Stability and rotational mixing of modes in Newtonian and relativistic stars

Despite the recent excitement over the r-mode instability of rotating stars, these modes are not yet well-understood for stellar models appropriate to neutron stars - perfect fluid models in which both the equilibrium and perturbed configurations obey the same one-parameter equation of state. In sph...

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Bibliographic Details
Published in:arXiv.org 1999-09
Main Author: Lockitch, Keith H
Format: Article
Language:English
Subjects:
Angular velocity
Astronomical models
Equations of state
Neutron stars
Relativism
Relativistic effects
Spheroids
Stability
Stars
Stellar models
Stellar rotation
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Summary:Despite the recent excitement over the r-mode instability of rotating stars, these modes are not yet well-understood for stellar models appropriate to neutron stars - perfect fluid models in which both the equilibrium and perturbed configurations obey the same one-parameter equation of state. In spherical stars of this kind, r-modes and g-modes form a degenerate zero-frequency subspace. Rotation splits the degeneracy to zeroth order in the star's angular velocity \(\Omega\), and the resulting modes are generically hybrids, whose limit as \(\Omega\to 0\) is a stationary current with axial and polar parts. Lindblom and Ipser have recently found these hybrid rotational modes in an analytic study of the Maclaurin spheroids. This dissertation studies them in Newtonian stars (both uniform density models and \(n=1\) polytropes) and reports a first computation of the hybrid rotational modes of relativistic stars.
ISSN:2331-8422