Acceleration Mechanisms and Radiative Signature of the Electrons in Solar Flares

Details Acceleration Mechanisms and Radiative Signature of the Electrons in Solar Flares Acceleration Mechanisms and Radiative Signature of the Electrons in Solar Flares

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..aprk12004p&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

I will first outline the possible channels of the dissipation of the energy released during a solar flare, presumably from magnetic reconnection events, and then describe the possible particle acceleration mechanisms with particular focus on electrons. It will be shown that the most likely mechanism of acceleration to highest energies is stochastic acceleration by plasma turbulence. Two recent critical observations, namely spectra extending over a wide dynamic range and high spatial resolution hard X-ray observations, will be used to demonstrate how the model parameters can be constrained with the higher quality observations expected from HESSI. Possible application of these ideas to other high energy astrophysical sources such as gamma-ray bursts and accretion disk will be discussed.

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