Modeling particle acceleration and transport in gradual SEP events

Details Modeling particle acceleration and transport in gradual SEP events Modeling particle acceleration and transport in gradual SEP events

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh43b1531v&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH43B-1531

Physics

2139 Interplanetary Shocks, 7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114)

Scientific paper

Gradual Solar Energetic Particle events (SEPs) are now believed to be associated with shocks driven by Coronal Mass Ejections (CMEs). As a CME propagates out from the Sun, it drives a shock in front where particles are accelerated to energies to 10's MeV, presumably via first order Fermi acceleration mechanism. Once accelerated, these energetic particles can be trapped in the downstream complex of the shock, adiabatically cool as the shock propagates out and form the ESP (Energetic Storm Particle) portion of the event when the shock passes 1 AU. They can also escape from the shock front, reaching 1 AU much earlier than the shock, forming the SEP portion of the event. Depending on the geometry of the shock and which part (nose or flank) of the shock are magnetically connected to the Earth, the maximum energy observed can differ by an order of magnitude for events that have similar solar conditions and shock characteristics. To better understand gradual SEP events, a model that incorporates shock propagation, particle acceleration at both quasi-perpendicular and quasi-parallel shocks and the subsequent transport in the interplanetary medium is essential. In this work, we describe our model of particle acceleration and transport at CME-driven shocks. Recent progresses of the model such as 2-D extension, inclusion of realistic solar wind parameters and comparison with observations for specific events will be discussed.

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