Diffusive Shock Acceleration to Relativistic Energies in the Solar Corona

Details Diffusive Shock Acceleration to Relativistic Energies in the Solar Corona Diffusive Shock Acceleration to Relativistic Energies in the Solar Corona

Dec 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh33a1482s&link_type=abstract

American Geophysical Union, Fall Meeting 2009, abstract #SH33A-1482

Physics

Plasma Physics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7514] Solar Physics, Astrophysics, And Astronomy / Energetic Particles, [7845] Space Plasma Physics / Particle Acceleration

Scientific paper

In some of the largest solar energetic particle (SEP) events ions are accelerated into sufficiently high energies so that the secondary particles produced by these ions, when colliding with the particles in Earth's atmosphere, are detectable at the surface. These ground level enhancements are much rarer than gradual SEP events in general, roughly one event per year vs. on average 20 events per year during solar maximum. This suggests that there are some special requirements for ions to be accelerated into GeV per nucleon energies and above, or that these ions are produced in so small regions in the solar corona that they are only rarely magnetically connected with the Earth. We study diffusive shock acceleration (DSA) in the vicinity of an active region in the corona, as modeled by a bipolar magnetic structure just below the surface (so-called delta spot), using test particle simulations. We find that the exact geometry of the magnetic field can have a significant effect on the efficiency of DSA, and that there are regions where, all other simulation parameters kept constant, the coronal protons can be accelerated into significantly higher energies (1-10 GeV vs. 100 MeV) than elsewhere.

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