Geometry of ICMEs with and without magnetic flux-rope structure from a Cosmic Ray perspective

Details Geometry of ICMEs with and without magnetic flux-rope structure from a Cosmic Ray perspective Geometry of ICMEs with and without magnetic flux-rope structure from a Cosmic Ray perspective

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsh22a..06k&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SH22A-06

Physics

2100 Interplanetary Physics, 2101 Coronal Mass Ejections (7513), 2104 Cosmic Rays, 2111 Ejecta, Driver Gases, And Magnetic Clouds, 2134 Interplanetary Magnetic Fields

Scientific paper

We have determined ICME (Interplanetary coronal mass ejection) geometry from galactic cosmic ray data recorded by the ground-based muon detector network. The cosmic ray density depression inside the ICME, which is the cause of a Forbush decrease, is represented by an expanding cylinder that is based on a theoretical model of cosmic ray particle diffusion. In 8 ICME events from March 2001 to May 2005, ICME geometry and orientation are deduced from observed time variations of cosmic ray density and density gradient, and are compared with that deduced from a magnetic flux rope model. In 3 of these 8 events, clear signatures of flux rope structure were seen, and the ICME geometry and orientation deduced from the two methods (flux rope modeling and cosmic ray modeling) were very similar. Flux rope modeling was also applied to 2 other events with weaker flux rope signatures, but here the agreement with the cosmic ray method was not as good, presumably because the small magnetic field rotations reduce the efficacy of the flux rope method. In the final 3 events, magnetic fields are distorted because of multiple CME interactions, so the flux rope analysis was not applied. The cosmic ray method could nonetheless be applied and yielded physically reasonable results compatible with results obtained for the flux-rope events.

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