Turning-point method for axisymmetric stability of rotating relativistic stars

Details Turning-point method for axisymmetric stability of rotating relativistic stars Turning-point method for axisymmetric stability of rotating relativistic stars

Feb 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...325..722f&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 325, Feb. 15, 1988, p. 722-724.

Astronomy and Astrophysics

Astrophysics

66

Relativistic Velocity, Stellar Motions, Stellar Rotation, Angular Momentum, Neutron Stars, Perturbation Theory, Polytropic Processes, Secular Variations

Scientific paper

A turning-point method is used to obtain a simple criterion governing the secular stability of uniformly rotating relativistic stars to axisymmetric perturbations. In particular, along a sequence of rotating neutron stars with fixed angular momentum and increasing central density, the configuration with maximum mass marks the onset of instability.

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