Solution of the equilibrium equations for rapidly rotating stars

Journal Article · Thu Jun 15 04:00:00 EDT 1978 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/156215· OSTI ID:6684689

Clement, M J

A two-dimensional, finite-difference technique is presented for the solution of the general stellar structure equations in the case of conservative rotation. The relaxation method makes no approximation with respect to the gravitational potential and is not limited by large central concentration. Numerical tests on differentially rotating models of upper--main-sequence stars show that convergence is very rapid and also that the technique can be applied to a wide range of stellar masses with rotation rates up to the point of secular instability.

• Research Organization: David Dunlap Observatory, University of Toronto
• OSTI ID: 6684689
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 222:3; ISSN ASJOA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
CONVECTION
DIFFERENTIAL EQUATIONS
ENERGY TRANSFER
EQUATIONS
EQUATIONS OF STATE
EQUILIBRIUM
HEAT TRANSFER
MAIN SEQUENCE STARS
MATHEMATICAL MODELS
MOTION
POISSON EQUATION
ROTATION
STAR MODELS
STARS