Other
Scientific paper
May 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.203..457s&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 203, May 1983, p. 457-489.
Other
65
Gravitational Waves, Neutron Stars, Stellar Models, Stellar Oscillations, Conservation Laws, Eigenvalues, Equations Of Motion, Liapunov Functions, Mathematical Models, Pulsars, Spherical Harmonics, Tensors
Scientific paper
In view of the possibility that torsional oscillations of neutron stars may be observable in the timing of pulsar subpulses and/or in future gravitational-wave detectors, the detailed mathematical theory of such torsional oscillations and of the gravitational waves they emit is developed. The oscillations are analyzed with the formulation of first-order perturbations of a fully general relativistic spherical stellar model. With the exception of gravitational radiation reaction, all sources of damping are ignored. The perturbations are resolved into spherical harmonics, which, it is noted, decouple from each other. For each harmonic, the study presents equations of motion, an action principle, an energy conservation law, and a Liapunov-type proof that the oscillations are always stable. Each harmonic is then resolved into normal modes with outgoing gravitational waves, and an eigenvalue problem is raised for the eigenfunctions and the eigenfrequencies. Five methods of solving the eigenvalue problem are given. Three methods are valid in general; one is valid for the slow-motion approximation; and one is valid in the weak gravity approximation.
Schumaker Bonny L.
Thorne Kip S.
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