Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1982
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982saosr.392a.121h&link_type=abstract
In Smithsonian Astrophysics Observatory 2nd Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun, Vol. 1 p 121-135 (
Astronomy and Astrophysics
Astrophysics
1
Heating, Main Sequence Stars, Stellar Coronas, Temperature Dependence, Cooling, Stellar Mass Ejection, Stellar Temperature, Stellar Winds, Thermal Conductivity
Scientific paper
Models of open regions in hot stellar coronae are presented. For a given star these regions depend on the total amount phiMo of coronal heating and on the characteristic length (L) over which this energy is dissipated. The height of the temperature maximum is mainly determined by L. The coronal temperature, the mass loss rate, and the relative fraction of wind energy losses increase strongly with L as long as L is much smaller than the stellar radius. For large L, however, these quantities are only weak functions of L, while they still increase with increasing phiMo. Thus, if the heating occurs close to the stellar surface, the open coronal regions are cool, and most of the energy is used for radiation. Extended coronal heating, on the other hand, leads to hot coronal regions with small base pressure and predominating energy losses due to stellar wind (for large phiMo and/or outward thermal conduction (for small phi sub Mo).
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