On the dividing line for stellar coronae

Details On the dividing line for stellar coronae On the dividing line for stellar coronae

Aug 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...307l..55a&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 307, Aug. 15, 1986, p. L55-L59. Research supported

Astronomy and Astrophysics

Astrophysics

40

Emission Spectra, Hertzsprung-Russell Diagram, Late Stars, Stellar Coronas, Stellar Magnitude, X Ray Spectra, Gravitational Effects, Stellar Atmospheres, Stellar Gravitation, Stellar Magnetic Fields, Stellar Temperature

Scientific paper

The authors describe a possible explanation for the observation that late-type stars falling in a certain region of the H-R diagram exhibit no X-ray emission and, hence, appear not to have coronae. The basic idea of the authors' model is that due to the low surface gravity that characterizes the stars without X-ray emission, a hot (T > 106K) corona is thermally unstable and spontaneously cools down to chromospheric temperatures. The key parameter that determines the outer atmospheric structure is shown to be the ratio of the gravitational scale height of plasma at T = 105K to the maximum height of closed magnetic field lines in the corona.

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