Oscillations and stability of rapidly rotating neutron stars. [SN 1987A]

Journal Article · Mon Jun 12 04:00:00 EDT 1989 · Phys. Rev. Lett.; (United States)

DOI:https://doi.org/10.1103/PhysRevLett.62.2777· OSTI ID:6069073

Ipser, J R; Lindblom, L

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.

• Research Organization: Department of Physics, University of Florida, Gainesville, Florida 32611(US); Department of Physics, Montana State University, Bozeman, Montana 59717
• OSTI ID: 6069073
• Journal Information: Phys. Rev. Lett.; (United States), Journal Name: Phys. Rev. Lett.; (United States) Vol. 62:24; ISSN PRLTA
• Country of Publication: United States
• Language: English

Related Subjects

640102* -- Astrophysics & Cosmology-- Stars & Quasi-Stellar
Radio & X-Ray Sources
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ACCRETION DISKS
ANGULAR VELOCITY
BASIC INTERACTIONS
DATA
EIGENFUNCTIONS
ERUPTIVE VARIABLE STARS
FUNCTIONS
GRAVITATIONAL INTERACTIONS
INFORMATION
INTERACTIONS
MATHEMATICAL MODELS
NEUTRON STARS
NUMERICAL DATA
NUMERICAL SOLUTION
OSCILLATION MODES
PERTURBATION THEORY
STABILITY
STAR MODELS
STARS
SUPERNOVAE
TEMPERATURE DEPENDENCE
VARIABLE STARS
VELOCITY