Computer Science – Numerical Analysis
Scientific paper
Feb 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422..227c&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 1, p. 227-242
Computer Science
Numerical Analysis
93
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
Scientific paper
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.
Cook Gregory B.
Shapiro Stuart L.
Teukolsky Saul A.
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