Astronomy and Astrophysics – Astrophysics
Scientific paper
Sep 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...272..739r&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 272, Sept. 15, 1983, p. 739-755.
Astronomy and Astrophysics
Astrophysics
45
Atmospheric Heating, Chromosphere, Radiative Heat Transfer, Solar Electrons, Solar Flares, Solar Temperature, Conductive Heat Transfer, Finite Difference Theory, Gas Pressure, Plasma Heating, Solar Corona, Solar Spectra
Scientific paper
The response of the solar chromosphere to flare processes, namely nonthermal electrons, thermal conduction, and coronal pressure, is modeled. Finite difference methods employing linearization and iteration are used in obtaining simultaneous solutions to the equations of steady-state energy balance, hydrostatic equilibrium, radiative transfer, and atomic statistical equilibrium. The atmospheric response is assumed to be confined to one dimension by a strong vertical magnetic field. A solution is obtained to the radiative transfer equation for the most important optically thick transitions of hydrogen, magnesium, and calcium. The theoretical atmospheres discussed here are seen as elucidating the role of various physical processes in establishing the structure of flare chromospheres. At low coronal pressures, conduction is found to be more important than nonthermal electrons in establishing the position of the transition region. Only thermal conduction can adequately account for the chromospheric evaporation in compact flares. Of the mechanisms considered, only nonthermal electrons bring about significant heating below the flare transition region.
Canfield Richard C.
Ricchiazzi P. J.
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