Computer Science – Sound
Scientific paper
Apr 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...267..384l&link_type=abstract
Astrophysical Journal, Part 1, vol. 267, Apr. 1, 1983, p. 384-401.
Computer Science
Sound
32
Magnetohydrodynamic Stability, Relativistic Plasmas, Relativity, Stellar Gravitation, Stellar Models, Stellar Rotation, Energy Dissipation, Equations Of Motion, Gauge Invariance, Heat Transfer, Plane Waves, Plasma Oscillations, Rotating Plasmas, Thermal Conductivity, Viscosity
Scientific paper
The effects of viscosity and thermal conductivity on the stability of rotating stellar models in general relativity theory are investigated. 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 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.
Hiscock William A.
Lindblom Lee
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