Heating and acceleration processes in hot thermal and impulsive solar flares

Details Heating and acceleration processes in hot thermal and impulsive solar flares Heating and acceleration processes in hot thermal and impulsive solar flares

Mar 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...290..353t&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 290, March 1, 1985, p. 353-358.

Astronomy and Astrophysics

Astronomy

49

High Temperature Plasmas, Particle Acceleration, Plasma Density, Plasma Heating, Solar Flares, Solar X-Rays, Electric Fields, Magnetic Fields, Ohmic Dissipation, Particle Collisions, Resistance Heating, X Ray Astronomy

Scientific paper

A simple numerical model describing the time-dependent characteristics of hot thermal impulsive solar flares is presented. The model is based on observations in the hard X-ray (about 10 keV) region carried out onboard the Hinotori satellite. It is assumed in the model that a steady electric field is applied by an external driver during the course of flare evolution. Preliminary integrations of the model show that the plasma density and in the energy release site plays an important role in determining the mode of energy release in the flare. In the impulsive phase, more than 10 to the 35th electrons per sec can escape due to the relatively low plasma density of no more than 4 x 10 to the 10th per cubic cm. The estimated number of runaway electrons in the model is found to be consistent with the observed target flux above 30-40 keV. In the gradual phase, electron runaway was reduced due to an increase in plasma density. The plasma in the energy release site is in the classical state throughout the flare, irrespective of the possible ion-cyclotron turbulence at the onset of the impulsive phase. The model parameters for the gradual phase of flare activity are given in a table.

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