X-ray emission and structure of coronas of active late-type dwarfs

Details X-ray emission and structure of coronas of active late-type dwarfs X-ray emission and structure of coronas of active late-type dwarfs

Dec 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987azh....64.1243k&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 64, Nov.-Dec. 1987, p. 1243-1255. In Russian.

Astronomy and Astrophysics

Astronomy

15

Dwarf Stars, Emission Spectra, Late Stars, Stellar Coronas, Stellar Structure, X Ray Spectra, Density Distribution, G Stars, K Stars, M Stars, Main Sequence Stars, Nonthermal Radiation, Spectral Energy Distribution

Scientific paper

A method for the determination of the density in stellar coronas from X-ray data is suggested. Its application to 45 G, K, and M main-sequence stars shows that the density at the corona base increases by the transition from G stars to MO-M3 stars, and drops thereafter. The rising-density branch is connected with the intensification of solar-type activity processes on G-K stars. The properties of the X-ray emission of active M3-M6 stars, its rapid variability, and its association with flare activity and with nonthermal radio emission are apparently evidence that heating of the coronas of these stars is due to numerous processes of the subflare type.

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