The oscillations of rapidly rotating Newtonian stellar models. II - Dissipative effects

Journal Article · Wed May 01 04:00:00 EDT 1991 · Astrophysical Journal; (United States)

DOI:https://doi.org/10.1086/170039· OSTI ID:5588714

Ipser, J R; Lindblom, L ^[1]

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1. Florida, University, Gainesville (USA) Montana State University, Bozeman (USA)

A method is described for determining the dissipative effects of viscosity and gravitational radiation on the modes of rapidly rotating Newtonian stellar models. Integral formulae for the dissipative imaginary parts of the frequencies (i.e., the damping or growth times) of these modes are derived. These expressions are evaluated numerically to determine the angular-velocity dependence of these dissipative effects on the l = m f-modes of uniformly rotating polytropes. The importance of the gravitational-radiation driven secular instability in limiting the rotation rate of neutron stars is estimated using these results. 13 refs.

• OSTI ID: 5588714
• Journal Information: Astrophysical Journal; (United States), Journal Name: Astrophysical Journal; (United States) Vol. 373; ISSN ASJOA; ISSN 0004-637X
• 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
ANGULAR VELOCITY
DAMPING
GRAVITATION
GRAVITATIONAL RADIATION
MATHEMATICAL MODELS
MOTION
NEUTRON STARS
OSCILLATION MODES
OSCILLATIONS
RADIATIONS
ROTATION
STAR MODELS
STARS
VELOCITY
VISCOSITY