2-dimensional models of rapidly rotating stars I. Uniformly rotating zero age main sequence stars

Details 2-dimensional models of rapidly rotating stars I. Uniformly rotating zero age main sequence stars 2-dimensional models of rapidly rotating stars I. Uniformly rotating zero age main sequence stars

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...428..171r&link_type=abstract

Astronomy and Astrophysics, v.428, p.171-179 (2004)

Astronomy and Astrophysics

Astrophysics

14

Stars: Interiors, Stars: Rotation

Scientific paper

We present results for 2-dimensional models of rapidly rotating main sequence stars for the case where the angular velocity Ω is constant throughout the star. The algorithm used solves for the structure on equipotential surfaces and iteratively updates the total potential, solving Poisson's equation by Legendre polynomial decomposition; the algorithm can readily be extended to include rotation constant on cylinders. We show that this only requires a small number of Legendre polynomials to accurately represent the solution. We present results for models of homogeneous zero age main sequence stars of mass 1, 2, 5, 10 M&sun; with a range of angular velocities up to break up. The models have a composition X=0.70, Z=0.02 and were computed using the OPAL equation of state and OPAL/Alexander opacities, and a mixing length model of convection modified to include the effect of rotation. The models all show a decrease in luminosity L and polar radius Rp with increasing angular velocity, the magnitude of the decrease varying with mass but of the order of a few percent for rapid rotation, and an increase in equatorial radius Re. Due to the contribution of the gravitational multipole moments the parameter Ω2 Re3/GM can exceed unity in very rapidly rotating stars and Re/Rp can exceed 1.5.

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