October/November 2003 interplanetary coronal mass ejections: ACE/EPAM solar energetic particle observations

Details October/November 2003 interplanetary coronal mass ejections: ACE/EPAM solar energetic particle observations October/November 2003 interplanetary coronal mass ejections: ACE/EPAM solar energetic particle observations

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jgra..11009s06m&link_type=abstract

Journal of Geophysical Research, Volume 110, Issue A9, CiteID A09S06

Physics

11

Interplanetary Physics: Coronal Mass Ejections (7513), Interplanetary Physics: Energetic Particles (7514), Interplanetary Physics: Interplanetary Magnetic Fields, Interplanetary Physics: Interplanetary Shocks, Interplanetary Physics: Solar Wind Plasma

Scientific paper

In late October and early November 2003 the ACE spacecraft at 1 AU detected two shock-associated interplanetary coronal mass ejections (ICMEs). In the sheath region formed in front of both ICMEs, some of the highest speeds ever directly measured in the solar wind were observed. We analyze in detail the energetic particle signatures measured at 1 AU by the EPAM experiment on board ACE during the passage and in the vicinity of these ICMEs. Solar energetic particles (SEPs) are utilized as diagnostic tracers of the large-scale structure and topology of the interplanetary magnetic field (IMF) embedded within both ICME events. In order to explain the bidirectional particle flows observed within both ICMEs, we have examined two candidate scenarios for these ICMEs in terms of open and closed magnetic field configurations. In the context of an open field configuration, the enhanced magnetic field regions associated with the CME-driven shocks mirror the energetic particles and hence the observed bidirectional flows. In the context of a closed field configuration, bidirectional flows result from particle circulation and reflection in a looped field configuration. Furthermore, we use the ACE/EPAM observations to reassess the leading and trailing boundaries of the ICMEs with respect to those previously proposed based upon ACE/SWEPAM solar wind plasma, suprathermal electron measurements, and ACE/MAG magnetic field data.

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