that is, rotation couples a polar
l
-term to an axial
term (the coupling to the
l
+1 term is, however, strongly favoured over the coupling to the
l
-1 term [61
]). Similarly, for a rotating ``axial'' mode with
l
=
m,
In rotating stars, quasi-normal modes of oscillation have been
studied only in the slow rotation limit, in the post-Newtonian,
and in the Cowling approximations. The solution of the fully
relativistic perturbation equations for a rapidly rotating star
is still a very challenging task and only recently have they been
solved for zero-frequency (neutral) modes [293,
296
]. First frequencies of quasi-radial modes have now been obtained
through 3D numerical time evolutions of the nonlinear
equations [105
].
Going further The equations that describe oscillations of the solid crust of a rapidly rotating relativistic star are derived by Priou in [247]. The effects of superfluid hydrodynamics on the oscillations of neutron stars have been investigated by several authors, see e.g. [203, 67, 8, 10] and references therein.
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Rotating Stars in Relativity
Nikolaos Stergioulas http://www.livingreviews.org/lrr-2003-3 © Max-Planck-Gesellschaft. ISSN 1433-8351 Problems/Comments to livrev@aei.mpg.de |