A Numerical Method for Generating Rapidly Rotating Bipolytropic Structures in Equilibrium

Abstract

We demonstrate that rapidly rotating bipolytropic (composite polytropic) stars and toroidal disks can be obtained using Hachisu's self consistent field technique. The core and the envelope in such a structure can have different polytropic indices and also different average molecular weights. The models converge for high $T/|W|$ cases, where T is the kinetic energy and W is the gravitational energy of the system. The agreement between our numerical solutions with known analytical as well as previously calculated numerical results is excellent. We show that the uniform rotation lowers the maximum core mass fraction or the Sch$\ddot{\mathrm{o}}$nberg-Chandrasekhar limit for a bipolytropic sequence. We also discuss the applications of this method to magnetic braking in low mass stars with convective envelopes.

References in corpus (3)

• Modules for Experiments in Stellar Astrophysics (MESA)
• The fast spin-rotation of a young extrasolar planet
• Numerical Methods for the Simulation of Dynamical Mass Transfer in Binaries

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