Rapidly rotating stellar models with radiation pressure

Details Rapidly rotating stellar models with radiation pressure Rapidly rotating stellar models with radiation pressure

Feb 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ap%26ss..67..407d&link_type=abstract

Astrophysics and Space Science, vol. 67, no. 2, Feb. 1980, p. 407-416. Research supported by the Indian National Science Academ

Astronomy and Astrophysics

Astrophysics

4

Early Stars, Perturbation Theory, Radiation Pressure, Stellar Models, Stellar Rotation, Convective Flow, Gas Pressure, Stellar Gravitation, Stellar Mass, Stellar Structure, Thermodynamic Equilibrium

Scientific paper

A modified perturbation technique, developed earlier by the authors, has been used to study the effect of rapid uniform and differential rotation on the equilibrium structure of early type stars. The models are in convective equilibrium with significant radiation pressure. The effects of both uniform and differential rotation on various structural parameters such as mass, radius, central condensation etc., are calculated for different values of the ratio of central radiation pressure to central gas pressure.

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