Modeling of Energetic Particle Acceleration and Transport in Solar Corona

Details Modeling of Energetic Particle Acceleration and Transport in Solar Corona Modeling of Energetic Particle Acceleration and Transport in Solar Corona

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh44a..01v&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH44A-01

Physics

7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114), 7807 Charged Particle Motion And Acceleration, 7851 Shock Waves (4455), 7867 Wave/Particle Interactions (2483, 6984)

Scientific paper

Some recent modeling efforts to understand the transport and acceleration of solar energetic particles (SEPs) in corona and interplanetary medium are reviewed. We will present results from analytical calculations and from particle simulations employing the Monte Carlo method. Our modeling efforts concentrate on ions. Specifically, we have considered (i) velocity dispersion analysis of particles observed during the initial rise of an SEP event as obtained from particle transport simulations; (ii) particle acceleration in coronal shock waves during the initial phases of an SEP event; and (iii) the role of the generation of turbulence by the accelerated particles themselves. Ion acceleration by coronal shocks is shown to be consistent with the typical observational results on SEP event onsets. This holds true for both small gradual SEP events, which can be treated under the test-particle approximation, and for the largest SEP events, in which the accelerated particles significantly enhance the turbulence in the solar corona.

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