Static spherically symmetric NLTE model atmospheres near the Eddington limit

Details Static spherically symmetric NLTE model atmospheres near the Eddington limit Static spherically symmetric NLTE model atmospheres near the Eddington limit

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1171..357k&link_type=abstract

RECENT DIRECTIONS IN ASTROPHYSICAL QUANTITATIVE SPECTROSCOPY AND RADIATION HYDRODYNAMICS: Proceedings of the International Confe

Astronomy and Astrophysics

Astrophysics

Stellar Atmospheres, Radiative Transfer, Stars, Stellar Atmospheres, Radiative Transfer, Opacity And Line Formation, Radiative Transfer, Scattering, Star Formation

Scientific paper

Radiative force plays an important role in setting structure of stellar atmospheres. If radiative force overcomes gravity, stellar wind appears. In O and B stars, force coming from radiation absorbed by spectral lines of metals dominates the radiative force. However, in first stars metals are not present, the radiative force is dominated by contribution of continuum hydrogen and helium absorption, and does not overcome gravity. Since no stellar wind is present in these stars, static model atmospheres are suitable. However, if such star is close to the Eddington limit, calculation procedure is often unstable.

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