A versatile numerical method for obtaining structures of rapidly rotating baroclinic stars: selfconsistent and systematic solutions with shellulartype rotation
Abstract
This paper develops a novel numerical method for obtaining structures of rapidly rotating stars based on a selfconsistent field scheme. The solution is obtained iteratively. Both rapidly rotating barotropic and baroclinic equilibrium states are calculated selfconsistently using this method. Two types of rotating baroclinic stars are investigated by changing the isentropic surfaces inside the star. Solution sequences of these are calculated systematically and critical rotation models beyond which no rotating equilibrium state exists are also obtained. All of these rotating baroclinic stars satisfy necessarily the BjerknesRosseland rules. Selfconsistent solutions of baroclinic stars with shellulartype rotation are successfully obtained where the isentropic surfaces are oblate and the surface temperature is hotter at the poles than at the equator if it is assumed that the star is an ideal gas star. These are the first selfconsistent and systematic solutions of rapidly rotating baroclinic stars with shellulartype rotations. Since they satisfy the stability criterion due to their rapid rotation, these rotating baroclinic stars would be dynamically stable. This novel numerical method and the solutions of the rapidly rotating baroclinic stars will be useful for investigating stellar evolution with rapid rotations.
 Publication:

Monthly Notices of the Royal Astronomical Society
 Pub Date:
 December 2015
 DOI:
 10.1093/mnras/stv2175
 arXiv:
 arXiv:1507.02693
 Bibcode:
 2015MNRAS.454.3060F
 Keywords:

 stars: massive;
 stars: rotation;
 Astrophysics  Solar and Stellar Astrophysics;
 Astrophysics  High Energy Astrophysical Phenomena
 EPrint:
 14 pages, 6 figures