPC
  CPU, receives commands from the spacecraft, controls the instrument
  operations, acquires the images and compresses them for downlink
  through the main science channel (at compression factors typically
  up to 20×) and also through a low bandwidth channel to be used for
  space weather forecasting (at compression factors up to 200×). An
  image compression factor of about 10× enable the collection of images
  at the rate of about one every 2 3 minutes. Identical instruments,
  except for different sizes of occulters, are included on the STEREO-A
  and STEREO-B spacecraft.

---------------------------------------------------------
Title: Interplanetary Space Weather and Its Planetary Connection
Authors: Crosby, Norma; Bothmer, Volker; Facius, Rainer; Grießmeier,
   Jean-Mathias; Moussas, Xenophon; Panasyuk, Mikhail; Romanova, Natalia;
   Withers, Paul
2008SpWea...6.1003C    Altcode:
  Interplanetary travel is not just a science fiction scenario anymore,
  but a goal as realistic as when our ancestors started to cross the
  oceans. With curiosity driving humans to visit other planets in our
  solar system, the understanding of interplanetary space weather is
  a vital subject today, particularly because the physical conditions
  faced during a space vehicle's transit to its targeted solar system
  object are crucial to a mission's success and vital to the health
  and safety of spacecraft crew, especially when scheduling planned
  extravehicular activities.

---------------------------------------------------------
Title: The SECCHI Experiment on the STEREO Mission
Authors: Howard, R. A.; Moses, J. D.; Vourlidas, A.; Newmark, J. S.;
   Socker, D. G.; Wang, D.; Plunkett, S. P.; Baugh, R.; McMullin, D. R.;
   Davila, J. M.; Thompson, W. T.; Lemen, J. R.; Wuelser, J.; Harrison,
   R. A.; Waltham, N. R.; Davis, C. J.; Eyles, C. J.; Defise, J.; Halain,
   J.; Bothmer, V.; Delaboudiniere, J.; Auchere, F.; Mercier, R.; Ravet,
   M. F.
2007AGUSMSH33A..01H    Altcode:
  The Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) on the NASA Solar Terrestrial Relations Observatory (STEREO)
  mission is a suite of remote sensing instruments consisting of an
  extreme ultraviolet (EUV) imager, two white light coronagraphs, and
  two telescopes that comprise the heliospheric imager. SECCHI will
  observe coronal mass ejections (CMEs) from their birth at the sun,
  through the corona and into the heliosphere. A complete instrument
  suite is being carried on each of the two STEREO spacecraft, which
  will provide the first sampling of a CME from two vantage points. The
  spacecraft, launched 25 October 2006, are orbiting the Sun, one Ahead
  of the Earth and the other Behind, each separating from Earth at about
  22 degrees per year. The varying separation means that we will have
  different observational capabilities as the spacecraft separate and
  therefore differing science goals. The primary science objectives
  all are focused on understanding the physics of the CME process
  their initiation, 3D morphology, propagation, interaction with the
  interplanetary medium and space weather effects. By observing the CME
  from multiple viewpoints with UV and coronagraphic telescopes and by
  combining these observations with radio and in-situ observations from
  the other instruments on STEREO as well as from other satellites and
  ground based observatories operating at the same time, answers to some
  of the outstanding questions will be obtained. We will show some of
  the initial results.

---------------------------------------------------------
Title: Stereo Observations Of The Solar Corona Using The Secchi
    Experiment
Authors: Plunkett, Simon P.; Howard, R. A.; Moses, J. D.; Vourlidas,
   A.; Socker, D.; Newmark, J.; Wang, D.; Baugh, R.; Davila, J.;
   Thompson, W.; St. Cyr, O. C.; Lemen, J.; Wuelser, J. P.; Harrison,
   R. A.; Waltham, N.; Davis, C. J.; Eyles, C. J.; Defise, J. M.; Halain,
   J. P.; Bothmer, V.; Delaboudiniere, J. P.; Auchere, F.; Mercier, R.;
   Ravet, M. F.
2007AAS...21011901P    Altcode: 2007BAAS...39..243P
  The Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) on the NASA Solar Terrestrial Relations Observatory (STEREO)
  mission is a suite of remote sensing instruments consisting of an
  extreme ultraviolet (EUV) imager, two white light coronagraphs,
  and two telescopes that comprise the heliospheric imager. The main
  objective of SECCHI is to observe coronal mass ejections (CMEs) from
  their birth at the sun, through the corona and into the heliosphere. A
  complete instrument suite is being carried on each of the two STEREO
  spacecraft, which will provide the first sampling of a CME from two
  vantage points as the spacecraft separate from each other at the rate
  of about 45 degrees per year. We will show examples of some of the
  data and some of the initial stereo results.

---------------------------------------------------------
Title: Understanding coronal heating and solar wind acceleration:
    Case for in situ near-Sun measurements
Authors: McComas, D. J.; Velli, M.; Lewis, W. S.; Acton, L. W.;
   Balat-Pichelin, M.; Bothmer, V.; Dirling, R. B.; Feldman, W. C.;
   Gloeckler, G.; Habbal, S. R.; Hassler, D. M.; Mann, I.; Matthaeus,
   W. H.; McNutt, R. L.; Mewaldt, R. A.; Murphy, N.; Ofman, L.; Sittler,
   E. C.; Smith, C. W.; Zurbuchen, T. H.
2007RvGeo..45.1004M    Altcode:
  The solar wind has been measured directly from 0.3 AU outward,
  and the Sun's atmosphere has been imaged from the photosphere out
  through the corona. These observations have significantly advanced our
  understanding of the influence of the Sun's varying magnetic field on
  the structure and dynamics of the corona and the solar wind. However,
  how the corona is heated and accelerated to produce the solar wind
  remains a mystery. Answering these fundamental questions requires
  in situ observations near the Sun, from a few solar radii (R <SUB> S
  </SUB>) out to ~20 R <SUB> S </SUB>, where the internal, magnetic, and
  turbulent energy in the coronal plasma is channeled into the bulk energy
  of the supersonic solar wind. A mission to make such observations has
  long been a top priority of the solar and space physics community. The
  recent Solar Probe study has proven that such a mission is technically
  feasible and can be accomplished within reasonable resources.

---------------------------------------------------------
Title: Evolution of the photospheric magnetic field in the source
    regions of coronal mass ejections
Authors: Bothmer, V.; Tripathi, D.
2007msfa.conf..257B    Altcode:
  Six coronal mass ejections associated with erupting quiescent filaments
  on the visible solar disk were identified in data from SoHO (Solar
  and Heliospheric Observatory) LASCO (Large Angle and Spectrometric
  Coronagraph), EIT (Extreme ultraviolet Imaging Telescope) and MDI
  (Michelson Doppler Imager) data and ground-based Hα observations
  from Big Bear and Meudon observatories. These events were analysed to
  investigate whether their initiations could be related to changes of
  the underlying photospheric field. The results show that in five out
  of the six events, substantial changes in the photospheric magnetic
  field occurred in the source regions prior and around the CME's lift-off
  times as identified from emerging/diminishing flux detected by MDI. In
  one event large magnetic flux changes could be identified not in the
  source region itself, but in a neighbouring active region. The results
  demonstrate that new missions, such as STEREO and Hinode (Solar-B)
  in conjunction with SoHO and ground-based measurements, will provide
  joint data sets that have the potential to provide new insight into
  the physical causes of CMEs.

---------------------------------------------------------
Title: The SECCHI Experiment on the STEREO Mission
Authors: Howard, R. A.; Moses, D.; Vourlidas, A.; Newmark, J.; Socker,
   D. G.; Plunkett, S.; Wang, D.; Baugh, R.; McMullin, D.; Davila, J.;
   St. Cyr, C.; Thompson, W. T.; Lemen, J.; Wuelser, J.; Harrison, R. A.;
   Waltham, N. R.; Davis, C.; Eyles, C. J.; Defise, J.; Halain, J.;
   Bothmer, V.; Delaboudiniere, J.; Auchere, F.; Mercier, R.; Ravet, M.
2006AGUFMSM12A..02H    Altcode:
  The Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI) on the NASA Solar Terrestrial Relations Observatory (STEREO)
  mission is a suite of remote sensing instruments consisting of an
  extreme ultraviolet (EUV) imager, two white light coronagraphs, and
  two telescopes that comprise the heliospheric imager. SECCHI will
  observe coronal mass ejections (CMEs) from their birth at the sun,
  through the corona and into the heliosphere. A complete instrument
  suite is being carried on each of the two STEREO spacecraft, which
  will provide the first sampling of a CME from two vantage points. The
  spacecraft will orbit the Sun, one Ahead of the Earth and the other
  Behind, each separating from Earth at about 22 degrees per year. The
  varying separation means that we will have different observational
  capabilities as the spacecraft separate and therefore differing science
  goals. The primary science objectives all are focused on understanding
  the physics of the CME process their initiation, 3D morphology,
  propagation, interaction with the interplanetary medium and space
  weather effects. By observing the CME from multiple viewpoints with UV
  and coronagraphic telescopes and by combining these observations with
  radio and in-situ observations from the other instruments on STEREO as
  well as from other satellites and ground based observatories operating
  at the same time, answers to some of the outstanding questions will
  be obtained. STEREO follows the very successful SOHO mission. SOHO's
  success was primarily due to the highly complementary nature of the
  instruments, but it was partly due to the very stable platform. The
  L1 orbit enables an extremely stable thermal environment and thus
  very stable pointing, as well as uninterrupted solar viewing. The
  STEREO will have both of these characteristics, but in addition will
  have multi-viewpoint viewing of CMEs, which will greatly enhance the
  many discoveries that SOHO data have produced. We have been developing
  techniques to interpret the observations from multiple viewpoints and
  to perform 3-dimensional deconvolution of the CME observations using
  forward modeling and inversion techniques. A continuous downlink of
  STEREO data will provide a low-resolution, real- time view from all
  of the instruments. The full data are downlinked once a day and will
  be available about 24 hours later. We will present some preliminary
  results from the instrument, which is expected to be launched in
  October/November, 2006

---------------------------------------------------------
Title: Photospheric Field Evolution in the Source Regions of Coronal
    Mass Ejections
Authors: Bothmer, V.; Tripathi, D.
2006ESASP.617E..20B    Altcode: 2006soho...17E..20B
  No abstract at ADS

---------------------------------------------------------
Title: Observation of a bright coronal downflow by SOHO/EIT
Authors: Tripathi, D.; Solanki, S. K.; Schwenn, R.; Bothmer, V.;
   Mierla, M.; Stenborg, G.
2006A&A...449..369T    Altcode:
  A distinct coronal downflow has been discovered in the course of a
  prominence eruption associated coronal mass ejection (CME) imaged by
  EIT (Extreme ultraviolet Imaging Telescope) and LASCO (Large Angle
  Spectrometric Coronagraph) on board SOHO (Solar and Heliospheric
  Observatory) on 5-Mar.-2000. Evolution of the prominences seen by EIT
  was tracked into the LASCO/C2 and C3 field-of-view where they developed
  as the core of a typical three-part CME. In contrast to the inflow
  structures reported earlier in the literatures, which were dark and
  were interpreted as plasma voids moving down, the downflow reported
  here was bright. The downflow, which was only seen in EIT FOV had an
  onset time that coincided with the deceleration phase of the core
  of the CME. The downflow showed a rapid acceleration followed by a
  strong deceleration. The downflow followed a curved path which may be
  explained by material following the apex of a contracting magnetic loop
  sliding down along other field lines, although other explanations are
  also possible. Irrespective of the detailed geometry, this observation
  provides support for the pinching off of the field lines drawn-out by
  the erupting prominences and the contraction of the arcade formed by
  the reconnection.

---------------------------------------------------------
Title: Understanding Interplanetary Coronal Mass Ejection Signatures.
    Report of Working Group B
Authors: Wimmer-Schweingruber, R. F.; Crooker, N. U.; Balogh, A.;
   Bothmer, V.; Forsyth, R. J.; Gazis, P.; Gosling, J. T.; Horbury, T.;
   Kilchenmann, A.; Richardson, I. G.; Richardson, J. D.; Riley, P.;
   Rodriguez, L.; von Steiger, R.; Wurz, P.; Zurbuchen, T. H.
2006SSRv..123..177W    Altcode: 2006SSRv..tmp...66W
  While interplanetary coronal mass ejections (ICMEs) are understood to
  be the heliospheric counterparts of CMEs, with signatures undeniably
  linked to the CME process, the variability of these signatures and
  questions about mapping to observed CME features raise issues that
  remain on the cutting edge of ICME research. These issues are discussed
  in the context of traditional understanding, and recent results using
  innovative analysis techniques are reviewed.

---------------------------------------------------------
Title: ICMEs in the Inner Heliosphere: Origin, Evolution and
    Propagation Effects.  Report of Working Group G
Authors: Forsyth, R. J.; Bothmer, V.; Cid, C.; Crooker, N. U.; Horbury,
   T. S.; Kecskemety, K.; Klecker, B.; Linker, J. A.; Odstrcil, D.;
   Reiner, M. J.; Richardson, I. G.; Rodriguez-Pacheco, J.; Schmidt,
   J. M.; Wimmer-Schweingruber, R. F.
2006SSRv..123..383F    Altcode: 2006SSRv..tmp...69F
  This report assesses the current status of research relating the origin
  at the Sun, the evolution through the inner heliosphere and the effects
  on the inner heliosphere of the interplanetary counterparts of coronal
  mass ejections (ICMEs). The signatures of ICMEs measured by in-situ
  spacecraft are determined both by the physical processes associated
  with their origin in the low corona, as observed by space-borne
  coronagraphs, and by the physical processes occurring as the ICMEs
  propagate out through the inner heliosphere, interacting with the
  ambient solar wind. The solar and in-situ observations are discussed
  as are efforts to model the evolution of ICMEs from the Sun out to 1 AU.

---------------------------------------------------------
Title: The SECCHI Experiment on the STEREO Mission
Authors: Howard, R.; Moses, D.; Vourlidas, A.; Davila, J.; Lemen, J.;
   Harrison, R.; Eyles, C.; Defise, J. -M.; Bothmer, V.; Ravet, M. -F.;
   Secchi Team
2006cosp...36..870H    Altcode: 2006cosp.meet..870H
  The Sun Earth Connection Coronal and Heliospheric Investigation SECCHI
  on the NASA Solar Terrestrial Relations Observatory STEREO mission
  is a suite of remote sensing instruments consisting of an extreme
  ultraviolet EUV imager two white light coronagraphs and two telescopes
  that comprise the heliospheric imager SECCHI will observe coronal mass
  ejections CMEs from their birth at the sun through the corona and into
  the heliosphere A complete instrument suite is being carried on each
  of the two STEREO spacecraft which will provide the first sampling of
  a CME from two vantage points The spacecraft will orbit the Sun one
  Ahead of the Earth and the other Behind each separating from Earth at
  about 22 degrees per year The varying separation means that we will
  have different observational capabilities as the spacecraft separate
  and therefore differing science goals The primary science objectives
  all are focused on understanding the physics of the CME process -
  their initiation 3D morphology propagation interaction with the
  interplanetary medium and space weather effects By observing the CME
  from multiple viewpoints with UV and coronagraphic telescopes and by
  combining these observations with radio and in-situ observations from
  the other instruments on STEREO as well as from other satellites and
  ground based observatories operating at the same time answers to some
  of the outstanding questions will be obtained STEREO follows the very
  successful SOHO mission SOHO s success was primarily due to the highly
  complementary nature of the instruments but it was

---------------------------------------------------------
Title: Properties of structured coronal mass ejections in solar
    cycle 23
Authors: Cremades, H.; Bothmer, V.; Tripathi, D.
2006AdSpR..38..461C    Altcode:
  The Solar and Heliospheric Observatory has provided to date doubtlessly
  the best dataset of coronal observations ever taken over the course
  of a solar cycle. Structured coronal mass ejections, i.e. events
  with clear white-light fine structures, have been selected from the
  dataset of the large angle spectroscopic coronagraph during the period
  1996 2002. Their source regions in the low corona and photosphere
  have been deduced by analyzing data from the Extreme-ultraviolet
  Imaging Telescope and Michelson Doppler Imager onboard the Solar and
  Heliospheric Observatory and from ground-based Hα measurements. Based
  on this subset of coronal mass ejections, originally compiled to study
  their three-dimensional configuration, we have analyzed the variation
  of their properties during the present solar cycle. These properties
  include latitude and tilt angle of source regions of coronal mass
  ejections, position angle of coronal mass ejections, and deviation
  of coronal mass ejections with respect to their corresponding source
  regions. The results show a pronounced and systematic confinement of
  position angles at equatorial latitudes and equatorward deviations
  during low solar activity. In contrast, fluctuating position angles
  and deviations in all directions were found at times of high solar
  activity. A method to explain the observed deflections is presented.

---------------------------------------------------------
Title: Solar Activity and its Magnetic Origin
Authors: Bothmer, Volker; Hady, Ahmed Abdel
2006IAUS..233.....B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Activity and its Magnetic Origin
Authors: Bothmer, Volker; Hady, Ahmed Abdel
2006IAUS..233....7B    Altcode:
  The variability of the Sun's magnetic field is the main driver of
  solar activity. IAU S233 was held to further our understanding about
  solar magnetic processes and also its interplanetary consequences. The
  Symposium was organized into seven sessions covering: the generation
  and transport of solar magnetic fields; magnetic fields and coupling
  processes in the solar atmosphere; coronal heating and small-scale
  dynamics; large-scale coronal structure; the origin and evolution of
  the solar wind; flares, CMEs and SEPs; and new instrumentation and
  missions. Each session included contributions by leading scientists
  in the form of tutorials, research reviews and presentations of the
  latest results. A special eighth session was dedicated to educating
  young national and international astronomers. <P />With reviews and
  research contributions covering a broad range of disciplines in solar
  and heliospheric research, this volume is a valuable interdisciplinary
  resource for professional astronomers and graduate students.

---------------------------------------------------------
Title: Understanding Interplanetary Coronal Mass Ejection Signatures
Authors: Wimmer-Schweingruber, R. F.; Crooker, N. U.; Balogh, A.;
   Bothmer, V.; Forsyth, R. J.; Gazis, P.; Gosling, J. T.; Horbury, T.;
   Kilchenmann, A.; Richardson, I. G.; Richardson, J. D.; Riley, P.;
   Rodriguez, L.; von Steiger, R.; Wurz, P.; Zurbuchen, T. H.
2006cme..book..177W    Altcode:
  While interplanetary coronal mass ejections (ICMEs) are understood to
  be the heliospheric counterparts of CMEs, with signatures undeniably
  linked to the CME process, the variability of these signatures and
  questions about mapping to observed CME features raise issues that
  remain on the cutting edge of ICME research. These issues are discussed
  in the context of traditional understanding, and recent results using
  innovative analysis techniques are reviewed.

---------------------------------------------------------
Title: ICMEs in the Inner Heliosphere: Origin, Evolution and
    Propagation Effects
Authors: Forsyth, R. J.; Bothmer, V.; Cid, C.; Crooker, N. U.; Horbury,
   T. S.; Kecskemety, K.; Klecker, B.; Linker, J. A.; Odstrcil, D.;
   Reiner, M. J.; Richardson, I. G.; Rodriguez-Pacheco, J.; Schmidt,
   J. M.; Wimmer-Schweingruber, R. F.
2006cme..book..383F    Altcode:
  This report assesses the current status of research relating the origin
  at the Sun, the evolution through the inner heliosphere and the effects
  on the inner heliosphere of the interplanetary counterparts of coronal
  mass ejections (ICMEs). The signatures of ICMEs measured by in-situ
  spacecraft are determined both by the physical processes associated
  with their origin in the low corona, as observed by space-borne
  coronagraphs, and by the physical processes occurring as the ICMEs
  propagate out through the inner heliosphere, interacting with the
  ambient solar wind. The solar and in-situ observations are discussed
  as are efforts to model the evolution of ICMEs from the Sun out to 1 AU.

---------------------------------------------------------
Title: The Solar Atmosphere and Space Weather
Authors: Bothmer, Volker
2006ssu..book....1B    Altcode:
  First ideas about possible physical influences of the Sun on Earth other
  than by electromagnetic (EM) radiation were scientifically discussed
  more seriously after Richard Carrington's famous observation of a
  spectacular white-light flare in 1859 and the subsequent conclusion
  that this flash of EM radiation was connected with the origin of
  strong perturbations of the Earth's outer magnetic field, commonly
  referred to as geomagnetic storms, which were recorded about 24 hours
  after the solar flare. Tentatively significant correlations of the
  number of geomagnetic storms and aurorae with the varying number of
  sunspots seen on the visible solar disk were found in the long-term
  with respect to the roughly 11-year periodicity of the solar activity
  cycle. Although theories of sporadic solar eruptions were postulated
  soon after the Carrington observations, the physical mechanism of the
  transfer of energy from the Sun to the Earth remained unknown. Early
  in the 20<SUP>th</SUP> century Chapman and Ferraro proposed the
  concept of huge clouds of charged particles emitted by the Sun as
  the triggers of geomagnetic storms. Based on the inference of the
  existence of a solar magnetic field, magnetized plasma clouds were
  subsequently introduced. Eugene Parker derived theoretical evidence for
  a continuous stream of ionized particles, the solar wind, leading to
  continuous convection of the Sun's magnetic field into interplanetary
  space. The existence of the solar wind was confirmed soon after the
  launch of the first satellites. Since then the Sun is known to be a
  permanent source of particles filling interplanetary space. However,
  it was still thought that the Sun's outer atmosphere, the solar corona,
  is a static rather than a dynamic object, undergoing only long-term
  structural changes in phase with the Sun's activity cycle. This view
  completely changed after space borne telescopes provided extended series
  of solar images in the EUV and soft X-ray range of the EM spectrum,
  invisible to ground-based observers. The remote-sensing observations
  undertaken by Yohkoh, followed by multi-wavelength movies from SoHO
  (Solar Heliospheric Observatory) and high resolution EUV imaging by
  TRACE (Transition Region and Coronal Explorer) have revealed to date
  that the Sun's atmosphere is highly dynamic and never at rest. Solar
  eruptions have been tracked into space in unprecedented detail. In
  combination with near-Earth satellites, their interplanetary and
  geo-space effects could be investigated in depth, having provided
  the roots for space weather forecasts. This chapter summarizes the
  discoveries about the origin and evolution of solar storms and their
  space weather effects, providing a comprehensive picture of the most
  important links in the Sun-Earth system. It finally provides an outlook
  to future research in the field of space weather.

---------------------------------------------------------
Title: Solar Probe: Humanity's First Visit to a Star (Invited)
Authors: McComas, D. J.; Velli, M.; Lewis, W. S.; Acton, L. W.;
   Balat-Pichelin, M.; Bothmer, V.; Dirling, R. B.; Eng, D. A.; Feldman,
   W. C.; Gloeckler, G.; Guhathakurtha, M.; Habbal, S. R.; Hassler, D. M.;
   Mann, I.; Maldonado, H. M.; Matthaeus, W. H.; McNutt, R. L.; Mewaldt,
   R. A.; Murphy, N.; Ofman, L.; Potocki, K. A.; Sittler, E. C.; Smith,
   C. W.; Zurbuchen, T. H.
2005ESASP.592..279M    Altcode: 2005ESASP.592E..42M; 2005soho...16E..42M
  No abstract at ADS

---------------------------------------------------------
Title: Properties and geoeffectiveness of magnetic clouds in the
    rising, maximum and early declining phases of solar cycle 23
Authors: Huttunen, K. E. J.; Schwenn, R.; Bothmer, V.; Koskinen,
   H. E. J.
2005AnGeo..23..625H    Altcode:
  The magnetic structure and geomagnetic response of 73 magnetic clouds
  (MC) observed by the WIND and ACE satellites in solar cycle 23 are
  examined. The results have been compared with the surveys from the
  previous solar cycles. The preselected candidate MC events were
  investigated using the minimum variance analysis to determine if
  they have a flux-rope structure and to obtain the estimation for the
  axial orientation (θC, φC). Depending on the calculated inclination
  relative to the ecliptic we divided MCs into "bipolar" (θC&lt;45°)
  and "unipolar" (θC&gt;45°). The number of observed MCs was largest in
  the early rising phase, although the halo CME rate was still low. It
  is likely that near solar maximum we did not identify all MCs at 1AU,
  as they were crossed far from the axis or they had interacted strongly
  with the ambient solar wind or with other CMEs. The occurrence rate of
  MCs at 1AU is also modified by the migration of the filament sites on
  the Sun towards the poles near solar maximum and by the deflection of
  CMEs towards the equator due to the fast solar wind flow from large
  polar coronal holes near solar minimum. In the rising phase nearly
  all bipolar MCs were associated with the rotation of the magnetic
  field from the south at the leading edge to the north at the trailing
  edge. The results for solar cycles 21-22 showed that the direction
  of the magnetic field in the leading portion of the MC starts to
  reverse at solar maximum. At solar maximum and in the declining
  phase (2000-2003) we observed several MCs with the rotation from
  the north to the south. We observed unipolar (i.e. highly inclined)
  MCs frequently during the whole investigated period. For solar cycles
  21-22 the majority of MCs identified in the rising phase were bipolar
  while in the declining phase most MCs were unipolar. The geomagnetic
  response of a given MC depends greatly on its magnetic structure and the
  orientation of the sheath fields. For each event we distinguished the
  effect of the sheath fields and the MC fields. All unipolar MCs with
  magnetic field southward at the axis were geoeffective (Dst&lt;-50nT)
  while those with the field pointing northward did not cause magnetic
  storms at all. About half of the all identified MCs were not geoffective
  or the sheath fields preceding the MC caused the storm. MCs caused
  more intense magnetic storms (Dst&lt;-100nT) than moderate magnetic
  storms (-50nT ≥Dst≥-100nT). &lt;p style="line-height: 20px;"&gt;
  &lt;/td&gt; &lt;/tr&gt;

---------------------------------------------------------
Title: SoHO/EIT Observation of a Coronal Inflow
Authors: Tripathi, D.; Bothmer, V.; Solanki, S. K.; Schwenn, R.;
   Mierla, M.; Stenborg, G.
2005IAUS..226..133T    Altcode:
  A distinct coronal inflow has been discovered after ∼90 min
  of prominence eruption associated coronal mass ejection (CME) on
  05-Mar-2000 by EIT (Extreme ultraviolet Imaging Telescope) aboard SoHO
  (Solar and Heliospheric Observatory). Evolution of the prominence seen
  by EIT was tracked into the LASCO/C2 and C3 field-of-view (FOV; 4-10
  R<SUB>⊙</SUB>) where it developed as the core of a typical three-part
  CME. The speed of the inflow, which was only seen in EIT FOV, was 70-80
  km/s at a height between 1.5-1.2 R<SUB>⊙</SUB> coinciding with the
  deceleration phase of the core of the CME in LASCO/C2. In contrast to
  dark inflow structures observed earlier and interpreted as plasma void
  moving down, the inflow reported here was bright. The inflow showed a
  constant deceleration and followed a curved path suggesting the apex
  of a contracting magnetic loop sliding down along other field lines.

---------------------------------------------------------
Title: Solar Cycle Variation of the Internal Magnetic Field Structure
    of CMEs
Authors: Bothmer, Volker
2005IAUS..226..208B    Altcode:
  The internal magnetic field structure of CMEs and the field structure
  of the solar source regions were systematically investigated during
  different phases of the solar cycle in cycles 19-23 based on plasma
  and magnetic field measurements sampled by various satellites and
  through multi-wavelength remote sensing observations. It is found that:
  1. To first order, the internal magnetic structure of CMEs varies
  systematically from one solar cycle to the next with respect to the
  prevailing hemispheric magnetic patterns of bipolar regions following
  the law of hemispheric helicity dependence. 2. To second order, the
  field structure in CMEs varies with respect to the complex spatial
  evolution of the magnetic flux in the photosphere in both hemispheres
  over the course of the cycle itself. The two effects can naturally
  explain the cyclic behavior of the SN, NS variations of the internal
  magnetic fields in CMEs in the solar wind as well as intermittent
  periods of mixed distributions.

---------------------------------------------------------
Title: Solar origins of intense geomagnetic storms in 2002 as seen
    by the CORONAS-F satellite
Authors: Panasenco, O.; Veselovsky, I. S.; Dmitriev, A. V.; Zhukov,
   A. N.; Yakovchouk, O. S.; Zhitnik, I. A.; Ignat'ev, A. P.; Kuzin,
   S. V.; Pertsov, A. A.; Slemzin, V. A.; Boldyrev, S. I.; Romashets,
   E. P.; Stepanov, A.; Bugaenco, O. I.; Bothmer, V.; Koutchmy, S.;
   Adjabshirizadeh, A.; Fazel, Z.; Sobhanian, S.
2005AdSpR..36.1595P    Altcode:
  We analyze solar origins of intense geomagnetic perturbations recorded
  during 2002. All of them were related to coronal mass ejections
  (CMEs). The initiation of CMEs was documented using the SPIRIT
  instrument (SPectrohelIographic Soft X-Ray Imaging Telescope) onboard
  the CORONAS-F satellite. Monochromatic full Sun images taken in the Mg
  XII doublet at 8.418 and 8.423 Å showed the appearance of free energy
  release sites at altitudes up to 0.4 solar radii. CMEs were initiated
  at these sites and propagated in interplanetary space under appropriate
  local conditions including the geometry of the magnetic fields.

---------------------------------------------------------
Title: Magnetic storm cessation during sustained northward IMF
Authors: Veselovsky, I. S.; Bothmer, V.; Cargill, P.; Dmitriev, A. V.;
   Ivanov, K. G.; Romashets, E.; Zhukov, A. N.; Yakovchouk, O. S.
2005AdSpR..36.2460V    Altcode:
  Times of sustained strong northward IMF can interrupt the magnetic
  storm development and lead to lower levels of geomagnetic activity
  for many hours. During 1997-2000 we have found two events of this
  kind observed on November 8, 1998 and October 13, 2000. In both
  cases, the storms started as usual after arrival of ejecta with a
  southward IMF component from the Sun to the Earth, but ceased after
  several hours due to the onset of sustained northward IMF leading
  to the faster recovery process. After the passage of this so-called
  positive domain, the storm development started again. The heliospheric
  magnetic field intensity remained enhanced and nearly constant. The
  solar origins of the geomagnetic storm interruptions have been
  investigated. Tentatively they may be related to strong nonlinear
  Alfvйn type solitary waves excited by non-stationary coronal current
  variations with a characteristic time-scale of about a day.

---------------------------------------------------------
Title: Geometrical Properties of Coronal Mass Ejections
Authors: Cremades, Hebe; Bothmer, Volker
2005IAUS..226...48C    Altcode:
  Based on the SOHO/LASCO dataset, a collection of "structured" coronal
  mass ejections (CMEs) has been compiled within the period 1996-2002,
  in order to analyze their three-dimensional configuration. These CME
  events exhibit white-light fine structures, likely indicative of their
  possible 3D topology. From a detailed investigation of the associated
  low coronal and photospheric source regions, a generic scheme has been
  deduced, which considers the white-light topology of a CME projected
  in the plane of the sky as being primarily dependent on the orientation
  and position of the source region's neutral line on the solar disk. The
  obtained results imply that structured CMEs are essentially organized
  along a symmetry axis, in a cylindrical manner. The measured dimensions
  of the cylinder's base and length yield a ratio of 1.6. These CMEs
  seem to be better approximated by elliptic cones, rather than by the
  classical ice cream cone, characterized by a circular cross section.

---------------------------------------------------------
Title: IMPACT: Science goals and firsts with STEREO
Authors: Luhmann, J. G.; Curtis, D. W.; Lin, R. P.; Larson, D.;
   Schroeder, P.; Cummings, A.; Mewaldt, R. A.; Stone, E. C.; Davis, A.;
   von Rosenvinge, T.; Acuna, M. H.; Reames, D.; Ng, C.; Ogilvie, K.;
   Mueller-Mellin, R.; Kunow, H.; Mason, G. M.; Wiedenbeck, M.; Sauvaud,
   A.; Aoustin, C.; Louarn, P.; Dandouras, J.; Korth, A.; Bothmer, V.;
   Vasyliunas, V.; Sanderson, T.; Marsden, R. G.; Russell, C. T.; Gosling,
   J. T.; Bougeret, J. L.; McComas, D. J.; Linker, J. A.; Riley, P.;
   Odstrcil, D.; Pizzo, V. J.; Gombosi, T.; DeZeeuw, D.; Kecskemety, K.
2005AdSpR..36.1534L    Altcode:
  The in situ measurements of particles and CME transients (IMPACT)
  investigation on the twin STEREO spacecraft focuses on the solar
  energetic particle, solar wind and suprathermal electron, and magnetic
  field measurements needed to address STEREO's goals. IMPACT will provide
  regular, identical, in situ multipoint measurements bracketing Earth
  as each spacecraft separates from it at a rate of ∼22°/yr along
  Earth's orbit. Combined with the PLASTIC and SWAVES investigations,
  IMPACT fills a critical role in the STEREO quest to connect SECCHI's
  3D coronal images to their interplanetary consequences.

---------------------------------------------------------
Title: Morphology Indicators of the Three-Dimensional Size of Flux
Rope CMEs: A Prediction for STEREO
Authors: St. Cyr, O. C.; Cremades, H.; Bothmer, V.; Krall, J.;
   Burkepile, J. T.
2004AGUFMSH22A..04S    Altcode:
  We provide a new estimate of the three-dimensional sizes of flux
  rope coronal mass ejections (CMEs). We base our estimate on the
  interpretation of two CME morphologies that have previously been
  considered distinct. We believe these morphologies represent two
  perspectives of the same large scale cylindrical structure (a magnetic
  flux rope) seen axially versus broadside. This distinction has not been
  previously recognized because both morphologies have been classified
  as "three-part structures". Our preliminary study based on 21 events
  (13 axial and 8 broadside) indicated an average diameter of 46° and
  an average length of 76° for these flux rope CMEs. We compare our
  statistical results to those obtained using an elliptical flux rope
  model, and we present the current status of this work-in-progress. This
  result will be tested in the future by observations of individual CMEs
  from different locations by NASA's STEREO mission.

---------------------------------------------------------
Title: Solar and Heliospheric Phenomena in October-November 2003:
    Causes and Effects
Authors: Veselovsky, I. S.; Panasyuk, M. I.; Avdyushin, S. I.;
   Bazilevskaya, G. A.; Belov, A. V.; Bogachev, S. A.; Bogod, V. M.;
   Bogomolov, A. V.; Bothmer, V.; Boyarchuk, K. A.; Vashenyuk, E. V.;
   Vlasov, V. I.; Gnezdilov, A. A.; Gorgutsa, R. V.; Grechnev,
   V. V.; Denisov, Yu. I.; Dmitriev, A. V.; Dryer, M.; Yermolaev,
   Yu. I.; Eroshenko, E. A.; Zherebtsov, G. A.; Zhitnik, I. A.;
   Zhukov, A. N.; Zastenker, G. N.; Zelenyi, L. M.; Zeldovich,
   M. A.; Ivanov-Kholodnyi, G. S.; Ignat'ev, A. P.; Ishkov, V. N.;
   Kolomiytsev, O. P.; Krasheninnikov, I. A.; Kudela, K.; Kuzhevsky,
   B. M.; Kuzin, S. V.; Kuznetsov, V. D.; Kuznetsov, S. N.; Kurt, V. G.;
   Lazutin, L. L.; Leshchenko, L. N.; Litvak, M. L.; Logachev, Yu. I.;
   Lawrence, G.; Markeev, A. K.; Makhmutov, V. S.; Mitrofanov, A. V.;
   Mitrofanov, I. G.; Morozov, O. V.; Myagkova, I. N.; Nusinov, A. A.;
   Oparin, S. N.; Panasenco, O. A.; Pertsov, A. A.; Petrukovich, A. A.;
   Podorol'sky, A. N.; Romashets, E. P.; Svertilov, S. I.; Svidsky, P. M.;
   Svirzhevskaya, A. K.; Svirzhevsky, N. S.; Slemzin, V. A.; Smith, Z.;
   Sobel'man, I. I.; Sobolev, D. E.; Stozhkov, Yu. I.; Suvorova, A. V.;
   Sukhodrev, N. K.; Tindo, I. P.; Tokhchukova, S. Kh.; Fomichev, V. V.;
   Chashey, I. V.; Chertok, I. M.; Shishov, V. I.; Yushkov, B. Yu.;
   Yakovchouk, O. S.; Yanke, V. G.
2004CosRe..42..435V    Altcode:
  We present new observational data on the phenomena of extremely
  high activity on the Sun and in the heliosphere that took place
  in October-November 2003. A large variety of solar and heliospheric
  parameters give evidence that the interval under consideration is unique
  over the entire observation time. Based on these data, comparing them
  with similar situations in the past and using available theoretical
  concepts, we discuss possible cause-and-effect connections between
  the processes observed. The paper includes the first results and
  conclusions derived by the collaboration “Solar Extreme Events-2003”
  organized in Russia for detailed investigations of these events. As a
  result of our consideration, it is beyond question that the physical
  causes of solar and heliospheric phenomena in October-November 2003
  are not exclusively local and do not belong only to the active regions
  and solar atmosphere above them. The energy reservoirs and driving
  forces of these processes have a more global nature. In general, they
  are hidden from an observer, since ultimately their sources lie in
  the subphotospheric layers of the Sun, where changes that are fast
  and difficult to predict can sometimes take place (and indeed they
  do). Solar flares can serve as sufficiently good tracers of these sudden
  changes and reconstructions on the Sun, although one can still find
  other diagnostic indicators among the parameters of magnetic fields,
  motions of matter, and emission characteristics.

---------------------------------------------------------
Title: The Solar and Interplanetary Causes of Space Storms in Solar
    Cycle 23
Authors: Bothmer, V.
2004ITPS...32.1411B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the three-dimensional configuration of coronal mass
    ejections
Authors: Cremades, H.; Bothmer, V.
2004A&A...422..307C    Altcode:
  Coronal mass ejections (CMEs) are a direct consequence of the dynamic
  nature of the solar atmosphere. They represent fundamental processes
  in which energy is transferred from the Sun into interplanetary
  space, including geospace. Their origin, 3D structure and internal
  magnetic field configuration are to date not well understood. The SOHO
  spacecraft, launched by the end of 1995, has provided unprecedented
  data on CMEs since instruments switched on in 1996. From a detailed
  investigation of the full set of LASCO (Large Angle Spectroscopic
  Coronagraph) observations from 1996 to the end of 2002, a set of
  structured CME events has been identified, which exhibits white-light
  fine structures likely indicative of their internal magnetic field
  configuration and possible 3D structure. Their source regions in the
  low corona and photosphere have been inferred by means of complementary
  analyses of data from the Extreme-Ultraviolet Imaging Telescope (EIT)
  and Michelson Doppler Imager (MDI) on board SOHO, and ground-based
  Hα measurements. According to the results of this study, structured
  CMEs arise in a self-similar manner from pre-existing small scale
  loop systems, overlying regions of opposite magnetic polarities. From
  the characteristic pattern of the CMEs' source regions in both solar
  hemispheres, a generic scheme is presented in which the projected
  white-light topology of a CME depends primarily on the orientation and
  position of the source region's neutral line on the solar disk. The
  paper also provides information about the white-light characteristics
  of the analysed CMEs, such as angular width and position angle,
  with respect to their source region properties, such as heliographic
  location, inclination and length, including the frequency and variation
  of these parameters over the investigated time period.

---------------------------------------------------------
Title: The basic characteristics of EUV post-eruptive arcades and
    their role as tracers of coronal mass ejection source regions
Authors: Tripathi, D.; Bothmer, V.; Cremades, H.
2004A&A...422..337T    Altcode:
  The Extreme ultraviolet Imaging Telescope (EIT) on board the Solar and
  Heliospheric Observatory (SOHO) spacecraft provides unique observations
  of dynamic processes in the low corona. The EIT 195 Å data taken from
  1997 to the end of 2002 were investigated to study the basic physical
  properties of post-eruptive arcades (PEAs) and their relationship with
  coronal mass ejections (CMEs) as detected by SOHO/LASCO (Large Angle
  Spectrometric Coronagraph). Over the investigated time period, 236 PEA
  events have been identified in total. For each PEA, its EUV lifetime
  as derived from the emission time at 195 Å, its heliographic position
  and length, and its corresponding photospheric source region inferred
  from SOHO/MDI (Michelson Doppler Imager) data has been studied, as well
  as the variation of these parameters over the investigated phase of
  solar cycle 23. An almost one to one correspondence is found between
  EUV PEAs and white-light CMEs. Based on this finding, PEAs can be
  considered as reliable tracers of CME events even without simultaneous
  coronagraph observations. A detailed comparison of the white-light,
  soft X-ray and EUV observation for some of the events shows, that PEAs
  form in the aftermath of CMEs likely in the course of the magnetic
  restructurings taking place at the coronal source sites. The average
  EUV emission life-time for the selected events ranged from 2 to 20
  h, with an average of 7 h. The heliographic length of the PEAs was
  in the range of 2 to 40 degrees, with an average of 15 degrees. The
  length increased by a factor of 3 to 4 in the latitude range of 20
  to 40 degrees in the northern and southern hemispheres, with longer
  PEAs being observed preferentially at higher latitudes. The PEAs were
  located mainly in the activity belts in both hemispheres, with the
  southern hemispheric ones being shifted by about 15 degree in latitude
  further away from the solar equator during 1997-2002. The decrease
  in latitude of the PEA positions was 10 to 15 degrees in the northern
  and southern hemispheres over this period. The axes of the PEAs were
  overlying magnetic polarity inversion lines when traced back to the
  MDI synoptic charts of the photospheric field. The magnetic polarities
  on both sides of the inversion lines agreed with the dominant magnetic
  pattern expected in cycle 23, i.e. being preferentially positive to the
  West of the PEA axes in the North and negative in the South. One third
  (31%) of the PEA events showed reversed polarities. The origin of PEAs
  is found not just in single bipolar regions (BPRs), but also in between
  pairs of neighboring BPRs. <P />Table 1 is available in electronic
  form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
  or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/422/337

---------------------------------------------------------
Title: VizieR Online Data Catalog: Solar EUV Post-Eruptive Arcades
    (Tripathi+, 2004)
Authors: Tripathi, D.; Bothmer, V.; Cremades, H.
2004yCat..34220337T    Altcode:
  The Extreme ultraviolet Imaging Telescope (EIT) on board the Solar and
  Heliospheric Observatory (SOHO) spacecraft provides unique observations
  of dynamic processes in the low corona. The EIT 195{AA} data taken from
  1997 to the end of 2002 were investigated to study the basic physical
  properties of post-eruptive arcades (PEAs) and their relationship with
  coronal mass ejections (CMEs) as detected by SOHO/LASCO (Large Angle
  Spectrometric Coronagraph). Over the investigated time period, 236 PEA
  events have been identified in total. For each PEA, its EUV lifetime as
  derived from the emission time at 195{AA}, its heliographic position
  and length, and its corresponding photospheric source region inferred
  from SOHO/MDI (Michelson Doppler Imager) data has been studied, as
  well as the variation of these parameters over the investigated phase
  of solar cycle 23. <P />(1 data file).

---------------------------------------------------------
Title: MAGRITTE: an instrument suite for the solar atmospheric
    imaging assembly (AIA) aboard the Solar Dynamics Observatory
Authors: Rochus, Pierre L.; Defise, Jean-Marc; Halain, Jean-Philippe;
   Jamar, Claude A. J.; Mazy, Emmanuel; Rossi, Laurence; Thibert,
   Tanguy; Clette, Frederic; Cugnon, Pierre; Berghmans, David; Hochedez,
   Jean-Francois E.; Delaboudiniere, Jean-Pierre; Auchere, Frederic;
   Mercier, Raymond; Ravet, Marie-Francoise; Delmotte, Franck; Idir,
   Mourad; Schuehle, Udo H.; Bothmer, Volker; Fineschi, Silvano; Howard,
   Russell A.; Moses, John D.; Newmark, Jeffrey S.
2004SPIE.5171...53R    Altcode:
  The Solar Atmospheric Imaging Assembly (AIA) aboard the Solar Dynamics
  Observatory will characterize the dynamical evolution of the solar
  plasma from the chromosphere to the corona, and will follow the
  connection of plasma dynamics with magnetic activity throughout the
  solar atmosphere. The AIA consists of 7 high-resolution imaging
  telescopes in the following spectral bandpasses: 1215Å. Ly-a,
  304 Å He II, 629 Å OV, 465 Å Ne VII, 195 Å Fe XII (includes Fe
  XXIV), 284 Å Fe XV, and 335 Å Fe XVI. The telescopes are grouped
  by instrumental approach: the MAGRITTE Filtergraphs (R. MAGRITTE,
  famous 20th Century Belgian Surrealistic Artist), five multilayer EUV
  channels with bandpasses ranging from 195 to 1216 Å, and the SPECTRE
  Spectroheliograph with one soft-EUV channel at OV 629 Å. They will be
  simultaneously operated with a 10-second imaging cadence. These two
  instruments, the electronic boxes and two redundant Guide Telescopes
  (GT) constitute the AIA suite. They will be mounted and coaligned on a
  dedicated common optical bench. The GTs will provide pointing jitter
  information to the whole SHARPP assembly. This paper presents the
  selected technologies, the different challenges, the trade-offs to be
  made in phase A, and the model philosophy. From a scientific viewpoint,
  the unique combination high temporal and spatial resolutions with the
  simultaneous multi-channel capability will allow MAGRITTE / SPECTRE
  to explore new domains in the dynamics of the solar atmosphere, in
  particular the fast small-scale phenomena. We show how the spectral
  channels of the different instruments were derived to fulfill the
  AIA scientific objectives, and we outline how this imager array will
  address key science issues, like the transition region and coronal waves
  or flare precursors, in coordination with other SDO experiments. We
  finally describe the real-time solar monitoring products that will be
  made available for space-weather forecasting applications.

---------------------------------------------------------
Title: EUVI: the STEREO-SECCHI extreme ultraviolet imager
Authors: Wuelser, Jean-Pierre; Lemen, James R.; Tarbell, Theodore
   D.; Wolfson, C. J.; Cannon, Joseph C.; Carpenter, Brock A.; Duncan,
   Dexter W.; Gradwohl, Glenn S.; Meyer, Syndie B.; Moore, Augustus S.;
   Navarro, Rosemarie L.; Pearson, J. D.; Rossi, George R.; Springer,
   Larry A.; Howard, Russell A.; Moses, John D.; Newmark, Jeffrey S.;
   Delaboudiniere, Jean-Pierre; Artzner, Guy E.; Auchere, Frederic;
   Bougnet, Marie; Bouyries, Philippe; Bridou, Francoise; Clotaire,
   Jean-Yves; Colas, Gerard; Delmotte, Franck; Jerome, Arnaud; Lamare,
   Michel; Mercier, Raymond; Mullot, Michel; Ravet, Marie-Francoise;
   Song, Xueyan; Bothmer, Volker; Deutsch, Werner
2004SPIE.5171..111W    Altcode:
  The Extreme Ultraviolet Imager (EUVI) is part of the SECCHI instrument
  suite currently being developed for the NASA STEREO mission. Identical
  EUVI telescopes on the two STEREO spacecraft will study the structure
  and evolution of the solar corona in three dimensions, and specifically
  focus on the initiation and early evolution of coronal mass ejections
  (CMEs). The EUVI telescope is being developed at the Lockheed Martin
  Solar and Astrophysics Lab. The SECCHI investigation is led by the
  Naval Research Lab. The EUVI"s 2048 x 2048 pixel detectors have a
  field of view out to 1.7 solar radii, and observe in four spectral
  channels that span the 0.1 to 20 MK temperature range. In addition to
  its view from two vantage points, the EUVI will provide a substantial
  improvement in image resolution and image cadence over its predecessor
  SOHO-EIT, while complying with the more restricted mass, power, and
  volume allocations on the STEREO mission.

---------------------------------------------------------
Title: Plasma dynamics of a prominence associated coronal mass
    ejection
Authors: Tripathi, D.; Bothmer, V.; Solanki, S. K.; Schwenn, R.;
   Mierla, M.; Stenborg, G.
2004IAUS..223..401T    Altcode: 2005IAUS..223..401T
  An erupting prominence seen by SOHO/EIT was tracked into the field of
  view of the LASCO C2 and C3 coronagraphs where it developed into the
  core of a structured CME. The erupting prominence was deflected by an
  angle of sim 20^{circ} towards the north pole whereas the consequent
  core of the CME and it's leading edge propagated in the outer corona at
  constant position angle. The prominence material underwent a constant
  acceleration phase until a height of sim1.5 solar radii before it
  started to decelerate up to a distance of 5.0 solar radii. An inflow
  of plasma with a speed of about 70-80 km/s was discovered in the EIT
  observations at a height of 1.5-1.2 solar radii in the course of the
  prominence eruption, matching in time the prominence deceleration
  phase. The downflowing material followed a curved path, suggestive
  of the apex of a contracting magnetic loop sliding down along other
  field lines.

---------------------------------------------------------
Title: Properties of slow magnetic clouds
Authors: Tsurutani, B. T.; Gonzalez, W. D.; Zhou, X. -Y.; Lepping,
   R. P.; Bothmer, V.
2004JASTP..66..147T    Altcode: 2004JATP...66..147T
  Slow (V<SUB>SW</SUB>&lt;400kms<SUP>-1</SUP>) magnetic clouds
  have been analyzed to determine their characteristics and
  geoeffectiveness. It is found that slow clouds have mean magnetic
  field strengths of ~13nT, peak B<SUB>S</SUB>~9nT, and dawn-dusk
  electric fields of E<SUB>SW</SUB>~2.5mVm<SUP>-1</SUP>. The clouds
  are small in spatial size, typically ~0.18AU. The slowest events
  may have been accelerated to their speeds by interaction with the
  slow solar wind. Slow clouds are surprisingly geoeffective. Five
  out of 27 events caused major (D<SUB>ST</SUB>&lt;=-100nT) magnetic
  storms. Likewise, these geoeffective clouds may have been decelerated
  to V<SUB>SW</SUB>&lt;400kms<SUP>-1</SUP>. The issue of interplanetary
  acceleration/deceleration will be examined with SOHO coronal mass
  ejection data in the near future.

---------------------------------------------------------
Title: Properties of Structured Coronal Mass Ejections in Solar
    Cycle 23
Authors: Cremades, H.; Bothmer, V.; Tripathi, D.
2004cosp...35.1939C    Altcode: 2004cosp.meet.1939C
  The Solar and Heliospheric Observatory (SOHO) has provided to date the
  best dataset of coronal observations ever taken over the course of
  a solar cycle. Structured CMEs, i. e. events with clear white-light
  fine structures, have been selected from the LASCO (Large Angle
  Spectroscopic Coronagraph) dataset during the period 1996-2002. Their
  source regions (SRs) in the low corona and photosphere have been deduced
  by analyzing data from the EIT (Extreme-Ultraviolet Imaging Telescope)
  and MDI (Michelson Doppler Imager) instruments on board SOHO, and
  from ground-based Hα measurements. Based on this subset of CMEs,
  originally compiled to study the three-dimensional configuration of
  CMEs, we have analyzed the variation of their properties along the
  present solar cycle. These properties include SR latitude, tilt angle
  of CME SRs, CME position angle, and deviation of CMEs with respect to
  their corresponding SRs.

---------------------------------------------------------
Title: Evolution of the photospheric magnetic field in the source
    regions of coronal mass ejections
Authors: Tripathi, D.; Bothmer, V.; Cremades, H.
2004cosp...35.1966T    Altcode: 2004cosp.meet.1966T
  EIT (Extreme ultraviolet Imaging Telescope) and MDI (Michelson Doppler
  Imager) instruments on board SoHO (Solar and Heliospheric Observatory)
  provide an unprecedented opportunity to study the source regions of
  coronal mass ejections (CMEs) in the low corona and photosphere. Eight
  CMEs associated with filament eruptions observed by EIT near disk
  center were studied in detail. In five events new emerging magnetic
  flux occurred in spatial and temporal relationship with the instability
  sites of the filaments. In two cases field changes in nearby active
  regions seem to have triggered the filament eruptions. In one case,
  evidence for flux cancellation was found. The different possible causes
  of the eruptions are discussed in context with the related changes of
  the photospheric field.

---------------------------------------------------------
Title: Determination of the source regions, 3-D structures and
    magnetic field configurations of CMEs at the Sun and in the
    interplanetary medium
Authors: Bothmer, V.; Cremades, H.; Tripathi, D.
2004cosp...35.1976B    Altcode: 2004cosp.meet.1976B
  There are numerous unanswered questions concerning the origin, nature,
  evolution and consequences of coronal mass ejections at the Sun
  and in the interplanetary medium. STEREO will provide the first 3-D
  view of the Sun-Earth system and Solar-B will provide unprecedented
  measurements of the magnetic field structure of their photospheric
  source regions. The two NASA missions, scheduled for launch in 2006,
  will hence provide us with a new view of CMEs. In order to establish
  the scientific goals of these missions, this talk will provide: - A
  brief summary of our current understanding of the origin and evolution
  of CMEs based on the latest results obtained from SOHO, Yohkoh, TRACE,
  ACE and Wind observations. - A basic scheme explaining the 3-D structure
  and near-Sun evolution of CMEs that can be directly proven with STEREO
  and Solar-B. - An outline for joint science operations required to test
  existing models for the onset and evolution of CMEs up to Earth's orbit.

---------------------------------------------------------
Title: Solar Wind Disturbances and Their Sources in the EUV Solar
    Corona
Authors: Zhukov, A. N.; Veselovsky, I. S.; Clette, F.; Hochedez,
   J. -F.; Dmitriev, A. V.; Romashets, E. P.; Bothmer, V.; Cargill, P.
2003AIPC..679..711Z    Altcode:
  We investigate possible links between the activity manifestations in the
  solar corona and conditions in the solar wind. For the reduction of this
  immense task we have selected 206 events in the solar wind in 1997 -
  2000 corresponding to geomagnetic events with Ap &gt; 20 (compiled into
  a database at &lt;emph TYPE="46"&gt;http://alpha.sinp.msu.ru/apev). Up
  to now, 24 events during the epoch of low solar activity (January 1997 -
  January 1998) are investigated. The solar wind conditions monitored by
  ACE and WIND spacecraft were traced back to the solar corona observed
  by SOHO/EIT. The search for coronal signatures which are probably
  associated with the disturbed solar wind conditions was performed. The
  coronal sources of these 24 events are identified, namely: eruptions in
  active regions, filament eruptions and coronal holes. It is shown that
  halo and partial halo CMEs observed within the SOHO/LASCO sensitivity
  limits are not necessary indicators of Earth-directed eruptions, and
  coronal EUV dimmings can be used as a complementary indicator. We also
  found that a structure now conventionally called a “sigmoid” cannot
  be represented as a single S-shaped loop (flux tube), but exhibits an
  assembly of many smaller structures. It could be formed and destroyed
  via eruptions.

---------------------------------------------------------
Title: Sources of magnetic helicity over the solar cycle
Authors: Bothmer, Volker
2003ESASP.535..419B    Altcode: 2003iscs.symp..419B
  The magnetic field characteristics of a sample set of helical
  magnetic flux rope ICMEs (magnetic clouds) observed by the Wind and
  ACE satellites in solar cycle 23 and their related space weather
  effects are investigated. The solar source regions of the magnetic
  clouds were identified using remote sensing observations of the SOHO,
  Yohkoh and TRACE spacecraft together with ground-based Hα images. Each
  cloud observed at 1 AU could be uniquely associated with a well defined
  frontside halo CME some days before the cloud's arrival at 1 AU. The
  hemispheric origin is consistent with the expected hemispheric helicity
  pattern. The space weather effects of the clouds were quite variable,
  depending on their internal magnetic field configuration and speed
  of progagation.

---------------------------------------------------------
Title: How to forecast geomagnetic storms reliably - The
    characteristics of storms in the rising phase of solar cycle 23
Authors: Bothmer, V.; Cargill, P.; Dmitriev, A.; Romashets, E.;
   Veselovsky, I.; Zhukov, A.
2003EAEJA.....2018B    Altcode:
  The solar wind input parameters were studied for geomagnetic disturbed
  days in which Ap exceeded its average value by using plasma and magnetic
  field data from various near-Earth satellites. More than 270 events
  occurred during the time-period 1997 to 2002. The interplanetary
  and solar characteristics of these events have been summarised
  at http://alpha.sinp.msu.ru/apev. A unique identification of the
  corresponding solar sources was not possible for all of the events,
  but in general they could be classified based on SOHO white-light and
  EUV observations taken by the LASCO/EIT telescopes into disturbances
  caused by coronal hole flows and coronal mass ejections or interactions
  between them. Compression regions caused by stream interactions
  effects including compressed Alfven-waves are also an important
  cause of enhanced geomagnetic activity. Our results imply that the
  forecast of an individual storms does not only require sufficient
  real-time observations of the solar corona, but as well modelling of
  the heliospheric situation, finally taking into account a seasonal
  dependence of the coupling efficiency of the IMF with the Earth’s
  magnetosphere. The work is supported by grants INTAS-ESA 99-00727 and
  INTAS 00-752 .

---------------------------------------------------------
Title: 3D Magnetic Field Configuration and Evolution of Coronal
    Mass Ejections
Authors: Cremades, H.; Bothmer, V.; Tripathi, D.
2003EAEJA......852C    Altcode:
  Coronal Mass Ejections (CMEs) are the most energetic transient
  phenomena in the solar atmosphere. The origins of CMEs, their 3D
  structure and internal magnetic field configuration, as well as their
  evolution into interplanetary space are not well understood. Thanks
  to the high resolution telescopes of the SOHO Mission, for the first
  time magnetic fine structures can be resolved within CMEs observed
  close to the Sun. A set of CME events has been identified from a
  detailed investigation of LASCO (Large Angle Spectroscopic Coronagraph)
  observations taken since launch in 1995. This data set comprises those
  cases exhibiting white-light fine structures, from which their magnetic
  field configuration could be deduced. Since the observed white-light
  features are the result of an inherent line-of-sight integration
  projected on the plane of the sky, inferring the three-dimensional
  topology of CMEs is a challenging and complicated task. In order
  to reveal the actual 3D profile of a CME, an approach based on the
  characterization of their respective source region magnetic field
  configuration is addressed. The study indicates that many CMEs are
  comprised either of arcades of magnetic field lines or magnetic
  flux tubes which are trailed by prominence material. The analysis of
  additional coronal and magnetic field observations (EIT, MDI) shows
  that these magnetic structures seem to arise from already existing loop
  systems of much smaller scale that originate in bipolar field regions.

---------------------------------------------------------
Title: Solar wind disturbances and their sources in the EUV solar
    corona
Authors: Zhukov, A.; Veselovsky, I.; Bothmer, V.; Dmitriev, A.;
   Clette, F.; Romashets, E.; Cargill, P.
2003EAEJA.....2682Z    Altcode:
  We investigate possible links between the activity manifestations in
  the solar corona and conditions in the solar wind. For the reduction
  of this immense task we have selected 206 events in the solar wind
  in 1997 -- 2000 corresponding to geomagnetic events with Ap &gt; 20
  (compiled into a database at http://alpha.sinp.msu.ru/apev). The solar
  wind conditions monitored by ACE and WIND spacecraft were traced back to
  the solar corona observed by SOHO/EIT. The search for coronal signatures
  that are probably associated with the disturbed solar wind conditions
  was performed. The coronal sources of the events are identified, namely:
  eruptions in active regions, filament eruptions and coronal holes. It is
  shown that halo and partial halo CMEs observed within the SOHO/LASCO
  sensitivity limits are not necessary indicators of Earth-directed
  eruptions, and coronal EUV dimmings can be used as a complementary
  indicator. We also found that a structure now conventionally called a
  ”sigmoid” cannot be represented as a single S-shaped loop (flux tube),
  but exhibits an assembly of many smaller structures. It could be formed
  and destroyed via eruptions.

---------------------------------------------------------
Title: Identification of Solar Sources of Major Geomagnetic Storms
    between 1996 and 2000
Authors: Zhang, J.; Dere, K. P.; Howard, R. A.; Bothmer, V.
2003ApJ...582..520Z    Altcode:
  This paper presents identification of solar coronal mass ejection (CME)
  sources for 27 major geomagnetic storms (defined by disturbance storm
  timeindex&lt;=-100 nT) occurring between 1996 and 2000. Observations of
  CMEs and their solar surface origins are obtained from the Large Angle
  and Spectrometric Coronagraph (LASCO) and the EUV Imaging Telescope
  (EIT) instruments on the SOHO spacecraft. Our identification has
  two steps. The first step is to select candidate front-side halo
  (FSH) CMEs using a fixed 120 hr time window. The second step is
  to use solar wind data to provide further constraints, e.g., an
  adaptive time window defined based on the solar wind speed of the
  corresponding interplanetary CMEs. We finally find that 16 of the
  27 (59%) major geomagnetic storms are identified with unique FSH
  CMEs. Six of the 27 events (22%) are associated with multiple FSH
  CMEs. These six events show complex solar wind flows and complex
  geomagnetic activity, which are probably the result of multiple halo
  CMEs interacting in interplanetary space. A complex event occurs when
  multiple FSH CMEs are produced within a short period. Four of the 27
  (15%) events are associated with partial-halo gradual CMEs emerging
  from the east limb. The surface origin of these events is not known
  because of a lack of any EIT signature. We believe that they are
  longitudinally extended CMEs having a component moving along the
  Sun-Earth connection line. One of the 27 major geomagnetic storms is
  caused by a corotating interaction region. We find an asymmetry in
  the longitudinal distribution of solar source region for the CMEs
  responsible for major geomagnetic storms. They are more likely
  to originate from the western hemisphere than from the eastern
  hemisphere. In terms of latitude, most geoeffective CMEs originate
  within a latitude strip of +/-30°. The average transit time for a
  solar CME to arrive at the near-Earth space is found to be 64 hr,
  while it takes 78 hr on average to reach the peak of the geomagnetic
  storm. There is a correlation between CME transit time from the Sun
  to the near-Earth space (T, in hours) and the CME initial velocity
  (V, in unit of kilometers per second) at the Sun, which can be simply
  described as T=96-(V/21). We also find that while these geoeffective
  CMEs are either full-halo CMEs (67%) or partial-halo CMEs (30%),
  there is no preference for them to be fast CMEs or to be associated
  with major flares and erupting filaments.

---------------------------------------------------------
Title: Dynamics of open solar magnetic fields, active longitudes,
    and near earth disturbances
Authors: Ivanov, K.; Bothmer, V.; Kharshiladze, A.; Romashets, E.;
   Veselovsky, I.
2002ESASP.506..141I    Altcode: 2002ESPM...10..141I; 2002svco.conf..141I
  Open magnetic field lines in the solar corona are calculated in order to
  study their relationship to solar activity and near Earth disturbances
  in 2000. Slow, rotation by rotation, dynamics of photospheric regions
  with open fields show a correlation with generating and decay of
  active complexes located at longitudes 280-360 degrees, and with the
  series of the near Earth recurrent extra storms on May 24, July 15,
  August 12, and October 5.

---------------------------------------------------------
Title: Solar and Heliospheric Causes of Geomagnetic Perturbations
    during the Growth Phase of Solar Cycle 23
Authors: Bothmer, V.; Veselovsky, I. S.; Dmitriev, A. V.; Zhukov,
   A. N.; Cargill, P.; Romashets, E. P.; Yakovchouk, O. S.
2002SoSyR..36..499B    Altcode:
  A database is compiled for the study of solar and heliospheric causes
  of geomagnetic perturbations with the daily average index A<SUB>r</SUB>
  &gt; 20 that were observed in the period 1997-2000. The number of such
  events (more than 200) progressively increased and fluctuated as the
  current solar cycle developed. It is established that geomagnetic
  storms are generated by dynamical processes and structures near
  the center of the solar disk in a zone of several tens of degrees,
  and these processes are responsible for the appearance in the Earth's
  region, within several tens of hours, of quasistationary and transient
  solar wind streams with a sufficiently strong southward component of
  the heliospheric magnetic field. These streams lasted more than a few
  hours. The following structures can serve as morphological indicators
  for the prediction of the appearance of such streams: (1) active and
  disappearing filaments derived from synoptic N<SUB>α</SUB>-maps of the
  Sun, (2) solar flares, (3) coronal holes and evolving active regions,
  and (4) the heliospheric current sheet. The geometry of coronal mass
  ejections needs further observational study.

---------------------------------------------------------
Title: Solar energetic electron events and coronal shocks
Authors: Klassen, A.; Bothmer, V.; Mann, G.; Reiner, M. J.; Krucker,
   S.; Vourlidas, A.; Kunow, H.
2002A&A...385.1078K    Altcode:
  Mildly relativistic electrons appear during the solar energetic particle
  events. A detailed investigation on the origin of such electrons is
  presented for four particlular solar events. The mildly relativistic
  electrons have been detected at energies of 0.25-0.7 MeV by COSTEP/SOHO
  and below 0.392 MeV by Wind 3-DP experiments. Coronal shocks associated
  with these electron events are identified from the metric-to-decametric
  solar type II radio bursts. All selected events were associated with
  solar activity at western longitudes, so that the magnetic footpoints
  connecting the spacecraft with the Sun were close to the flare/shock/CME
  site. The associated type II bursts were accompanied by so-called shock
  accelerated (SA) type III bursts appearing to be emerging from the type
  II emission site. We found: (1) that all of the 0.25-0.7 MeV electron
  events were released during or after, but never simultaneously with the
  onset of type II bursts and CMEs. The time delay between the type II
  burst onset and the release of the mildly relativistic electrons is in
  the range of 11.5-45 min; (2) that the mildly relativistic electrons
  were released rather at the end of SA type III bursts or somewhat
  later; (3) that the mildly relativistic electrons were released when
  the associated type II burst and the CME reached a certain height
  (h ~ 1-4 R_s) above the photosphere. For the four events studied,
  it is concluded that mildly relativistic electrons at 0.25-0.7 MeV
  energies measured in the interplanetary medium from solar energetic
  particle events are accelerated by coronal shock waves, commonly in
  association with white-light CMEs.

---------------------------------------------------------
Title: Solar and heliospheric origins of geomagnetic perturbations
    in the rising phase of Solar Cycle 23
Authors: Bothmer, V.; Cargill, P.; Romashets, E. P.; Veselovsky, I. S.
2002ESASP.477..331B    Altcode: 2002scsw.conf..331B
  Solar sources of strong geomagnetic perturbations are connected
  to coronal mass ejections and corotating inhomogeneities in the
  heliosphere. Geomagnetic perturbations with Ap &gt; 20 in 1997-2000 were
  produced by heliospheric magnetic fields and solar wind plasma streams
  related to the following morphological features observed at the Sun:
  1) active and disappearing filaments and prominences (sdf) seen in Hα
  synoptic maps; 2) solar flares; 3) evolving active regions and coronal
  holes (CH); 4) heliospheric current sheet (HCS) positions deduced from
  photospheric magnetic field measurements. Strong geomagnetic storms
  during this period of time were observed when compound plasma streams
  from several sources on the Sun reached the Earth's magnetosphere. The
  combination of the transient processes and corotating inhomogeneities
  in the solar corona and deeper layers of the solar atmosphere not far
  from the center of the solar disk (first tens of degrees) represent
  a sufficient condition for the formation of such compound streams
  exemplified by sdf-CH-HCS passage.

---------------------------------------------------------
Title: Subsector structure of the interplanetary space - SOLSPA 2001
Authors: Ivanov, K. G.; Bothmer, V.; Cargill, P.; Kharshiladze, A. F.;
   Romashets, E. P.; Veselovsky, I. S.
2002ESASP.477..317I    Altcode: 2002scsw.conf..317I
  A new conception about sub-sector structure of the interplanetary
  space is introduced. It is shown that in a potential model of the
  solar magnetic field there exist direct relations between photospheric
  regions of open magnetic field lines and corresponding magnetic domains
  at the source surface and in the interplanetary magnetic field. These
  domains generate a large-scale sub-sector structure of the solar and
  interplanetary magnetic field, with boundaries between domains of the
  same polarities. Solar, interplanetary, and ground-based observations
  of 1999-2000 were used to test this conclusion.

---------------------------------------------------------
Title: The solar sources of magnetic helicity in interplanetary space
Authors: Bothmer, V.
2002cosp...34E1390B    Altcode: 2002cosp.meetE1390B
  About one third of all coronal mass ejections (CMEs) in the solar wind
  possess the internal structure of helical magnetic flux ropes. Recent
  studies have shown that the magnetic chiralities of the flux ropes can
  be traced back to individual bipolar regions in the Sun's northern
  and southern hemispheres. This presentations presents an overview
  about the solar source regions that lead to helical flux rope CMEs
  in the interplanetary medium including their solar cycle variability
  and addresses the possibility of conservation of magnetic helicity in
  space plasmas.

---------------------------------------------------------
Title: Magnetic storm cessation during sustained Northward IMF
Authors: Veselovsky, I.; Bothmer, V.; Cargill, P.; Ivanov, K.;
   Romashets, E.; Yakovchouk, O.
2002cosp...34E.420V    Altcode: 2002cosp.meetE.420V
  Times of sustained strong Northward IMF can interrupt the magnetic
  storm development and lead to lower levels of geomagnetic activity
  for many hours. During 1997-2000 we have found two events of this kind
  observed on November 8, 1998 and October 13, 2000. In both cases, the
  storms started as usual after arrival of ejecta with a southward IMF
  component from the Sun to the Earth, but ceased after several hours
  due to the onset of sustained Northward IMF. After the passage of
  this so called positive domain storm development started again. The
  heliospheric magnetic field intensity remained enhanced and nearly
  constant. The solar origins of the geomagnetic storm interruptions have
  been investigated. Tentatively they may be related to strong nonlinear
  Alfven type solitary waves excited by nonstationary coronal current
  variations with a characteristic time-scale of about a day.

---------------------------------------------------------
Title: Formation and Development of Shock Waves in the Solar Corona
    and Near-Sun Interplanetary Space and Solar Energetic Particle Events
Authors: Mann, G. J.; Klassen, A.; Aurass, H.; Classen, H.; Bothmer,
   V.; Reiner, M. J.
2001AGUFMSH21B..03M    Altcode:
  At the Sun shock waves are produced either by flares or by coronal mass
  ejections and are regarded as the source of solar energetic particle
  events. In the corona shock waves appear as solar type II radio bursts
  often associated with coronal transient (or EIT) waves. The propagation
  of a disturbance through the corona away from an active region into the
  interplanetary space is considered by evaluating the radial behaviour
  of the Alfven speed. The magnetic field of an active region is modelled
  by a magnetic dipole and is superimposed on that of the quiet Sun as
  deduced from the EIT wave analysis. Such a behaviour of the magnetic
  field leads to a local minimum of the Alfven speed in the range 1.2-1.8
  solar radii in the corona as well as a maximum of 740 km/2 at a distance
  of 3.8 solar radii. The occurrence of such a minimum and maximum of the
  Alfven speed has important consequences to the formation and development
  of shock waves in the corona and near-Sun interplanetary space and to
  their ability to accelerate particles leading to a special temporal
  behaviour of solar energetic particle events.

---------------------------------------------------------
Title: <SUP>3</SUP>He-enrichments in solar energetic particle events:
    SOHO/COSTEP observations
Authors: Bothmer, V.; Sierks, H.; Böhm, E.; Kunow, H.
2001AIPC..598..349B    Altcode: 2001sgc..conf..349B
  We present first results based on a systematic survey of 4-41
  MeV/N <SUP>3</SUP>He/<SUP>4</SUP>He isotope abundances with ratios
  &gt;0.01 detected by the COmprehensive SupraThermal and Energetic
  Particle analyzer (COSTEP) onboard the SOHO (SOlar and Heliospheric
  Observatory) spacecraft. During 53 out of 148 identified days with a
  <SUP>3</SUP>He/<SUP>4</SUP>He ratio &gt;=0.01, the ratio was in the
  range 0.1-1.0. For days with sufficiently high detector count rates,
  the atomic mass plots could be resolved up to a time resolution of
  1 hour. These days were most suitable for comparisons with in situ
  solar wind plasma and magnetic field measurements and SOHO's optical
  white-light and extreme ultraviolet (EUV) observations of the Sun. Here
  we present a brief overview of a <SUP>3</SUP>He/<SUP>4</SUP>He-rich
  particle event detected on October 30, 2000 that was associated with
  the passage of a fast CME. .

---------------------------------------------------------
Title: Galactic abundances: Report of working group 3
Authors: Klecker, B.; Bothmer, V.; Cummings, A. C.; George, J. S.;
   Keller, J. W.; Salerno, E.; Sofia, U. J.; Stone, E. C.; Thielemann,
   F. -K.; Wiedenbeck, M. E.; Buclin, F.; Christian, E. R.; Flückiger,
   E. O.; Hofer, M. Y.; Jones, F. C.; Kirilova, D.; Kunow, H.; Laming,
   M.; Tranquille, C.; Wenzel, K. -P.
2001AIPC..598..207K    Altcode: 2001sgc..conf..207K
  We summarize the various methods and their limitations and strengths
  to derive galactic abundances from in-situ and remote-sensing
  measurements, both from ground-based observations and from instruments
  in space. Because galactic abundances evolve in time and space it is
  important to obtain information with a variety of different methods
  covering different regions from the Very Local Insterstellar Medium
  (VLISM) to the distant galaxy, and different times throughout the
  evolution of the galaxy. We discuss the study of the present-day VLISM
  with neutral gas, pickup ions, and Anomalous Cosmic Rays, the study of
  the local interstellar medium (ISM) at distances &lt;1.5 kpc utilizing
  absorption line me asurements in H I clouds, and the study of galactic
  cosmic rays, sampling contemporary (~15 Myr) sources in the local ISM
  within a few kiloparsec of the solar system. Solar system abundances,
  derived from solar abundances and meteorite studies are discussed
  in several other chapters of this volume. They provide samples of
  matter from the ISM from the time of solar system format ion, about
  4.5 Gyr ago. The evolution of galactic abundances on longer time
  scales is discussed in the context of nuclear synthesis in the various
  contributing stellar objects. .

---------------------------------------------------------
Title: MeV He3/He4 isotope abundances in solar energetic particle
events: SOHO/COSTEP observations
Authors: Bothmer, V. :; Sierks, H.; Böhm, E.; Kunow, H.
2001ICRC....8.3095B    Altcode: 2001ICRC...27.3095B
  We present first results based on a systematic survey of 4-41 MeV/N
  3He/4He isotope abundances with ratios &gt;0.01 detected by the
  COmprehensive SupraThermal and Energetic Particle analyzer (COSTEP)
  onboard the SOHO (SOlar and Heliospheric Observatory) spacecraft. More
  than about 25% of the identified events showed 3He/4He ratios in
  the range 0.1-1. For events with sufficiently high detector count
  rates the atomic mass plots can be resolved up to a time resolution
  of about 1 hour. These events are most suitable for comparisons with
  in situ solar wind plasma and magnetic field measurements and SOHO's
  optical white-light and extreme ultraviolet (EUV) observations of
  the Sun. The correlations show an association with passages of shock
  associated coronal mass ejections (CMEs) in the solar wind that
  inhibit high He/H plasma overabundances. It is likely that the CMEs
  have been released in strong magnetic reconfiguration processes at
  the solar source sites. Here we present a brief overview of such an
  event detected on October 30, 2000. 1. Introduction The SOHO/COSTEP
  instrument measures solar energetic particles (SEPs) at MeV energies
  in the interplanetary medium. The solid state detectors are capable
  to detect 3 He/4 He-enrichments at these energies (Müller-Mellin
  et al., 1995). Usually, the 3 He/4 He-ratio in the solar wind is at
  the order of 10-4 , but occasionally ratios up to about values of ~1
  or even above have been observed in SEP events (e.g., Mason et al.,
  1999). The origin of these isotope abundances has commonly been
  attributed to impulsive solar flares and wave-particle interaction
  mechanisms (Temerin and Roth, 1992). However, fully satisfying physical
  explanations are still lacking. Here we present first results of a
  systematic survey of the He-measurements taken by COSTEP since launch
  in 1995 until the end of the year 2000. 2. Data For this study we have
  analyzed SOHO/COSTEP measurements of 4.3-40.9 MeV/N helium particles
  as well as COSTEP data covering proton and electron measurements at
  energies below 10 MeV. These data were compared with magnetic field
  and plasma data from the Advanced Coposition Explorer (ACE), SOHO/LASCO
  (Large Angle Spectroscopic COronagraph) observations of CMEs and X-ray
  flare measurements taken by the GOES satellite. 3. Identification of
  3 He/4 He-rich events Figure 1 shows an example of a 3 He/4 He-rich
  event as identified from the COSTEP mass separation plot for Oct. 30,
  2000. The vertical axis in Figure 1 provides information about the
  detector count rates, the horizontal axis is labelled such that 4 He
  corresponds to a value of 0. The two largest peaks in the count rates
  at -0.6 and 0 correspond to proton (-0.6) and 4 He particles. The
  presence of a major contribution of 3 He isotopes at about -0.05
  is very distinguished. The ratio of 3 He/4 He was 0.7 (see Table 1,
  doy 304 in 2000). All identified ratios &gt;0.01 are listed in Table
  1. Figure 1. COSTEP mass plot for 30 October 2000. The peaks at -0.6,
  -0.05 and 0 correspond to p, 3 He and 4 He. p 3 He 4 He

---------------------------------------------------------
Title: EIT Waves, Coronal Shock Waves, and Solar Energetic Particle
    Events
Authors: Mann, G.; Klassen, A.; Aurass, H.; Classen, H. T.; Bothmer,
   V.; Reiner, M. J.
2001pre5.conf..445M    Altcode:
  EIT waves are often associated with Solar type II radio bursts as
  recently revealed by Klassen et al. [2000]. It is well-known that Solar
  type II radio bursts are generated by shock waves traveling through the
  corona of the Sun. Since both phenomena are causally connected with each
  other, they can be used as a diagnostic tool of the magnetic field in
  the corona. Thus, a magnetic field of 2.2 G and 0.5 G is deduced to be
  at the photosphere and at a distance of 2 Solar radii above quiet Solar
  regions, respectively. Such a behaviour of the magnetic field leads to
  a local maximum of the Alfven speed of about 740 km/s at a distance
  of 3.8 Solar radii. The occurrence of such a maximum has important
  consequences for the formation and development of shock waves in the
  Solar corona and the near-sun interplanetary space and their ability
  to accelerate particles leading to Solar energetic particle events.

---------------------------------------------------------
Title: Recurrent modulation of galactic cosmic ray electrons and
protons: Ulysses COSPIN/KET observations
Authors: Heber, B.; Blake, J. B.; Paizis, C.; Bothmer, V.; Kunow,
   H.; Wibberenz, G.; Burger, R. A.; Potgieter, M. S.
2000AIPC..528..357H    Altcode: 2000atep.conf..357H
  Since measurements of space probes in the interplanetary space became
  available it has been known that associated with the occurrence
  of recurrent fast and slow solar wind streams, forming Corotating
  Interaction Regions, recurrent variations in the cosmic ray nuclei
  flux are observed (1). As pointed out recently by Jokipii and Kota (2)
  recurrent modulation for positively and negatively charged particles
  may be different. In the time interval extending from July 1992 to
  July 1994, Ulysses on its journey to high heliographic latitudes
  registered ~20 stable and long-lasting Corotating Interaction Regions
  (CIRs). In this work we use data from the Cosmic Ray and Solar Particle
  Investigation Kiel Electron Telescope (COSPIN/KET) instrument on
  board Ulysses to study the recurrent variation of 2.5 GV electrons and
  protons. We find that 1) electrons are indeed periodically modulated,
  but that 2) the periodicity of ~29 days is longer than the period of
  ~26 days for protons, and that 3) the amplitude is larger than the
  one observed for protons. .

---------------------------------------------------------
Title: Solar energetic particle event and radio bursts associated
    with the 1996 July 9 flare and coronal mass ejection
Authors: Laitinen, T.; Klein, K. -L.; Kocharov, L.; Torsti, J.;
   Trottet, G.; Bothmer, V.; Kaiser, M. L.; Rank, G.; Reiner, M. J.
2000A&A...360..729L    Altcode:
  Using spaceborne particle and gamma-ray detection and radio diagnostics
  we study solar energetic particle (SEP) production in the 1996 July
  9 event. This event is associated with an impulsive soft X-ray flare
  (9:10 UT) and a coronal mass ejection (CME). In a global classification
  the event is considered as mixed-impulsive. A sequence of acceleration
  processes is identified, starting early in the flare impulsive phase
  and continuing throughout the period when the CME propagated up to
  several R<SUB>solar</SUB> above the photosphere: (1) Gamma-ray,
  hard X-ray and cm-wave emitting particles seen during the flare
  impulsive phase in the low corona had no counterpart at the Solar and
  Heliospheric Observatory (SoHO) spacecraft. (2) Electrons accelerated
  at a coronal shock wave were revealed by decimetric- to-metric type II
  radio emission and by simultaneous radio signatures of beams traveling
  to 1 AU. (3) Mildly relativistic (&gt;=250 keV) electrons detected by
  SoHO did not correspond to these shock-accelerated populations, but
  to later mainly impulsive injection which was associated with radio
  brightenings over a large range of coronal altitudes. (4) Energetic
  protons detected by SoHO were accelerated during about 100 min after
  the flare impulsive phase with a gradually evolving production profile
  that bore some similarity with the time profile of broadband metric
  (type IV) emission. (5) While all other particle signatures decayed,
  a second period of interplanetary proton production took place &gt;=2
  hours after flare onset. The first, 100 min period of SEP acceleration,
  post-impulsive phase coronal acceleration, is definitely dominant in
  mildly relativistic electrons. Two acceleration periods nearly equally
  contribute to the production of ~ 20 MeV protons. However, the second
  period is more productive in low energy, ~ 1 MeV, protons. The timing
  of the SEP injections indicates that neither the impulsive flare
  acceleration in the low corona nor the interplanetary CME at &gt;=
  10 R<SUB>solar</SUB> are the main sources of the high-energy particles
  observed onboard SoHO. We suggest that various acceleration processes
  related to the reconfiguration of the corona in the course of the flare
  and CME lift-off contribute to the interacting and escaping particle
  populations, with different signatures at different energies and in
  different species.

---------------------------------------------------------
Title: Energetic Particle Signatures of a Corotating Interaction
Region from a High Latitude Coronal Hole: SOHO, Wind and Ulysses
    Observations
Authors: Posner, A.; Bothmer, V.; Kunow, H.; Gosling, J. T.; Heber,
   B.; Lazarus, A. J.; Linker, J. A.; Marsden, R. G.; Mikić, Z.;
   Müller-Mellin, R.; Sanderson, T. R.; Szabo, A.; Thompson, B. J.
2000AdSpR..26..865P    Altcode:
  In mid 1996 the Comprehensive Suprathermal and Energetic Particle
  Analyser (COSTEP) onboard the Solar and Heliospheric Observatory, at
  1 AU in the ecliptic plane, detected recurrent periods of enhanced
  MeV ions in association with a corotating interaction region
  (CIR). Measurements of energetic ions from the Cosmic Ray and Solar
  Particle Instrument/Low Energy Telescope (COSPIN/LET) onboard Ulysses
  taken at 5 AU, at mid-northern heliographic latitudes, showed that
  Ulysses encountered recurrent particle events during the same time
  period. We used the solar wind speeds observed at both locations to
  estimate the cor-responding solar source longitudes of the particle
  events. These longitudes are related to warps of the Sun's large high
  latitude northern coronal hole boundaries observed by SOHO's Extreme
  Ultraviolet Imaging Telescope (EIT). The findings are supported
  by threedimensional magnetohydrodynamic (MHD) calculations of the
  footpoint positions of the magnetic field lines at both spacecraft. The
  observations suggest that close to the Sun a superradial expansion of
  the fast solar wind from the Sun's high latitude northern coronal hole
  down to ecliptic latitudes is present

---------------------------------------------------------
Title: SOHO und das neue Bild der Sonne.
Authors: Bothmer, V.
1999A&R....36...28B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Reply
Authors: Kahler, S. W.; Cane, H. V.; Hudson, H. S.; Kurt, V. G.;
   Gotselyuk, Y. V.; MacDowall, R. J.; Bothmer, V.
1999JGR...10422411K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Differences in the temporal variations of galactic cosmic
ray electrons and protons: Implications from Ulysses at solar minimum
Authors: Heber, B.; Ferrando, P.; Raviart, A.; Wibberenz, G.;
   Müller-Mellin, R.; Kunow, H.; Sierks, H.; Bothmer, V.; Posner, A.;
   Paizis, C.; Potgieter, M. S.
1999GeoRL..26.2133H    Altcode:
  According to standard drift dominated modulation models the intensity
  variations of galactic cosmic ray protons and electrons respond
  differently to the latitudinal extension of the heliospheric current
  sheet α. In an A&gt;0 solar cycle intensities of protons should vary
  weakly with the latitudinal extension, whereas electrons should show
  a strong response. We investigate this charge dependent variation
  in the 1990s (A&gt;0) using Ulysses Kiel Electron Telescope (KET)
  measurements. Proton measurements at 2.5 GV corrected for latitudinal
  variations show the same time profile as electrons from mid 1994 until
  the beginning of 1996, and later from September 1997 to the end of
  1997. In 1996 and 1997, when α was below ∼25°, two long lasting time
  periods were found when electrons had a ∼5-10% higher level. These
  variations are in agreement with our computations indicating that drift
  effects play an important role in determining the temporal variation
  of electrons close to solar minimum.

---------------------------------------------------------
Title: CIR Morphology, Turbulence, Discontinuities, and Energetic
    Particles
Authors: Crooker, N. U.; Gosling, J. T.; Bothmer, V.; Forsyth, R. J.;
   Gazis, P. R.; Hewish, A.; Horbury, T. S.; Intriligator, D. S.; Jokipii,
   J. R.; Kóta, J.; Lazarus, A. J.; Lee, M. A.; Lucek, E.; Marsch, E.;
   Posner, A.; Richardson, I. G.; Roelof, E. C.; Schmidt, J. M.; Siscoe,
   G. L.; Tsurutani, B. T.; Wimmer-Schweingruber, R. F.
1999SSRv...89..179C    Altcode:
  Corotating interaction regions (CIRs) in the middle heliosphere have
  distinct morphological features and associated patterns of turbulence
  and energetic particles. This report summarizes current understanding
  of those features and patterns, discusses how they can vary from
  case to case and with distance from the Sun and possible causes of
  those variations, presents an analytical model of the morphological
  features found in earlier qualitative models and numerical simulations,
  and identifies aspects of the features and patterns that have yet to
  be resolved.

---------------------------------------------------------
Title: The Solar Origin of Corotating Interaction Regions and Their
    Formation in the Inner Heliosphere
Authors: Balogh, A.; Bothmer, V.; Crooker, N. U.; Forsyth, R. J.;
   Gloeckler, G.; Hewish, A.; Hilchenbach, M.; Kallenbach, R.; Klecker,
   B.; Linker, J. A.; Lucek, E.; Mann, G.; Marsch, E.; Posner, A.;
   Richardson, I. G.; Schmidt, J. M.; Scholer, M.; Wang, Y. -M.;
   Wimmer-Schweingruber, R. F.; Aellig, M. R.; Bochsler, P.; Hefti, S.;
   Mikić, Z.
1999SSRv...89..141B    Altcode:
  Corotating Interaction Regions (CIRs) form as a consequence of the
  compression of the solar wind at the interface between fast speed
  streams and slow streams. Dynamic interaction of solar wind streams
  is a general feature of the heliospheric medium; when the sources of
  the solar wind streams are relatively stable, the interaction regions
  form a pattern which corotates with the Sun. The regions of origin
  of the high speed solar wind streams have been clearly identified
  as the coronal holes with their open magnetic field structures. The
  origin of the slow speed solar wind is less clear; slow streams may
  well originate from a range of coronal configurations adjacent to,
  or above magnetically closed structures. This article addresses
  the coronal origin of the stable pattern of solar wind streams
  which leads to the formation of CIRs. In particular, coronal models
  based on photospheric measurements are reviewed; we also examine
  the observations of kinematic and compositional solar wind features
  at 1 AU, their appearance in the stream interfaces (SIs) of CIRs,
  and their relationship to the structure of the solar surface and the
  inner corona; finally we summarise the Helios observations in the
  inner heliosphere of CIRs and their precursors to give a link between
  the optical observations on their solar origin and the in-situ plasma
  observations at 1 AU after their formation. The most important question
  that remains to be answered concerning the solar origin of CIRs is
  related to the origin and morphology of the slow solar wind.

---------------------------------------------------------
Title: Magnetic field structure and topology within CMEs in the
    solar wind
Authors: Bothmer, Volker
1999AIPC..471..119B    Altcode: 1999sowi.conf..119B
  This paper provides a brief overview on the magnetic field structure and
  topology within coronal mass ejections (CMEs) in the solar wind. The
  overview starts summarizing the magnetic field characteristics within
  CMEs (magnetic clouds) which exhibit large-scale internal magnetic field
  rotations indicative of helical magnetic flux ropes and those of non
  flux rope CMEs lacking smooth internal field rotations. The overview
  continues with a presentation of Ulysses observations showing evidence
  for mixed magnetic topologies of open and closed field lines within some
  CMEs followed by a discussion of the magnetic field structure of CMEs
  near the Sun in relationship with the observed field properties of CMEs
  in the solar wind. Finally, the to date main open questions concerning
  the magnetic origin, evolution and fate of CMEs are addressed.

---------------------------------------------------------
Title: In-ecliptic CIR-associated energetic particle events and polar
coronal hole structures: SOHO/COSTEP observations for the Whole Sun
    Month Campaign
Authors: Posner, Arik; Bothmer, Volker; Thompson, Barbara J.; Kunow,
   Horst; Heber, Bernd; Müller-Mellin, Reinhold; Lazarus, Alan J.;
   Szabo, Adam; Mikić, Zoran; Linker, Jon A.
1999JGR...104.9881P    Altcode:
  The Solar and Heliospheric Observatory (SOHO), in halo orbit around
  the L1 Lagrangian point of the Sun-Earth system, combines a unique
  set of instruments for studies of the Sun and the heliosphere. SOHO's
  Comprehensive Suprathermal and Energetic Particle Analyser measures
  in situ particles in the energy range 44 keV/particle to above 53
  MeV/nucleon. For the time period of the Whole Sun Month Campaign in
  mid 1996 we have identified recurrent energetic particle intensity
  increases in association with corotating interaction regions (CIRs)
  in the energy range &lt;10 MeV. Solar wind measurements of the Wind
  spacecraft were used to estimate the corresponding magnetic source
  location in Carrington longitude for comparison of energetic particles
  with synoptic maps of the lower corona, derived from images of SOHO's
  Extreme-ultraviolet Imaging Telescope. The comparison reveals a close
  relationship of latitudinal extensions of polar coronal holes, situated
  in regions up to 40° away from the ecliptic, with CIR-associated
  in-ecliptic particle events.

---------------------------------------------------------
Title: Determination of 7-30 MeV electron intensities: ULYSSES
    COSPIN/KET Results
Authors: Heber, Bernd; Raviart, A.; Ferrando, P.; Sierks, H.; Paizis,
   C.; Kunow, H.; Muller-Mellin, R.; Bothmer, V.; Posner, A.
1999ICRC....7..186H    Altcode: 1999ICRC...26g.186H
  The COsmic and Solar Particle INvestigation Kiel Electron Telescope
  was designed to measure electrons from a few MeV up to a few
  GeV using particle energy loss and particle velocity measurement
  techniques. Unfortunately the KET channel measuring electrons in the
  energy range from 7-170 MeV is contaminated by a γ-ray background
  (Ferrando et al., 1996). Besides a possible slight contribution from the
  RTG radiation, we have shown that this background is mainly generated
  by high energy protons interacting with the spacecraft matter. Such
  γ-rays can enter "unseen" the instrument and are partially converted
  into electrons in the calorimeter consisting of a high Z lead fluoride
  Cherenkov detector. Such electrons could be counted in the 7-170 MeV
  electron channels. In this paper we present a method to quantify this
  background and thus determine lower and upper limits for the intensities
  of electrons with energies from 7 to 30 MeV. Our analysis shows that
  above 30 MeV the background in this specific channel is so dominant,
  that no correction is possible.

---------------------------------------------------------
Title: CIR Morphology, Turbulence, Discontinuities, and Energetic
    Particles
Authors: Crooker, N. U.; Gosling, J. T.; Bothmer, V.; Forsyth, R. J.;
   Gazis, P. R.; Hewish, A.; Horbury, T. S.; Intriligator, D. S.; Jokipii,
   J. R.; Kóta, J.; Lazarus, A. J.; Lee, M. A.; Lucek, E.; Marsch, E.;
   Posner, A.; Richardson, I. G.; Roelof, E. C.; Schmidt, J. M.; Siscoe,
   G. L.; Tsurutani, B. T.; Wimmer-Schweingruber, R. F.
1999cir..book..179C    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Energetic Particle Events recorded aboard SOHO on
    December 24, 1996 and on May 6, 1998
Authors: McKenna-Lawlor, Susan M. P.; Kecskeméty; K.; Bothmer, V.;
   Rodriguez-Pacheco, J.; Facskó, G.; St. Cyr, C.
1999ICRC....6..423M    Altcode: 1999ICRC...26f.423M
  The LION experiment on SOHO (which records protons from 44 keV-6 MeV
  and electrons from 44 keV-300 keV), and the energetically complementary
  EPHIN experiment (which measures protons + helium ions to &gt;53 MeV/n
  and electrons to &gt;5 MeV), each detected many energetic particle
  events (SEPs) in the early rising phase of Solar Cycle 23 (from ~
  July 1996) - a period commonly associated with Coronal Mass Ejections
  (CMEs). The present paper contains an account of two representative
  rapid intensity increases recorded simultaneously by LION and
  EPHIN, each of which was accompanied by a CME and by impulsive type
  flaring. The SEPs have characteristics typical of both Gradual and
  Impulsive events and may be described as `Mixed'.

---------------------------------------------------------
Title: Solar Corona, Solar Wind Structure and Solar Particle Events
Authors: Bothmer, V.
1999spwe.work..117B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Energy spectra of protons, deuterium, and helium nuclei during
    quiet solar activity periods in 1996-97
Authors: Kecskemety, Karoly; Kunow, H.; Valtonen, E.; Kiraly, P.;
   Muller-Mellin, R.; Torsti, J.; Bothmer, V.
1999ICRC....6..167K    Altcode: 1999ICRC...26f.167K
  A background reduction method based on pulse-height analysis (see
  accompanying paper by Valtonen et al.) is applied for the data of
  the ERNE and EPHIN energetic particle telescopes aboard SOHO. Energy
  spectra of protons, deuterons, 3He and 4He nuclei have been obtained
  during very low activity periods in 1996-97 in the energy range of 1.3
  to 22 MeV/n. The proton spectra are comparable to the lowest spectra
  of the Ulysses (COSPIN/LET, 1996) and near-Earth IMP-8 (1985-87)
  measurements. Deuterons and 3He are only significantly seen above about
  10 MeV/n, their spectra are consistent with an increase proportional
  to kinetic energy, expected for purely galactic origin.

---------------------------------------------------------
Title: Latitudinal and radial variation of &gt;2 GeV/n protons and
α-particles in the northern heliosphere: ulysses cospin/ket and
    neutron monitor network observations
Authors: Belov, A. V.; Eroshenko, E. A.; Heber, B.; Yanke, V. G.;
   Ferrando, P.; Raviart, A.; Bothmer, V.; Dröge, W.; Kunow, H.;
   Müller-Mellin, R.; Röhrs, K.; Wibberenz, G.; Paizis, C.
1999AdSpR..23..443B    Altcode:
  Ulysses, launched in October 1990, crossed in December 1997
  the heliographic equator and completed its first out of ecliptic
  orbit. During the time period from February 1995 to November 1997 solar
  activity was low and the spacecraft scanned the latitude range from 80°
  N to the heliographic equator. The Kiel Electron Telescope on-board
  Ulysses measures protons and α-particles in the energy range from 5
  MeV/n to &gt; 2 GeV/n. To separate spatial and temporal variations of
  &gt; 2 GeV/n protons and α-particles along the spacecraft trajectory
  we used the data set from the world wide neutron monitor network. We
  found negligible latitudinal gradients below ~29° N and for the radial
  gradient an upper limit of ≈ 0.5 %/AU for &gt; 2 GeV/n protons and
  α-particles. In the latitudinal range from ≈ 25 to &gt; 70° N the
  latitudinal gradient is ~0.17 %/° and ~0.12 %/° for &gt; 2 GeV/n
  protons and α-particles, respectively, independent of spacecraft
  latitude and radial distance.

---------------------------------------------------------
Title: Observation of a ~ 7 MeV Electron Super-flux at 5 AU by Ulysses
Authors: Ferrando, Philippe; Raviart, A.; Heber, B.; Bothmer, V.;
   Kunow, H.; Muller-Mellin, R.; Paizis, C.
1999ICRC....7..135F    Altcode: 1999ICRC...26g.135F
  From the Ulysses launch up to the end of 1995, the 4-10 MeV energy
  electron count rate of the COSPIN/KET instrument has been consistent
  with simple expectations from Jovian electrons propagation. From the
  beginning of 1996 to the end of 1998, Ulysses was below ~ 30 degrees
  of heliographic latitude and between 4.5 and 5.4 AUs from the Sun,
  making it the first spacecraft to reach the region around the Jupiter
  orbit but with the planet being very far away. During this period,
  this electron flux around 7 MeV has surprisingly increased and has
  stayed at a high level up to the latest data of early 1999. In this
  paper, we present these data and discuss the possible origin of this
  electron super-flux, which reaches a level similar to that obtained
  in 1991 when Ulysses was perfectly magnetically connected to Jupiter.

---------------------------------------------------------
Title: Charge sign dependent modulation: Ulysses COSPIN/KET results
Authors: Heber, Bernd; Ferrando, P.; Raviart, A.; Wibberenz, G.;
   Paizis, C.; Bothmer, V.; Kunow, H.; Muller-Melin, R.; Posner, A.;
   Sierks, H.; Potgieter, M. S.
1999ICRC....7...99H    Altcode: 1999ICRC...26g..99H
  According to drift dominated modulation models galactic cosmic
  ray protons and electrons respond differently to the latitudinal
  extension of the heliospheric current sheet. In an A 0 solar magnetic
  cycle intensities of ¥ positively charged particles should vary only
  weakly with the latitudinal extension, whereas electrons should show
  a much stronger response. In this paper we investigate the charge sign
  dependent modulation in the 1990s using measurements of 2.5 GV protons
  and electrons of the Cosmic and Solar Particle Investigation Kiel
  Electron Telescope (COSPIN/KET) on board Ulysses from the beginning of
  1992 to the end of 1998. Only close to solar minimum, when the maximum
  latitudinal extend is below 30 , differences in the temporal variation
  of electrons and protons are observed.

---------------------------------------------------------
Title: The Solar Origin of Corotating Interaction Regions and their
    Formation in the Inner Heliosphere
Authors: Balogh, A.; Bothmer, V.; Crooker, N. U.; Forsyth, R. J.;
   Gloeckler, G.; Hewish, A.; Hilchenbach, M.; Kallenbach, R.; Klecker,
   B.; Linker, J. A.; Lucek, E.; Mann, G.; Marsch, E.; Posner, A.;
   Richardson, I. G.; Schmidt, J. M.; Scholer, M.; Wang, Y. -M.;
   Wimmer-Schweingruber, R. F.; Aellig, M. R.; Bochsler, P.; Hefti, S.;
   Mikić, Z.
1999cir..book..141B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Amplitude evolution and rigidity dependence of the 26-day
recurrent cosmic ray decreases: COSPIN/KET results
Authors: Paizis, C.; Heber, B.; Ferrando, P.; Raviart, A.; Falconi, B.;
   Marzolla, S.; Potgieter, M. S.; Bothmer, V.; Kunow, H.; Müller-Mellin,
   R.; Posner, A.
1999JGR...10428241P    Altcode:
  In the time interval extending from July 1992 to July 1994, Ulysses
  climbed from 10°S heliographic latitude up to over 70°S. During this
  time lapse, solar minimum conditions were gradually approached, which,
  in turn, led to stable and long-lasting corotating interaction regions
  (CIRs). The corotating particle events observed during this period,
  associated with ~30 registered CIRs, offer a unique opportunity to
  probe the three-dimensional structures of the heliosphere. In this work
  we use data from the Cosmic Ray and Solar Particle Investigation Kiel
  Electron Telescope (COSPIN/KET) instrument on board Ulysses to study
  the amplitude evolution of the 26-day recurrent cosmic ray decreases,
  generated by these CIRs, at different energies and derive its rigidity
  dependence. We find that the amplitude has a maximum around 25°-30°
  heliolatitude. We also find that the rigidity dependence of both the
  latitudinal gradient as well as the 26-day variation amplitude show
  a remarkable similarity. We discuss these observations within the
  framework of our current understanding of heliospheric phenomena.

---------------------------------------------------------
Title: The solar energetic particle event of April 14, 1994, as a
    probe of shock formation and particle acceleration
Authors: Kahler, S. W.; Cane, H. V.; Hudson, H. S.; Kurt, V. G.;
   Gotselyuk, Y. V.; MacDowall, R. J.; Bothmer, V.
1998JGR...10312069K    Altcode:
  Gradual solar energetic particle (SEP) events observed at 1 AU are
  associated with coronal mass ejections (CME) that drive shocks which
  are presumed to accelerate the ions and electrons to suprathermal
  energies. However, high-energy (&gt;30 MeV) proton and (&gt;1 MeV)
  electron events are nearly always associated with both CMEs and flares,
  suggesting that the acceleration of those particles, particularly
  the electrons, could be attributed to the associated flares. Only one
  clear example of a high-energy SEP event without an active region flare
  association has been reported previously. We discuss a second such SEP
  event, on April 14, 1994, associated with a well-observed solar X ray
  arcade structure spanning ~150° of solar longitude. The SEP event,
  observed by detectors on the IMP 8 and Koronas I spacecraft, began
  ~10 hrs after the beginning of the X ray event and was temporally
  and spatially associated with the last of three weak interplanetary
  type III radio bursts observed by the Ulysses low-frequency radio
  experiment. The delayed onset and rapid rise of the SEP intensities
  preclude a recent interpretation in which SEPs were presumed to be
  accelerated by a shock driven by a CME which erupted at the onset of
  the X ray event. Yohkoh soft X ray subtracted images show a large-scale
  arcade brightening west of ~E10° beginning about 8 hours after the
  initial brightening near the east limb. We suggest that the April 14
  SEP event at Earth was produced by a shock driven by a CME associated
  with the later brightening near central meridian. The initial X ray
  brightening may also have been associated with an earlier CME.

---------------------------------------------------------
Title: Latitudinal distribution of &gt;106MeV protons and its
    relation to the ambient solar wind in the inner southern and northern
heliosphere: Ulysses Cosmic and Solar Particle Investigation Kiel
    Electron Telescope results
Authors: Heber, B.; Bothmer, V.; Dröge, W.; Kunow, H.; Müller-Mellin,
   R.; Sierks, H.; Wibberenz, G.; Ferrando, P.; Raviart, A.; Paizis,
   C.; Potgieter, M. S.; Burger, R. A.; Hattingh, M.; Haasbroek, L. J.;
   McComas, D.
1998JGR...103.4809H    Altcode:
  We present observations and model calculations of the modulated
  intensities of galactic cosmic ray protons above 106 MeV/n along the
  Ulysses trajectory. Data are taken by the Cosmic and Solar Particle
  Investigation (COSPIN) Kiel Electron Telescope (KET) from spring 1993
  to fall 1996. During this time period solar activity decreased and
  galactic cosmic rays recovered. To separate spatial from temporal
  variations we used the University of Chicago measurements from IMP
  8 near Earth and compare the residual spatial variation with time
  independent modulation models. According to standard drift dominated
  modulation model, one would expect a radial gradient of ~2%/AU and
  a latitudinal gradient of ~1.2%/degree in both hemispheres. The
  measured mean radial gradient of ~3%/AU is within the uncertainties
  in good agreement with the model predictions. However, the measured
  mean latitudinal gradient has a value of (0.33+/-0.04)%/degree in
  both hemispheres at intermediate latitudes and is by a factor of 4
  lower than expected. In the modified models the latitudinal gradient
  is in agreement with the measured ones when we increase the diffusion
  coefficient κ<SUB>θθ</SUB> perpendicular to the magnetic field in
  polar direction to a value of 15% of the diffusion coefficient parallel
  to the magnetic field. The latitudinal gradients &gt;106MeV protons
  calculated by modified modulation models are in very good agreement
  with the measured ones at intermediate latitudes. At lower latitudes,
  when Ulysses is embedded in the streamer belt, the models predict
  approximately the same latitudinal gradient than at intermediate
  latitudes, whereas the measured ones are significant smaller, or
  even vanishing. The observations support the previous conclusion
  from Paizis et al. [1995] that a significant latitudinal gradient
  is only observed when Ulysses is outside the streamer belt. Another
  remarkable observation is the difference of the radial gradient
  G<SUB>r</SUB> at ~3.5AU in the southern (G<SUB>r</SUB>~3.5%/AU) and in
  the northern hemisphere (G<SUB>r</SUB>~2.3%/AU). Probable reasons for
  the significantly lower radial gradient in the northern hemisphere can
  be either a spatial asymmetry of the heliosphere or temporal variations.

---------------------------------------------------------
Title: Acceleration in Energetic Ions (~1 MeV) in Corotating
    Interaction Regions
Authors: Desai, M. I.; Bothmer, V.; Marsden, R. G.; Sanderson, T. R.;
   Balogh, A.; Forsyth, R. J.; Goldstein, B. E.
1998paac.conf..555D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: European Plans for the Solar/Heliospheric Stereo Mission
Authors: Bothmer, V.; Bougeret, J. -L.; Cargill, P.; Davila, J.;
   Delaboudiniere, J. -P.; Harrison, R.; Koutchmy, S.; Liewer, P.;
   Maltby, P.; Rust, D.; Schwenn, R.
1998ESASP.417..145B    Altcode: 1998cesh.conf..145B
  No abstract at ADS

---------------------------------------------------------
Title: Acceleration in energetics ions (~1MeV) in corotating
    interaction regions
Authors: Desai, M. I.; Bothmer, V.; Marsden, R. G.; Sanderson, T. R.;
   Balogh, A.; Forsyth, R. J.; Goldstein, B. E.
1998AdSpR..21..555D    Altcode:
  We have correlated the ~1 MeV proton intensity (J) measured at
  corotating reverse shocks detected by Ulysses near the ecliptic plane
  and in the southern hemisphere with the shock strength and shock
  normal angle. We find that J is essentially independent of the shock
  strength below 29 degS, whereas between 29 deg and 41 degS J showed
  a good correlation with the same. The poor correlation below 29 degS
  is attributed to temporal variations in the background intensity
  and to the presence of particles accelerated at other corotating and
  transient shocks. J is also independent of the shock normal angle at all
  latitudes, which is probably due to the combined effects of the drift
  and diffusive acceleration processes. We compensate for the effects
  of variations in the background by assuming that two reverse shocks
  observed during the same ~26 day period accelerate particles out of
  the same background population. By correlating the ratio of the proton
  intensities with the ratios of the shock parameters for such pairs of
  reverse shocks, we show that the shock acceleration efficiency is well
  correlated with the strength but is independent of the normal angle.

---------------------------------------------------------
Title: The structure and origin of magnetic clouds in the solar wind
Authors: Bothmer, V.; Schwenn, R.
1998AnGeo..16....1B    Altcode: 1998AnG....16....1B
  Plasma and magnetic field data from the Helios 1/2 spacecraft have
  been used to investigate the structure of magnetic clouds (MCs) in the
  inner heliosphere. 46 MCs were identified in the Helios data for the
  period 1974-1981 between 0.3 and 1 AU. 85% of the MCs were associated
  with fast-forward interplanetary shock waves, supporting the close
  association between MCs and SMEs (solar mass ejections). Seven MCs
  were identified as direct consequences of Helios-directed SMEs, and
  the passage of MCs agreed with that of interplanetary plasma clouds
  (IPCs) identified as white-light brightness enhancements in the Helios
  photometer data. The total (plasma and magnetic field) pressure in MCs
  was higher and the plasma-&lt;beta&gt; lower than in the surrounding
  solar wind. Minimum variance analysis (MVA) showed that MCs can best be
  described as large-scale quasi-cylindrical magnetic flux tubes. The axes
  of the flux tubes usually had a small inclination to the ecliptic plane,
  with their azimuthal direction close to the east-west direction. The
  large-scale flux tube model for MCs was validated by the analysis
  of multi-spacecraft observations. MCs were observed over a range
  of up to ~60° in solar longitude in the ecliptic having the same
  magnetic configuration. The Helios observations further showed that
  over-expansion is a common feature of MCs. From a combined study of
  Helios, Voyager and IMP data we found that the radial diameter of MCs
  increases between 0.3 and 4.2 AU proportional to the distance, R, from
  the Sun as R0.8 (R in AU). The density decrease inside MCs was found to
  be proportional to R-2.4, thus being stronger compared to the average
  solar wind. Four different magnetic configurations, as expected from
  the flux-tube concept, for MCs have been observed in situ by the Helios
  probes. MCs with left- and right-handed magnetic helicity occurred
  with about equal frequencies during 1974-1981, but surprisingly,
  the majority (74%) of the MCs had a south to north (SN) rotation of
  the magnetic field vector relative to the ecliptic. In contrast, an
  investigation of solar wind data obtained near Earth's orbit during
  1984-1991 showed a preference for NS-clouds. A direct correlation
  was found between MCs and large quiescent filament disappearances
  (disparition brusques, DBs). The magnetic configurations of the
  filaments, as inferred from the orientation of the prominence axis,
  the polarity of the overlying field lines and the hemispheric helicity
  pattern observed for filaments, agreed well with the in situ observed
  magnetic structure of the associated MCs. The results support the model
  of MCs as large-scale expanding quasi-cylindrical magnetic flux tubes in
  the solar wind, most likely caused by SMEs associated with eruptions of
  large quiescent filaments. We suggest that the hemispheric dependence
  of the magnetic helicity structure observed for solar filaments can
  explain the preferred orientation of MCs in interplanetary space as
  well as their solar cycle behavior. However, the white-light features
  of SMEs and the measured volumes of their interplanetary counterparts
  suggest that MCs may not simply be just H&lt;alpha&gt;-prominences,
  but that SMEs likely convect large-scale coronal loops overlying the
  prominence axis out of the solar atmosphere.

---------------------------------------------------------
Title: Development of Coronal Mass Ejections and Association with
    Interplanetary Events
Authors: Pick, M.; Maia, D.; Howard, R.; Thompson, B.; Lanzerotti,
   L. J. L.; Bothmer, V.; Lamy, P.
1997ESASP.415..195P    Altcode: 1997cpsh.conf..195P
  No abstract at ADS

---------------------------------------------------------
Title: Solar Energetic Particle Events and Coronal Mass Ejections:
    New Insights from SOHO
Authors: Bothmer, V.; Posner, A.; Kunow, H.; Müller-Mellin, R.;
   Herber, B.; Pick, M.; Thompson, B. J.; Delaboudinière, J. -P.;
   Brueckner, G. E.; Howard, R. A.; Michels, D. J.; Cyr, C. St.; Szabo,
   A.; Hudson, H. S.; Mann, G.; Classen, H. -T.; McKenna-Lawlor, S.
1997ESASP.415..207B    Altcode: 1997cpsh.conf..207B
  No abstract at ADS

---------------------------------------------------------
Title: Fluxes of MeV Particles at Earth's Orbit and their Relationship
with the Global Structure of the Solar Corona: Observations from SOHO
Authors: Posner, A.; Bothmer, V.; Kunow, H.; Herber, B.;
   Müller-Mellin, R.; Delaboudinière, J. -P.; Thompson, B. J.;
   Brückner, G. E.; Howard, R. A.; Muchels, D. J.
1997ESASP.415..377P    Altcode: 1997cpsh.conf..377P
  No abstract at ADS

---------------------------------------------------------
Title: The Solar Energetic Particle Event of 14 April 1994 as a
    Probe of Shock Formation and Particle Acceleration
Authors: Kahler, S. W.; Cane, H. V.; Hudson, H. S.; Kurt, V. G.;
   MacDowall, R. J.; Bothmer, V.
1997AAS...191.7412K    Altcode: 1997BAAS...29.1326K
  Gradual solar energetic particle (SEP) events observed at 1 AU are
  associated with coronal mass ejections (CMEs) that drive shocks which
  accelerate the ions and electrons to suprathermal energies. However,
  high energy (&gt; 30 MeV) proton and (&gt; 1 MeV) electron events are
  nearly always associated with both CMEs and flares, suggesting that
  the acceleration of those particles, particularly the electrons, could
  be attributed to the associated flares. Only one clear example of a
  high energy SEP event without a flare association has been reported
  previously. We discuss a second such SEP event, on 14 April 1994,
  associated with a well observed solar X-ray arcade structure spanning ~
  150deg of solar longitude. The SEP event, observed by detectors on the
  IMP-8 and Koronas-I space craft, began about 10 hrs after the beginning
  of the X-ray event and was temporally and spatially associated with
  the last of three weak interplanetary type III radio bursts observed
  by the Ulysses low frequency radio experiment. The delayed onset and
  rapid rise of the SEP intensities preclude a recent interpretation in
  which SEPs were accelerated by a shock driven by a CME which erupted
  at the onset of the X-ray event. Yohkoh soft X-ray subtracted images
  show a large-scale arcade brightening west of ~ E10deg beginning about 8
  hours after the initial brightening near the east limb. We suggest that
  the 14 April event consisted of at least two CMEs with progressively
  westward source regions and that the SEP event was produced in a second
  shock driven by a later CME.

---------------------------------------------------------
Title: Spatial Evolution of 26-day Recurrent Galactic Cosmic Ray
Decreases: Correlated Ulysses COSPIN/KET and SOHO COSTEP Observations
Authors: Heber, B.; Bothmer, V.; Dröge, W.; Kunow, H.; Müller-Mellin,
   R.; Posner, A.; Ferrando, P.; Raviart, A.; Raviart, A.; Paizis, C.;
   McComas, D.; Forsyth, R. J.; Szabo, A.; Lazarus, A. J.
1997ESASP.415..331H    Altcode: 1997cpsh.conf..331H
  No abstract at ADS

---------------------------------------------------------
Title: Search for the Origin of Quiet-Time Particle Fluxes in the
    Inner Heliosphere
Authors: Kiraly, P.; Bothmer, V.; Kecskemety, K.; Keppler, E.;
   Kudela, K.; Kunow, H.; Logachev, Yu. I.; sMüller-Mellin, R.;
   Rodriguez-Pacheco, J.; von Steiger, R.; Torsti, J.; Valtonen, E.;
   Zeldovich, M. A.
1997ICRC....2..477K    Altcode: 1997ICRC...25b.477K
  No abstract at ADS

---------------------------------------------------------
Title: The Effects of Coronal Mass Ejections on Galactic Cosmic
Rays in the High Latitude Heliosphere: Observations from Ulysses'
    First Orbit
Authors: Bothmer, V.; Heber, B.; Kunow, H.; Mueller-Mellin, R.;
   Wibberenz, G.
1997ICRC....1..333B    Altcode: 1997STIN...9928408B
  During its first solar orbit, the Ulysses spacecraft detected several
  coronal mass ejections (CMEs) at high heliographic latitudes. The
  authors present first observations on the effects of these high latitude
  CMEs on galactic cosmic rays (GCRs) using measurements from the Kiel
  Electron Telescope (KET) which is part of the Cosmic Ray and Solar
  Particle Investigation (COSPIN) experiment, the Los Alamos SWOOPS
  (Solar Wind Observations Over the Poles of the Sun) experiment and
  the magnetic field experiments. They find the passage of these CMEs
  over the spacecraft to be associated with short term decreases of GCR
  intensities The relatively weak shocks in these events, driven by
  the CMEs' over-expansion, had no strong influence on the GCRs. The
  intensity minimums of GCRs occurred on closed magnetic field lines
  inside the CMEs themselves as indicated by bidirectional fluxes of
  suprathermal electrons. Short episodes of intensity increases of GCRs
  inside CMEs at times when the bidirectional fluxes of suprathermal
  electrons disappeared, can be interpreted as evidence that GCRs can
  easily access the interior of those CMEs in which open magnetic field
  lines are embedded.

---------------------------------------------------------
Title: Time and Energy Dependence of 26-Day Recurrent Decreases
    of &gt;100 MeV Protons in the Inner Southern Heliosphere and its
Correlation to Latitudinal Gradients: Ulysses COSPIN/KET Results
Authors: Kunow, H.; Heber, B.; Raviart, A.; Paizis, C.; Bothmer, V.;
   Droege, W.; Schmidt, J.
1997ICRC....1..381K    Altcode: 1997ICRC...25a.381K
  No abstract at ADS

---------------------------------------------------------
Title: Evolution of Cosmic Ray Electron Spectra above 350 MeV along
    the Ulysses Trajectory
Authors: Raviart, A.; ferrando, P.; Heber, B.; Paizis, C.; Bothmer,
   V.; Dröge, W.; Kunow, H.; Müller-Mellin, R.; Wibberenz, G.
1997ICRC....2...37R    Altcode: 1997ICRC...25b..37R
  No abstract at ADS

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Title: EPHIN Observations of Energetic Particles during Solar Minimum
Authors: Müller-Mellin, R.; Bothmer, V.; Kunow, H.; Posner, A.;
   Sierks, H.; Sequeiros, J.; del Peral, L.; Rodriguez-Frias, M. D.;
   Potgieter, M.; Haasbroek, L.
1997ICRC....1..301M    Altcode: 1997ICRC...25a.301M
  No abstract at ADS

---------------------------------------------------------
Title: Development and Effects of Corotating Interaction Regions:
    Workshop Report
Authors: Kunow, H.; Bothmer, V.
1997ICRC....1..357K    Altcode: 1997ICRC...25a.357K
  No abstract at ADS

---------------------------------------------------------
Title: Joint ULYSSES and WIND observations of a particle event in
    April 1995.
Authors: Buttighoffer, A.; Pick, M.; Raviart, A.; Hoang, S.; Lin,
   R. P.; Simnett, G. M.; Lanzerotti, L. J.; Bothmer, V.
1996A&A...316..499B    Altcode:
  In this paper we analyze a solar particle event that was measured
  at two locations in the heliosphere. Ulysses was at 40°north
  heliolatitude and 130°west in heliolongitude from Earth while WIND
  was near Earth at 1 AU in the ecliptic plane. To establish the origin
  of the particle events, solar coronal activity is investigated. Direct
  observational evidence of the association between long-duration electron
  acceleration and a solar radio noise storm is shown. We also establish
  that the interplanetary type III burst studied here is produced by
  successive electron injections from distinct coronal locations. Two
  particle increases are observed during the event. For the first one,
  the particles are shown to be from coronal origin; for the second one,
  which is associated with a Forbush decrease, the particles are primarily
  shock accelerated. The differences in particle intensities observed at
  WIND and Ulysses are explained by the nature of the particle propagation
  to the spacecraft locations.

---------------------------------------------------------
Title: ULYSSES COSPIN/LET: latitudinal gradients of anomalous cosmic
    ray O, N and Ne.
Authors: Trattner, K. J.; Marsden, R. G.; Bothmer, V.; Sanderson,
   T. R.; Wenzel, K. -P.; Klecker, B.; Hovestadt, D.
1996A&A...316..519T    Altcode:
  A key goal of the Ulysses mission is the measurement of the latitudinal
  gradient of the Anomalous Cosmic Ray (ACR) component. Earlier studies
  using data from the COSPIN/LET experiment on board Ulysses together
  with in-ecliptic data from the HILT instrument on SAMPEX have shown
  a small (~2% per degree) positive latitudinal gradient for anomalous
  oxygen in the energy range 8 to 16MeV/n. This result is consistent
  with the effects of curvature and gradient drifts in the heliospheric
  magnetic field for the current polarity configuration: positively
  charged particles are expected to flow down to the heliographic equator
  from the polar regions. In this paper we extend our previous work and
  include two additional ACR species, nitrogen (4 to 20MeV/n) and neon
  (4 to 30MeV/n). We also present our latest results on the ACR oxygen
  latitudinal gradient over an extended energy range (4 to 20MeV/n). The
  period covered for all three species include the Ulysses south polar
  pass, the rapid transit from the south pole to the ecliptic and a
  significant portion of the climb to high northern latitudes. For all
  species and energy ranges the latitudinal gradients are between 1%
  and 2%, consistent with earlier studies, and show a slight tendency
  to larger gradients for higher magnetic rigidity.

---------------------------------------------------------
Title: ULYSSES observations of open and closed magnetic field lines
    within a coronal mass ejection.
Authors: Bothmer, V.; Desai, M. I.; Marsden, R. G.; Sanderson, T. R.;
   Trattner, K. J.; Wenzel, K. -P.; Gosling, J. T.; Balogh, A.; Forsyth,
   R. J.; Goldstein, B. E.
1996A&A...316..493B    Altcode:
  During the rapid passage from the Sun's south to north polar regions,
  the Ulysses spacecraft encountered in February 1995, at 24°S, a coronal
  mass ejection (CME) exactly at the time when it crossed from high speed
  solar wind coronal hole flow into low speed streamer belt flows. We have
  investigated this CME, which was superimposed on an energetic particle
  event associated with a corotating interaction region (CIR), using
  energetic particle, plasma and magnetic field measurements. Ulysses'
  entry into the CME was accompanied by a strong decrease in the intensity
  of 1-3MeV protons. The leading portion of the CME with a helical
  magnetic flux rope topology characteristic of magnetic clouds apparently
  consisted of closed magnetic loops as indicated by counterstreaming
  suprathermal electron fluxes along the interplanetary magnetic field
  (IMF) and bi-directional streaming 0.4-0.7MeV ions. In contrast, the
  absence of counterstreaming electrons and ions, the presence of sunward
  streaming 0.4-5MeV ions and sunward bursts of suprathermal electrons
  at energies from ~40eV up to several 100eV inside another portion of
  the CME suggest that here the magnetic field lines were "open" i.e.,
  with only one end rooted in the solar corona. These field lines were
  most likely connected to the reverse shock of a CIR beyond Ulysses. We
  suggest that 3-dimensional reconnection processes are responsible for
  the formation of magnetic flux rope CMEs from rising coronal loops
  leading to open and closed field topologies.

---------------------------------------------------------
Title: Ulysses observations of energetic ions over the south pole
    of the sun
Authors: Sanderson, T. R.; Bothmer, V.; Marsden, R. G.; Trattner,
   K. J.; Wenzel, K. -P.; Balogh, A.; Forsyth, R. J.; Goldstein, B. E.
1996AIPC..382..411S    Altcode:
  We present here observations of energetic ions during the following
  phases of the Ulysses prime mission: the first south polar pass,
  the low-latitude pass and part of the first north polar pass. Peaks
  are observed in the energetic ion intensity which recur either once
  per solar rotation during the ascent to high southern latitudes,
  or twice per rotation during the low latitude pass. The intensity
  of the peaks also rises with each major solar event, decaying slowly
  thereafter over a period of several rotations. The peaks are observed
  up to ~70° during the ascent to high southern latitudes, but not seen
  again until around 45° during the descent, this asymmetry most likely
  being caused by a decrease in the number of solar events.

---------------------------------------------------------
Title: Energetic particles and coronal mass ejections in the high
latitude heliosphere: Ulysses-LET observations
Authors: Bothmer, V.; Marsden, R. G.; Sanderson, T. R.; Trattner,
   K. J.; Wenzel, K. -P.; Balogh, A.; Forsyth, R. J.; Goldstein, B. E.;
   Uchida, Y.; Hudson, H. S.
1996AIPC..382..445B    Altcode:
  We have investigated energetic ions of non-corotating nature in the high
  latitude heliosphere. Major particle events were observed by Ulysses up
  to latitudes of 60 °S. All were associated with passage of coronal mass
  ejections (CMEs) over the spacecraft. The relationship of these events
  with solar activity was investigated using Yohkoh soft X-ray images.

---------------------------------------------------------
Title: Signatures of fast CMEs in interplanetary space
Authors: Bothmer, V.; Schwenn, R.
1996AdSpR..17d.319B    Altcode: 1996AdSpR..17..319B
  While fast coronal mass ejections (CMEs) have been uniquely identified
  as sources of transient shock-disturbances in interplanetary space,
  it is less understood why different kinds of plasma and magnetic field
  signatures are found in the individual post-shock flows. It is an
  open question if CMEs can produce various types of solar wind ejecta,
  e.g. magnetic flux ropes or flows without highly ordered internal
  fields. To help further clarify the consequences of fast CMEs in
  interplanetary space we have examined shock events measured by the
  Helios 1 spacecraft during the years 1979-1981 for which the associated
  CME has been directly observed with the coronagraph onboard the P78/1
  satellite. Seventeen (68%) out of 25 shock-disturbances were followed
  by clearly discernible driver gas signatures, but only 7 (41%) of the
  driver gases were magnetic clouds.

---------------------------------------------------------
Title: Stereoscopic viewing of solar coronal and interplanetary
    activity
Authors: Schmidt, W. K. H.; Bothmer, V.
1996AdSpR..17d.369S    Altcode: 1996AdSpR..17..369S
  The object of this presentation is to propose a concept for a space
  mission that would facilitate stereoscopic observations of the sun and
  interplanetary space, and to outline its scientific objectives. It is
  envisaged to place a spacecraft with a few lightweight telescopes,
  covering the wavelength range from the visible to the extreme UV,
  into orbit around the triangular libration point L5 of the sun-earth
  system. This point is also known as one of the Lagrangian points,
  which is in earth orbit around the sun, and lagging the sun-earth line
  by 60 degrees. A satellite (or perhaps more than one) with similar
  instrumentation is assumed to operate simultaneously in near earth
  orbit. Together, these observations would allow three dimensional
  viewing of the sun and interplanetary space. One of the main subjects
  of investigation would be to study the morphology and dynamics of
  coronal plasma structures and their extension into interplanetary
  space. Coronal structures would be imaged in EUV and soft X rays, while
  interplanetary events such as Coronal Mass Ejections (CMEs) and shock
  waves would be seen as density enhancements in white light. CMEs could
  be tracked from their start in the solar corona until their arrival
  and impact on the earth's magnetosphere. Thus the observations could
  also be used to predict major geomagnetic storms.

---------------------------------------------------------
Title: The Ulysses south polar pass: Transient fluxes of energetic
    ions
Authors: Bothmer, V.; Marsden, R. G.; Sanderson, T. R.; Trattner,
   K. J.; Wenzel, K. -P.; Balogh, A.; Forsyth, R. J.; Goldstein, B. E.
1995GeoRL..22.3369B    Altcode:
  Using Ulysses low energy telescope (LET) measurements of protons
  and alpha particles with energies of ∼1-5 MeV/n, we present first
  observations of transient energetic particle events in the high latitude
  heliosphere. Three transient particle events with gradual onsets and
  time durations of several days have been identified in the LET data
  at heliographic latitudes as high as ∼60°S, at radial distances
  from the Sun between 3.3-3.6 AU. No transient increases were observed
  polewards of 60°S. All three of the events were associated with
  passage of a coronal mass ejection (CME) over Ulysses, and two were
  associated with the newly identified type of forward/reverse shock
  pairs in the solar wind caused by over-expanding CMEs. The largest of
  the three transient events has also been observed at Earth's orbit,
  i.e. in the ecliptic. The observations show that energetic particles
  can be convected into the high latitude heliosphere through CMEs.

---------------------------------------------------------
Title: The Ulysses south polar pass: Anomalous component of cosmic
    rays
Authors: Trattner, K. J.; Marsden, R. G.; Bothmer, V.; Sanderson,
   T. R.; Wenzel, K. -P.; Klecker, B.; Hovestadt, D.
1995GeoRL..22.3349T    Altcode:
  We have expanded our previous study of latitudinal gradients of
  anomalous cosmic ray oxygen (8 to 12 MeV/n and 12 to 16 MeV/n) by
  using also helium (11 to 20 MeV/n) as an additional component and a
  larger ULYSSES/LET data set including the segment up to the maximum
  southern latitude and the pole-to-equator segment of the mission down
  to 38°S. The ULYSSES observations are compared with observations
  in the vicinity of the Earth, provided by SAMPEX and IMP 8. The data
  sets cover a time period from August 1992 to end of January 1995. Only
  quiet time periods which contain no increases due to solar energetic
  particles are taken into account. Both oxygen energy channels show a
  decrease of the SAMPEX to ULYSSES flux ratio which is equivalent to a
  positive latitudinal gradient of ∼2%/degree. However, no significant
  latitudinal gradient for helium was found using the IMP 8 to ULYSSES
  flux ratio.

---------------------------------------------------------
Title: The Ulysses south polar pass: Energetic ion observations
Authors: Sanderson, T. R.; Bothmer, V.; Marsden, R. G.; Trattner,
   K. J.; Wenzel, K. -P.; Balogh, A.; Forsyth, R. J.; Goldstein, B. E.
1995GeoRL..22.3357S    Altcode:
  We present here a preliminary analysis of observations of energetic ions
  during the first polar pass of the Ulysses spacecraft, concentrating
  mainly on the region where the spacecraft was continually immersed
  in high speed flow from the polar coronal hole. During the ascent to
  high latitudes, a single recurrent peak was observed once per solar
  rotation. From 70°S during ascent to 43°S during descent no major
  peaks were observed. Thereafter, two peaks per solar rotation were
  observed.

---------------------------------------------------------
Title: Energetic particles and coronal mass ejections in the high
latitude heliosphere: Ulysses-LET observations
Authors: Bothmer, V.; Sanderson, T. R.; Marsden, R. G.; Wenzel,
   K. -P.; Goldstein, B. E.; Balogh, A.; Forsyth, R. J.; Uchida, Y.
1995sowi.conf...47B    Altcode:
  The COSPIN Low Energy Telescope (LET) onboard the Ulysses spacecraft
  measures protons, alphas and heavier ions at energies of approximately
  1 to 50 MeV/n. Ulysses measurements offer favorable opportunities to
  study the effects of solar activity in the out-of-ecliptic regions of
  the heliosphere. Using LET data, we have investigated the properties of
  transient energetic ions at high heliographic latitudes when Ulysses
  was permanently immersed in high speed solar wind and magnetically
  connected to the Sun on open magnetic field lines. Recurrent increases
  in the fluxes of energetic ions at high heliographic latitudes at
  frequencies related to the solar rotation period were found to occur
  in association with co-rotating interaction regions (CIRs). Here we
  investigate fluxes of energetic particles that showed no relationship
  to ClRs. From the investigation of plasma and magnetic held data it
  is found that all of the transient high latitude particle events
  were associated with the passage of a coronal mass ejection (CME)
  over Ulysses. Enhancements in particle fluxes several days prior to
  the arrival of a CME, but with a significant time delay with respect
  to the estimated CME-onset at the Sun, were most probably associated
  with interplanetary shocks driven by fast CMEs. These particle events
  exhibit unusually high rho/alpha-ratios and are not observed for
  CMEs not driving a shock. However, not all CMEs that passed Ulysses
  were associated with a particle event. We find evidence that at high
  solar latitudes, solar flare particles cannot reach Ulysses on open
  magnetic field lines, but can reach the spacecraft if particles are
  injected into magnetic flux-ropes (CMEs) at the Sun. These findings are
  supported by soft X-ray observations from the Japanese Yohkoh-satellite.

---------------------------------------------------------
Title: ULYSSES observations of energetic ions over the south pole
    of the Sun
Authors: Sanderson, T. R.; Marsden, R. G.; Bothmer, V.; Trattner,
   K. J.; Wenzel, K. P.; Balogh, A.; Forsyth, R. J.; Goldstein, B. E.
1995sowi.conf...44S    Altcode:
  The Ulysses spacecraft began its journey out-of-the-ecliptic in February
  of 1992, when it encountered the planet Jupiter. In April of 1993,
  the spacecraft had reached 29 deg S, and from then on was completely
  immersed in the flow from the southern polar coronal hole. Accelerated
  ions were observed, recurring with a main peak once per solar rotation,
  with the intensity at the peak slowly decreasing with increasing
  latitude. This decrease continued to the end of 1993, when the
  spacecraft was at approximately 50 deg S. During the first three months
  of 1994 the intensity of the accelerated ions rose again, due either
  to an increase in magnetic activity on the sun or a reconfiguration
  of the heliospheric magnetic field. Recurrent accelerated ions were
  still being seen at the beginning of July 1994, when the spacecraft
  was at a latitude of 70 deg S, although with reduced intensity. The
  accelerated ions were no longer seen at latitudes higher than 70 deg S,
  the ion intensity staying constant at around the cosmic ray background
  level. This continued on until the highest latitude reached, 80.2 deg
  S, on 13 September 1994. The spacecraft then began its journey back
  towards lower latitudes, a small increase in the particle intensity
  being observed at the end of October whilst at approximately 72 deg
  S, and thereafter no more increases until the end of 1994, when the
  spacecraft was at approximately 45 deg S. We present interpretations
  for this asymmetry in latitude dependence.

---------------------------------------------------------
Title: Cosmic Ray and Solar Particle Investigations Over the South
    Polar Regions of the Sun
Authors: Simpson, J. A.; Anglin, J. D.; Bothmer, V.; Connell, J. J.;
   Ferrando, P.; Heber, B.; Kunow, H.; Lopate, C.; Marsden, R. G.;
   McKibben, R. B.; Muller-Mellin, R.; Paizis, C.; Rastoin, C.; Raviart,
   A.; Sanderson, T. R.; Sierks, H.; Trattner, K. J.; Wenzel, K. -P.;
   Wibberenz, G.; Zhang, M.
1995Sci...268.1019S    Altcode:
  Observations of galactic cosmic radiation and anomalous component nuclei
  with charged particle sensors on the Ulysses spacecraft showed that
  heliospheric magnetic field structure over the south solar pole does
  not permit substantially more direct access to the local interstellar
  cosmic ray spectrum than is possible in the equatorial zone. Fluxes
  of galactic cosmic rays and the anomalous component increased as
  a result of latitude gradients by less than 50% from the equator
  to -80^circ. Thus, the modulated cosmic ray nucleon, electron, and
  anomalous component fluxes are nearly spherically symmetric in the
  inner solar system. The cosmic rays and the anomalous nuclear component
  underwent a continuous, ~26 day recurrent modulation to -80.2^circ,
  whereas all recurring magnetic field compressions and recurring streams
  in the solar wind disappeared above ~55^circS latitude.

---------------------------------------------------------
Title: Eruptive prominences as sources of magnetic clouds in the
    solar wind
Authors: Bothmer, V.; Schwenn, R.
1994SSRv...70..215B    Altcode:
  Large amounts of coronal material are propelled outward into
  interplanetary space by Coronal Mass Ejections (CMEs). Thus one might
  expect to find evidence for expanding flux ropes in the solar wind
  as well. To prove this assumption magnetic clouds were analyzed and
  correlated with Hα-observations of disappearing filaments. When clouds
  were found to be directly associated with a disappearing filament,
  the magnetic structure of the cloud was compared with that of the
  associated filament. Additionally the expansion of magnetic clouds
  was examined over a wide range of the heliosphere and compared with
  the expansion observed for erupting prominences.

---------------------------------------------------------
Title: Comparison of CMEs, magnetic clouds, and bidirectionally
    streaming proton events in the heliosphere using helios data
Authors: Webb, D.; Jackson, B.; Hick, P.; Schwenn, R.; Bothmer, V.;
   Reames, D.
1993AdSpR..13i..71W    Altcode: 1993AdSpR..13...71W
  Coronal Mass Ejections (CMEs) are large, energetic expulsions of mass
  and magnetic fields from the Sun; they can significantly affect large
  volumes of the heliosphere and appear to be a key cause of geomagnetic
  storms. We have compiled a list of all significant CMEs detected by
  the HELIOS white light photometers from 1975-1982. We are studying the
  characteristics of these CMEs, and present preliminary results of their
  associations with in-situ features, especially magnetic “clouds” and
  periods of bidirectionally streaming ions, two classes of structures
  considered indicative of interplanetary loops. Advantages of this data
  set include reliable association in the interplanetary medium of the
  white light CME plasma with the in-situ features, and observations of
  a large number of events over a long time base.

---------------------------------------------------------
Title: Magnetic cloud observations by the HELIOS spacecraft
Authors: Bothmer, V.; Schwenn, R.
1992sws..coll..599B    Altcode:
  A possible interpretation for the observed characteristics of an
  interplanetary magnetic cloud is the passage of a magnetic flux
  rope. For simplification the flux rope might be considered as a
  cylindrically symmetric structure with the magnetic field lines being
  directed parallel to the axis at its center and circular at its outer
  edges. Near the center of this flux rope the magnetic field strength
  would be strongest. The minimum variance technique was applied to
  several magnetic clouds observed by the Helios spacecraft between 0.3
  and 1 AU in order to determine the orientations of the magnetic flux
  rope axis. The calculated orientations are examined with respect to the
  global solar wind stream structure, the surrounding solar wind flow,
  the radial distance to the sun and their solar origin.

---------------------------------------------------------
Title: Magnetic structures at sector boundaries in the inner
    heliosphere
Authors: Bothmer, V.; Schwenn, R.
1992sws..coll..151B    Altcode:
  The strong deflections of the IMF out of the ecliptic plane that
  have been noted at sector boundaries, and are therefore related to
  the heliospheric current sheet, have north-to-south turnings in the
  case of magnetic field deflections at sector boundaries that point
  to an origin for this phenomenon in magnetic field lines that remain
  parallel to the inclined current sheet. The plasma and magnetic field
  properties at sector boundaries closer to the sun may show interesting
  coronal streamer belt features.