Gas dynamics in the impulsive phase of solar flares. I Thick-target heating by nonthermal electrons

Details Gas dynamics in the impulsive phase of solar flares. I Thick-target heating by nonthermal electrons Gas dynamics in the impulsive phase of solar flares. I Thick-target heating by nonthermal electrons

Apr 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...279..896n&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 279, April 15, 1984, p. 896-908.

Astronomy and Astrophysics

Astrophysics

115

Hydrodynamics, Solar Atmosphere, Solar Electrons, Solar Flares, Atmospheric Heating, Hydrodynamic Equations

Scientific paper

A numerical investigation is carried out of the gas dynamical response of the solar atmosphere to a flare energy input in the form of precipitating nonthermal electrons. Rather than discussing the origin of these electrons, the spectral and temporal characteristics of the injected flux are inferred through a thick-target model of hard X-ray bremsstrahlung production. It is assumed that the electrons spiral about preexisting magnetic field lines, making it possible for a one-dimensional spatial treatment to be performed. It is also assumed that all electron energy losses are due to Coulomb collisions with ambient particles; that is, return-current ohmic effects and collective plasma processes are neglected. The results are contrasted with earlier work on conductive heating of the flare atmosphere. A local temperature peak is seen at a height of approximately 1500 km above the photosphere. This derives from a spatial maximum in the energy deposition rate from an electron beam. It is noted that such a feature is not present in conductively heated models. The associated localized region of high pressure drives material both upward and downward.

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