Confinement of hot, hard X-ray producing electrons in solar flares

Details Confinement of hot, hard X-ray producing electrons in solar flares Confinement of hot, hard X-ray producing electrons in solar flares

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...232..582s&link_type=abstract

Astrophysical Journal, Part 1, vol. 232, Sept. 1, 1979, p. 582-589.

Other

111

Hot Electrons, Magnetohydrodynamics, Solar Electrons, Solar Flares, Solar X-Rays, Astronomical Models, Collisionless Plasmas, Ionizing Radiation, Solar Corona

Scientific paper

Possible thermal models for solar, hard X-ray emission, consisting of small volumes in which the electrons are rapidly heated to 400 million K, are examined to determine under what conditions such models can be more efficient than nonthermal models. The analysis is restricted to one dimension by supposing that the hot electrons are confined in a flux tube and that conduction and convection act only along the magnetic field. A conduction front, thin in relation to other length scales involved, separates the hot electrons from the relatively cold plasma. The range of conduction-front velocity is studied by systematizing the present knowledge of heat conduction and applying it first to a simple model in which convection is neglected, and then to a detailed numerical model in which convection is included. Convection in which mass motion goes to zero at the conduction front does not lead to a change in the conduction-front velocity compared to conduction alone, but does constitute another nonradiative energy loss which reduces the source efficiency.

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