On the solution of the equilibrium equations for rapidly rotating stars

Details On the solution of the equilibrium equations for rapidly rotating stars On the solution of the equilibrium equations for rapidly rotating stars

Jun 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...222..967c&link_type=abstract

Astrophysical Journal, Part 1, vol. 222, June 15, 1978, p. 967-975. Research supported by the National Research Council of Cana

Mathematics

30

Finite Difference Theory, Main Sequence Stars, Stellar Models, Stellar Rotation, Stellar Structure, Potential Theory, Relaxation Method (Mathematics), Secular Variations, Stellar Gravitation, Stellar Mass

Scientific paper

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.

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