|
|||||
|
|
An Ensemble Study of a January 2010 Coronal Mass Ejection (CME): Connecting a Non-obvious Solar Source with Its ICME/Magnetic Cloud |
|
| Authors: | D F Webb M M Bisi C A de Koning C J Farrugia B V Jackson L K Jian N Lugaz K Marubashi C Möstl E P Romashets B E Wood H-S Yu |
| Institution: | 1. ISR, Boston College, Chestnut Hill, MA, USA 2. RAL Space Science & Technology Facilities Council, Rutherford Appleton Laboratory, Harwell Oxford, Oxfordshire, England, UK 3. NOAA Space Weather Prediction Center and University of Colorado, CIRES, Boulder, CO, USA 4. Space Science Center & Department of Physics, University of New Hampshire, Durham, NH, USA 5. Center for Astrophysics and Space Science, University of California, San Diego, La Jolla, CA, USA 6. Heliophysics Science Division, Code 672, NASA Goddard Space Flight Center, Greenbelt, MD, USA 7. Department of Astronomy, University of Maryland, College Park, MD, USA 8. Korea Astronomy and Space Science Institute, Daejeon, Korea 9. Sayama, Saitama, 350-1317, Japan 10. Institute of Physics, University of Graz, 8010, Graz, Austria 11. Space Research Institute, Austrian Academy of Sciences, 8042, Graz, Austria 12. Lone Star College, 2700 West W. Thorne Drive, Houston, TX, USA 13. Space Science Division, Naval Research Laboratory, Washington, DC, USA |
| Abstract: | A distinct magnetic cloud (MC) was observed in-situ at the Solar TErrestrial RElations Observatory (STEREO)-B on 20?–?21 January 2010. About three days earlier, on 17 January, a bright flare and coronal mass ejection (CME) were clearly observed by STEREO-B, which suggests that this was the progenitor of the MC. However, the in-situ speed of the event, several earlier weaker events, heliospheric imaging, and a longitude mismatch with the STEREO-B spacecraft made this interpretation unlikely. We searched for other possible solar eruptions that could have caused the MC and found a faint filament eruption and the associated CME on 14?–?15 January as the likely solar source event. We were able to confirm this source by using coronal imaging from the Sun Earth Connection Coronal and Heliospheric Investigation (SECCHI)/EUVI and COR and Solar and Heliospheric Observatory (SOHO)/Large Angle and Spectrometric Coronograph (LASCO) telescopes and heliospheric imaging from the Solar Mass Ejection Imager (SMEI) and the STEREO/Heliospheric Imager instruments. We use several empirical models to understand the three-dimensional geometry and propagation of the CME, analyze the in-situ characteristics of the associated ICME, and investigate the characteristics of the MC by comparing four independent flux-rope model fits with the launch observations and magnetic-field orientations. The geometry and orientations of the CME from the heliospheric-density reconstructions and the in-situ modeling are remarkably consistent. Lastly, this event demonstrates that a careful analysis of all aspects of the development and evolution of a CME is necessary to correctly identify the solar counterpart of an ICME/MC. |
| Keywords: | |
| 本文献已被 SpringerLink 等数据库收录！ | |