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Turbulent Acceleration in Solar Flares

Published online by Cambridge University Press:  12 April 2016

D. B. Melrose
D. B. Melrose*
Affiliation:
Research Centre for Theoretical Astrophysics, University of Sydney, NSW 2006Australia

Abstract

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Turbulent acceleration in the impulsive phase of solar flares is reviewed, with the emphasis on bulk energization of nonrelativistic electrons and prompt acceleration of the gamma-ray emitting nonrelativistic ions and relativistic electrons. The primary energy release in a flare cannot be due to collisional dissipation. Anomalous resistivity requires that the current flows in many narrow channels with the current density above threshold for current instability. The bulk energization of the electrons is due to the damping of low-frequency electrostatic turbulence generated by the current instability. This turbulence also limits the rate a nonthermal electron tail forms due to runaway acceleration. Stochastic and gyroresonant acceleration by MHD turbulence are discussed briefly, emphasizing the need for preacceleration. Stochastic acceleration is favorable for the gamma-ray emitting particles only if an adequated source of the MHD turbulence can be identified.

Subject headings: acceleration of particles — MHD — Sun: flares — turbulence

Type
Solar Flares
Information
International Astronomical Union Colloquium , Volume 142: Particle Acceleration Phenomena in Astrophysical Plasmas , 1994 , pp. 623 - 630
Copyright
Copyright © The American Astronomical Society 1994

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