Physics
Scientific paper
Apr 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aps..apr.q4004m&link_type=abstract
American Physical Society, April Meeting, April 28 - May 1, 2001 Washington, DC Bulletin of the American Physical Society, Vol.
Physics
Scientific paper
Solar flares are among the most interesting phenomena in the solar system, releasing up to 10^32 ergs of energy on timescales ranging from several seconds to several minutes. Much of this energy appears in the form of suprathermal ions and electrons, which are accelerated out of the background thermal distributions and into the relativistic regime in about 1 second. These energetic particles subsequently produce a host of secondary emissions, ranging from radio waves to nuclear de-excitation gamma-ray lines, as well as escape into space where they can be directly observed. The neutral emissions and the interplanetary particles are valuable diagnostics of the particle acceleration mechanism, the identification of which is a primary goal of solar research. In particular, ion abundance enhancements, first observed in the interplanetary particles but then later inferred from gamma-ray line spectroscopy, are important clues to the nature of the acceleration mechanism. After reviewing the pertinent observational data, we will present the basic requirements that any solar flare particle acceleration theory must satisfy. We will then review the three major classes of acceleration theories that have been discussed, and conclude with the claim that the most viable unified theory is stochastic resonant acceleration by cascading MHD turbulence.
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