Halo Coronal Mass Ejections and Configuration of the Ambient Magnetic Fields

Details Halo Coronal Mass Ejections and Configuration of the Ambient Magnetic Fields Halo Coronal Mass Ejections and Configuration of the Ambient Magnetic Fields

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh23b0350l&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH23B-0350

Physics

7513 Coronal Mass Ejections (2101), 7524 Magnetic Fields, 7599 General Or Miscellaneous

Scientific paper

This is a research following our previous work (Liu &Hayashi, 2006). In that work, we analyzed the fast halo Coronal Mass Ejections (CMEs) in 2003 October-November. We found that those CMEs were associated with special structures of the ambient magnetic fields, and we concluded that these magnetic configurations play an additional role in ensuring a high speed for those fast halo CMEs when they propagate through the heliosphere, while the related flares' characteristics may already define the CMEs' speeds in the first place. In this research, we examine whether this conclusion is held generally. Here, we classify halo CMEs into three types: CMEs occur under the heliospheric current sheet (type 1), in the open flux areas (type 2), and under the plasma sheet (type 3). The 2003 October-November fast halo CMEs are types 2 and 3. We studied 104 halo CMEs in the time interval from 2000 to 2004 from the SOHO LASCO CME CATALOG maintained by NASA and The Catholic University of America in cooperation with the Naval Research Laboratory, and conclude that (1) types 2 &3 halo CMEs appear to be faster than type 1 halo CMEs, which implies that the ambient magnetic field structure does play a role in determining the speeds of the halo CMEs, and (2) a weak correlation is found between the speed of type 3 CMEs and the peak of X-ray flux of the associated flares. We also place a discussion here. SOHO is a project of international cooperation between ESA and NASA.

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