X-ray-heated models of stellar flare atmospheres - Theory and comparison with observations

descriptionPublicationkeyboard_double_arrow_right Article 01 Feb 1992 English Publisher:American Astronomical SocietyJournal:The Astrophysical Journal Supplement Series, volume 78, page 565 (issn: 0067-0049, eissn: 1538-4365,

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Authors: Suzanne L. Hawley; George H. Fisher;

doi: 10.1086/191640

X-ray-heated models of stellar flare atmospheres - Theory and comparison with observations

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Abstract

A sequence of five model atmospheres consisting of the photosphere, chromosphere, and transition region is computed. The models represent the response of the gas in a magnetically confined loop to intense flare energy release. It is assumed that the energy release is confined to the corona, and the effects of chromospheric evaporation and indirect heating of the lower atmosphere by X-rays emitted from the coronal plasma are included. Line and continuum surface fluxes are presented in the wavelength range 1000-9000 A and are compared with those observed during a giant flare on the M dwarf star AD Leo

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