Physics
Scientific paper
May 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsh41a..09n&link_type=abstract
American Geophysical Union, Spring Meeting 2008, abstract #SH41A-09
Physics
7514 Energetic Particles (2114), 7845 Particle Acceleration, 7851 Shock Waves (4455), 7867 Wave/Particle Interactions (2483, 6984)
Scientific paper
We present simulations from a numerical model of solar-energetic-particle (SEP) acceleration at a coronal- mass-ejection-driven shock traveling through the solar corona. The model includes full pitch-angle dependence, self-consistent resonant wave-particle interaction, focusing, convection, adiabatic deceleration, wave propagation and wave transmission at shock. The model is solved with a new accurate finite-difference method. Outward streaming SEPs amplify upstream outward Alfvén waves, which are further enhanced by the wave transmission process as they travel downstream of the advancing shock. The explosively growing waves bootstrap SEP acceleration. However, shock accelerated SEPs also stream downstream, damping outward waves and enhancing inward waves there. Particles scattered between upstream outward waves and downstream inward waves experience less compression than SEPs scattered between upstream outward waves and downstream outward waves. Thus SEPs streaming inward downstream tend to slow shock acceleration and to produce a softer SEP energy spectrum. We will illustrate these opposing processes with computed results and discuss how SEP acceleration depends on model assumptions and physical parameters, e.g., shock speed, Alfvén speed, ambient wave intensity, seed particle energy and density. Acknowledgment: this work was supported by NASA LWS04-0000-0076 and SHP04-0016-0024.
Ng Chee K.
Reames Donald. V.
Tylka Allan J.
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