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This paper develops a novel numerical method for obtaining structures ofrapidly rotating stars based on a self-consistent field scheme. The solution isobtained iteratively. Both rapidly rotating barotropic and baroclinicequilibrium states are calculated self-consistently using this method. Twotypes of rotating baroclinic stars are investigated by changing the isentropicsurfaces inside the star. Solution sequences of these are calculatedsystematically and critical rotation models beyond which no rotatingequilibrium state exists are also obtained. All of these rotating baroclinicstars satisfy necessarily the Bjerknes-Rosseland rules. Self-consistentsolutions of baro-clinic stars with shellular-type rotation are successfullyobtained where the isentropic surfaces are oblate and the surface temperatureis hotter at the poles than at the equator if it is assumed that the star is anideal gas star. These are the first self-consistent and systematic solutions ofrapidly rotating baroclinic stars with shellular-type rotations. Since theysatisfy the stability criterion due to their rapid rotation, these rotatingbaroclinic stars would be dynamically stable. This novel numerical method andthe solutions of the rapidly rotating baroclinic stars will be useful forinvestigating stellar evolution with rapid rotations.

monthly notices of the royal astronomical society

A versatile numerical method for obtaining structures of rapidly  rotating baroclinic stars: self-consistent and systematic solutions with  shellular-type rotation