A model of solar coronal heating by classical inverse bremsstrahlung and generation of the solar wind

Details A model of solar coronal heating by classical inverse bremsstrahlung and generation of the solar wind A model of solar coronal heating by classical inverse bremsstrahlung and generation of the solar wind

Aug 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...412..827o&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 412, no. 2, p. 827-840.

Astronomy and Astrophysics

Astrophysics

3

Astronomical Models, Bremsstrahlung, Solar Corona, Solar Wind, Solar Atmosphere, Solar Heating

Scientific paper

A term which represents heating due to classical inverse bremsstrahlung is included in the equations for a one-fluid model of the solar atmosphere. To be effective, this heating mechanism needs an electric field that oscillates with a frequency comparable to the local plasma frequency and that has intensity strong enough slightly to influence particle motions during collisions. Starting low in the solar atmosphere with a temperature of the order of 10 exp 4 K and a small radial fluid velocity, the solution of the equations shows a sharp temperature rise through a rather thin layer and a velocity that farther out in the radial direction passes through a sonic point. In this sense the model is an extension of Parker's (1958) classical model which predicted the solar wind. Particular care has been taken to integrate through the singular point. At large distances of the order of 1 AU, temperature, density, and velocity tend toward values similar to known values in the solar wind at the position of the Earth.

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