Oscillations and stability of rapidly rotating neutron stars

Details Oscillations and stability of rapidly rotating neutron stars Oscillations and stability of rapidly rotating neutron stars

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989phrvl..62.2777i&link_type=abstract

Physical Review Letters (ISSN 0031-9007), vol. 62, June 12, 1989, p. 2777-2780.

Physics

44

Angular Velocity, Neutron Stars, Stellar Oscillations, Stellar Rotation, Stellar Gravitation, Stellar Models, Supernova 1987A

Scientific paper

A method for solving the pulsation equations of rapidly rotating inhomogeneous stellar models is presented in which the pulsation equations are expressed in terms of a single potential. The points of the onset of secular instability due to gravitational radiation have been identified. The results suggest that the 0.5-ms period of SN 1987A cannot be interpreted as the rotation of a neutron star using current descriptions of neutron-star matter.

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