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

Abstract

This paper develops a novel numerical method for obtaining structures of rapidly rotating stars based on a self-consistent field scheme. The solution is obtained iteratively. Both rapidly rotating barotropic and baroclinic equilibrium states are calculated self-consistently 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 Bjerknes-Rosseland rules. Self-consistent solutions of baro-clinic stars with shellular-type 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 self-consistent and systematic solutions of rapidly rotating baroclinic stars with shellular-type 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.

14 pages, 6 figures; published MNRAS 454, 3060--3072 (2015)

References in corpus (5)

• Pre-Supernova Evolution of Massive Single and Binary Stars
• The VLT-FLAMES survey of massive stars: atmospheric parameters and rotational velocity distributions for B-type stars in the Magellanic Clouds
• Stellar Yields of Rotating First Stars. I. Yields of Weak Supernovae and Abundances of Carbon-enhanced Hyper Metal Poor Stars
• Axisymmetric and stationary structures of magnetized barotropic stars with extremely strong magnetic fields deep inside
• Magnetized stars with differential rotation and a differential toroidal field

Cited by in corpus (8)

• Rotating neutron stars with non-barotropic thermal profile
• The optically thick rotating magnetic wind from a massive white dwarf merger product
• Gravity darkening in stars with surface differential rotation
• Rotating white dwarf models with finite-temperature envelope
• Propagation of Relativistic, Hydrodynamic, Intermittent Jets in a Rotating, Collapsing GRB Progenitor Star
• Rotational equilibria by Lagrangian variational principle: toward multi-dimensional stellar evolutions
• A Lagrangian construction of rotating stars
• Asymmetric emissions of neutrinos in the cooling of rotating proto-neutron stars