The structure of rotating polytropes (Second order)

Details The structure of rotating polytropes (Second order) The structure of rotating polytropes (Second order)

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984ap%26ss.106..161s&link_type=abstract

Astrophysics and Space Science (ISSN 0004-640X), vol. 106, no. 1, Nov. 1984, p. 161-171.

Statistics

Computation

6

Computational Astrophysics, Polytropic Processes, Rotating Matter, Stellar Models, Stellar Rotation, Stellar Structure, Equilibrium Equations, Perturbation Theory

Scientific paper

The structural equations for the inner and outer regions of a rotating polytrope (as used in stellar-structure models) are reformulated to include second-order terms in the perturbation parameter alpha and solved by extending the method of Monaghan and Roxburgh (1965), as used in the first order by Singh and Singh (1982). A critical configuration at which the centrifugal force balances gravity at the equator is defined, and numerical results for parameter values of interest in astrophysics are presented in tables. Comparison of the results for alpha, xi(e), and xi(p) with those of James (1964) and Singh and Singh (1982) shows that the improvement introduced by the use of the second-order method is small, and continued modeling based on the first-order values is recommended.

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