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Title:
Rapidly rotating polytropes in general relativity
Authors:
Cook, Gregory B.; Shapiro, Stuart L.; Teukolsky, Saul A.
Affiliation:
AA(Cornell Univ., Ithaca, NY, US), AB(Cornell Univ., Ithaca, NY, US), AC(Cornell Univ., Ithaca, NY, US)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 1, p. 227-242 (ApJ Homepage)
Publication Date:
02/1994
Category:
Astrophysics
Origin:
STI
NASA/STI Keywords:
Astronomical Models, Black Holes (Astronomy), Gravitational Collapse, Polytropic Processes, Relativity, Stellar Evolution, Stellar Rotation, Angular Momentum, Equilibrium Methods, Hydrostatics, Neutron Stars, Numerical Analysis, Stellar Mass
DOI:
10.1086/173721
Bibliographic Code:
1994ApJ...422..227C

Abstract

We construct an extensive set of equilibrium sequences of rotating polytropes in general relativity. We determine a number of important physical parameters of such stars, including maximum mass and maximum spin rate. The stability of the configurations against quasi-radial perturbations is diagnosed. Two classes of evolutionary sequences of fixed rest mass and entropy are explored: normal sequences which behave very much like Newtonian evolutionary sequences, and supramassive sequences which exist solely because of relativistic effects. Dissipation leading to loss of angular momentum causes a star to evolve in a quasi-stationary fashion along an evolutionary sequence. Supramassive sequences evolve towards eventual catastrophic collapse to a black hole. Prior to collapse, the star must spin up as it loses angular momentum, an effect which may provide an observational precursor to gravitational collapse to a black hole.

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