Phys. Rev. Lett. 62, 2777–2780 (1989)Oscillations and stability of rapidly rotating neutron starsSee Also: Erratum Received 20 March 1989; published in the issue dated 12 June 1989 A method is described for obtaining numerical solutions of the pulsation equations of rapidly rotating inhomogeneous stellar models. This previously intractable problem has been solved by reexpressing the pulsation equations in terms of a single potential. These equations are solved and the points of the onset of secular instability to gravitational radiation are found. These results indicate 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. © 1989 The American Physical Society URL:
http://link.aps.org/doi/10.1103/PhysRevLett.62.2777
DOI:
10.1103/PhysRevLett.62.2777
PACS:
97.60.Jd, 67.90.+z, 97.60.Gb
See AlsoErratum: James R. Ipser and Lee Lindblom, Oscillations and Stability of Rapidly Rotating Neutron Stars, Phys. Rev. Lett. 63, 1327 (1989). |
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