Theory of extended stellar atmospheres. II - A grid of static spherical models for O stars and planetary nebula nuclei

Details Theory of extended stellar atmospheres. II - A grid of static spherical models for O stars and planetary nebula nuclei Theory of extended stellar atmospheres. II - A grid of static spherical models for O stars and planetary nebula nuclei

Nov 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...202...92k&link_type=abstract

Astrophysical Journal, vol. 202, Nov. 15, 1975, pt. 1, p. 92-113.

Astronomy and Astrophysics

Astrophysics

79

Astronomical Models, Early Stars, O Stars, Planetary Nebulae, Stellar Atmospheres, Stellar Evolution, Energy Distribution, Line Spectra, Stellar Mass, Stellar Radiation

Scientific paper

Spherical static non-LTE model atmospheres are presented for stars from 30 to 60 solar masses at various points on their evolutionary tracks, and for some nuclei of planetary nebulae at two points of a modified Harman-Seaton sequence. The method of Mihalas and Hummer was employed, which uses a parametrized radiation force multiplier to simulate the force of radiation arising from the entire line spectrum. However, in the present work the density structure computed in the LTE models was held fixed in the calculation of the corresponding non-LTE models; in addition, the opacity of an average light ion was taken into account. The effects of sphericity, as distinct from those arising from a density structure modified by a large radiation force, were investigated by computing a few planar models using the same parametrized radiation force multiplier as for the spherical models. Extensive tables are given of monochromatic magnitudes, continuum jumps and gradients, Stroemgren-system colors, monochromatic extensions, and the profiles and equivalent widths of the hydrogen lines for all models.

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