Electron Beam Return-Current Losses in Solar Flares: Initial Comparison of Analytical and Numerical Results

Details Electron Beam Return-Current Losses in Solar Flares: Initial Comparison of Analytical and Numerical Results Electron Beam Return-Current Losses in Solar Flares: Initial Comparison of Analytical and Numerical Results

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21640417h&link_type=abstract

American Astronomical Society, AAS Meeting #216, #404.17; Bulletin of the American Astronomical Society, Vol. 41, p.902

Physics

Scientific paper

Accelerated electrons play an important role in the energetics of solar flares. Understanding the process or processes that accelerate these electrons to high, nonthermal energies also depends on understanding the evolution of these electrons between the acceleration region and the region where they are observed through their hard X-ray or radio emission. Energy losses in the co-spatial electric field that drives the current-neutralizing return current can flatten the electron distribution toward low energies. This in turn flattens the corresponding bremsstrahlung hard X-ray spectrum toward low energies. The lost electron beam energy also enhances heating in the coronal part of the flare loop.
Extending earlier work by Knight & Sturrock (1977), Emslie (1980), Diakonov & Somov (1988), and Litvinenko & Somov (1991), I have derived analytical and semi-analytical results for the nonthermal electron distribution function and the self-consistent electric field strength in the presence of a steady-state return-current. I review these results, presented previously at the 2009 SPD Meeting in Boulder, CO, and compare them and computed X-ray spectra with numerical results obtained by Zharkova & Gordovskii (2005, 2006). The physical significance of similarities and differences in the results will be emphasized.
This work is supported by NASA's Heliophysics Guest Investigator Program and the RHESSI Project.

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