On the theory of shock-heated atmospheres. III - Discussion of the formalism and application to stellar coronae

Details On the theory of shock-heated atmospheres. III - Discussion of the formalism and application to stellar coronae On the theory of shock-heated atmospheres. III - Discussion of the formalism and application to stellar coronae

May 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982a%26a...109..205s&link_type=abstract

Astronomy and Astrophysics, vol. 109, no. 2, May 1982, p. 205-212.

Astronomy and Astrophysics

Astrophysics

14

Shock Heating, Shock Waves, Stellar Atmospheres, Stellar Coronas, Stellar Winds, Atmospheric Temperature, Conservation Equations, Radiative Heat Transfer, Stellar Mass Ejection

Scientific paper

Thermally sustained coronas and stellar winds are investigated using a two-zone corona model describing a lower zone at constant pressure in which the mechanical dissipation and wind effects are neglected, and an upper zone characterized by an extended isothermal region. The interface between the two zones is treated as a dissipative layer of neglectable vertical extent, so that jumps of the physical quantities are consistently fixed by the conservation equations. The physical meaning of transition zone and coronal temperature is discussed, and the lower zone, shock formalism, and dissipation layer are analyzed, as are the upper bounds for the coronal temperature, base pressure, and mechanical flux. A detailed study of the model's special loss function is presented, including the minimum shock strength, conduction dominated case, pressure-mechanical flux relation, and base-temperature relation.

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