Energy balance of stellar coronae. I - Methods and examples. II - Effect of coronal heating

Details Energy balance of stellar coronae. I - Methods and examples. II - Effect of coronal heating Energy balance of stellar coronae. I - Methods and examples. II - Effect of coronal heating

Aug 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...259..767h&link_type=abstract

Astrophysical Journal, Part 1, vol. 259, Aug. 15, 1982, p. 767-791. Research supported by the Deutsche Forschungsgemeinschaft;

Astronomy and Astrophysics

Astrophysics

77

Atmospheric Heating, Late Stars, Stellar Coronas, Stellar Mass Ejection, Stellar Temperature, Stellar Winds, Boundary Conditions, Boundary Value Problems, Conductive Heat Transfer, Conservation Equations, Energy Dissipation, Magnetohydrodynamic Waves, Radiative Transfer, Stellar Models

Scientific paper

Simplified models of magnetically open coronal regions are computed, with the aim of fulfilling appropriate boundary conditions at the base of the atmosphere, at the critical point, and at infinity. The models are determined by the stellar mass and radius and by the amount and location of coronal heating, and this dependence is analyzed in terms of pressure, temperature, characteristic heights, energy losses, mass loss, and asymptotic behavior. The results are used to classify the magnetically open coronal regions according to the energy loss mechanism that dominates in the region between the base and the critical point, and it is shown that more complicated heating mechanisms may be replaced by the presented exponential heating law, provided that the damping length is suitably chosen.

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