Rapidly rotating general relativistic stars. I - Numerical method and its application to uniformly rotating polytropes

Details Rapidly rotating general relativistic stars. I - Numerical method and its application to uniformly rotating polytropes Rapidly rotating general relativistic stars. I - Numerical method and its application to uniformly rotating polytropes

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.237..355k&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 237, March 15, 1989, p. 355-379.

Statistics

Computation

190

Computational Astrophysics, Self Consistent Fields, Stellar Rotation, Einstein Equations, Polytropic Processes, Stellar Gravitation, Supernova Remnants

Scientific paper

The Newtonian self-consistent field method has been generalized to the general relativistic case as a means of modeling the structures of rapidly rotating relativistic stars. The method is used to compute uniformly rotating polytropic stars having polytropic indices N = 1/2, 3/2, and 3 for several values of gravitational strength. For the case of strong gravity, the configurations of rotating stars resemble Newtonian polytropes having much higher polytropic indices.

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