Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977azh....54.1268b&link_type=abstract
Astronomicheskii Zhurnal, vol. 54, Nov.-Dec. 1977, p. 1268-1280. In Russian.
Astronomy and Astrophysics
Astronomy
13
Stellar Envelopes, Stellar Models, Stellar Winds, T Tauri Stars, Coronas, Stellar Atmospheres, Stellar Mass Ejection, X Ray Astronomy
Scientific paper
A shell model for T Tauri stars is considered which consists of a hot (about 1 million K) radially outflowing solar-wind-type corona that is responsible for the observed UV excesses and colder (about 20,000 K) slowly moving clouds that are impregnated in the corona and give rise to the observed bright H Balmer and Ca II emission lines. The cold clouds are assumed to be formed in the hot outflowing corona as a result of thermal instability, and the observed delay between intensity variations in the H-alpha line and the U-band continuum is attributed to the time required for cooling from the coronal to the cloud temperature. Calculations show that in this model the nonthermal energy flux due to dissipation of convective motions may be substantially higher than the energy loss due to photospheric radiation. A soft X-ray flux from such stars is predicted, which may attain a value of 10 to the -10th or -11th power erg/sq cm per sec at earth in the energy range from 0.2 to 0.28 keV.
Bisnovatyi-Kogan Gennadi S.
Lamzin Sergei A.
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