Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005jrasc..99r.140l&link_type=abstract
Journal of the Royal Astronomical Society of Canada, Vol. 99, No. 4, p.140
Astronomy and Astrophysics
Astronomy
Scientific paper
Traditionally, rapidly rotating stars have been studied assuming the surface can be described as an equipotential surface with a simple point-mass approximation to the gravitational potential and that the centrifugal force can be written as a potential, as is true for conservative rotation laws. Variation in surface temperature and luminosity can then be calculated using von Zeipel's law. We test these assumptions using the results of 2-D stellar evolution calculations for rapidly rotating main-sequence stars. For uniformly rotating stars, we find the spherically symmetric point-mass potential is a good approximation, except for the equatorial regions when v ~ vcrit. For more extreme, but still conservative, angular momentum distributions, the interior mass distribution results in a significant deviation from the spherically symmetric gravitational potential deep inside the star, but not necessarily at the surface. This produces distortion of the deep interior equipotential surfaces, which results in surface temperatures and luminosities significantly different from those predicted by von Zeipel's law.
Deupree Robert G.
Lovekin Catherine
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