Stability of rotating stellar models in general relativity theory

Journal Article · Fri Apr 01 04:00:00 EST 1983 · Astrophys. J.; (United States)

DOI:https://doi.org/10.1086/160877· OSTI ID:5832457

Lindblom, L; Hiscock, W A

We investigate the effects of viscosity and thermal conductivity on the stability of rotating stellar models in general relativity theory. The equations of motion for the perturbed fluid stellar model (including nonadiabatic and dissipative effects) are used to construct an energy functional for the perturbed motion of the star. This energy is used to investigate the stability of rotating stellar models. The most interesting results of our investigation are (1) that the generic gravitational radiation-induced secular instability (discovered by J. L. Friedman in rotating perfect fluid stars) does not exist in slowly rotating stars having nonzero dissipation coefficients; and (2) three conditions necessary for the stability of these models are (a) the Schwarzschild criterion, (b) subluminal sound velocity, and (c) the dissipation coefficients not being too large.

• Research Organization: Institute of Theoretical Physics, Department of Physics, Stanford University
• OSTI ID: 5832457
• Journal Information: Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 267:1; ISSN ASJOA
• 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
DIFFERENTIAL EQUATIONS
DISSIPATION FACTOR
DISTURBANCES
EQUATIONS
EQUATIONS OF MOTION
FIELD THEORIES
FLUID MECHANICS
GENERAL RELATIVITY THEORY
GRAVITATIONAL RADIATION
MATHEMATICAL MODELS
MECHANICS
MOTION
PARTIAL DIFFERENTIAL EQUATIONS
PHYSICAL PROPERTIES
RADIATIONS
ROTATION
STABILITY
STAR MODELS
THERMAL CONDUCTIVITY
THERMODYNAMIC PROPERTIES
VISCOSITY