Viscosity driven instability in rotating relativistic stars
نویسندگان
چکیده
منابع مشابه
Gravitational-Wave Driven Instability of Rotating Relativistic Stars
A series of recent surprises appear dramatically to have improved the likelihood that the spin of rapidly rotating, newly formed neutron stars is limited by a nonaxisymmetric instability driven by gravitational waves – and that the emitted waves may be detectable. The first of these was the discovery that the r-modes, rotationally restored modes that have axial parity for spherical models, are ...
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Perturbations of rotating relativistic stars can be classified by their behavior under parity. For axial perturbations (r-modes), initial data with negative canonical energy is found with angular dependence e for all values of m ≥ 2 and for arbitrarily slow rotation. This implies instability (or marginal stability) of such perturbations for rotating perfect fluids. This low m-instability is str...
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Several recent surprises appear dramatically to have improved the likelihood that the spin of rapidly rotating, newly formed neutron stars (and, possibly, of old stars spun up by accretion) is limited by a nonaxisymmetric instability driven by gravitational waves. Except for the earliest part of the spin-down, the axial l=m=2 mode (an r-mode) dominates the instability, and the emitted waves may...
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ژورنال
عنوان ژورنال: Physical Review D
سال: 2006
ISSN: 1550-7998,1550-2368
DOI: 10.1103/physrevd.74.084006