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

Nov 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009a%26a...507l..21s&link_type=abstract

Astronomy and Astrophysics, Volume 507, Issue 2, 2009, pp.L21-L24

Astronomy and Astrophysics

Astrophysics

6

Acceleration Of Particles, Shock Waves, Sun: Activity, Sun: Coronal Mass Ejections (Cmes), Sun: Particle Emission

Scientific paper

Aims: We study the effect of magnetic geometry on the efficiency of diffusive shock acceleration (DSA) of protons in the solar corona with emphasis on conditions that may lead to the formation of so-called ground level enhancements (GLEs) where the protons are accelerated into energies ≳ 1 GeV. Methods: We use Monte Carlo simulations of DSA in a semirealistic large scale coronal magnetic field near a bipolar active region. This active region is assumed to be the source region of a coronal mass ejection (CME) driving a shock wave in the corona. The shock geometry evolves in time, and the obliquity angle goes through a wide range of values from perpendicular to quasi-parallel. We consider the effect of the evolving magnetic geometry on the acceleration efficiency in five selected field lines. Results: In most of the considered field lines the maximum proton energies are of the order of 100 MeV, which is rather typical for gradual solar energetic particle (SEP) events. We find that the DSA can be more effective on field lines where the shock starts out by being oblique and gradually turns quasi-perpendicular than on field lines where the shock starts perpendicularly.

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