Theory of extended stellar atmospheres. I - Computational method and first results for static spherical models

Details Theory of extended stellar atmospheres. I - Computational method and first results for static spherical models Theory of extended stellar atmospheres. I - Computational method and first results for static spherical models

Oct 1974

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1974apjs...28..343m&link_type=abstract

Astrophysical Journal Supplement Series (Supplement no. 265), vol. 28, Oct. 1974, p. 343-372.

Astronomy and Astrophysics

Astrophysics

54

Astronomical Models, Atmospheric Models, Early Stars, Radiative Transfer, Stellar Atmospheres, Computer Techniques, Differential Equations, Hydrostatics, Linear Equations, Mathematical Models, Stellar Gravitation, Stellar Luminosity, Stellar Temperature

Scientific paper

A method is presented that makes possible, for the first time, the calculation of extended spherical non-LTE model stellar atmospheres in hydrostatic and radiative equilibrium. This method is a generalization of the complete-linearization technique of Auer and Mihalas. Models have been obtained for a star with 60 solar masses, 1,000,000 solar luminosities, and 24 solar radii, whose atmosphere is characterized by an effective temperature of 39,500 K and a surface gravity log g = 3.45, i.e., with a spectral type near O6. These models are differentiated by the magnitude and radial dependence of a radiation force multiplier that is inserted into the equation of hydrostatic equilibrium to simulate the effect of radiation force on opacity sources which have not been included explicitly in the calculation. Models have been obtained very close to the limit at which the radiation force and gravity balance; as this condition is approached, the atmospheres become more and more extended.

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