Oscillations and stability of rapidly rotating neutron stars

James R. Ipser and Lee Lindblom
Phys. Rev. Lett. 62, 2777 – Published 12 June 1989; Erratum Phys. Rev. Lett. 63, 1327 (1989)
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Abstract

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.

  • Received 20 March 1989

DOI:https://doi.org/10.1103/PhysRevLett.62.2777

©1989 American Physical Society

Erratum

Oscillations and Stability of Rapidly Rotating Neutron Stars

James R. Ipser and Lee Lindblom
Phys. Rev. Lett. 63, 1327 (1989)

Authors & Affiliations

James R. Ipser

  • Department of Physics, University of Florida, Gainesville, Florida 32611

Lee Lindblom

  • Department of Physics, Montana State University, Bozeman, Montana 59717

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Issue

Vol. 62, Iss. 24 — 12 June 1989

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