Non-linear Evolution of Rotating Relativistic Stars

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dc.creatorStergioulas, N.
dc.creatorFont, J. A.
dc.creatorKokkotas, K. D.
dc.date1999-04-05
dc.date.accessioned2026-07-07T03:33:07Z
dc.date.available2026-07-07T03:33:07Z
dc.descriptionWe present first results of the non-linear evolution of rotating relativistic stars obtained with an axisymmetric relativistic hydrodynamics code in a fixed spacetime. As initial data we use stationary axisymmetric and perturbed configurations. We find that, in order to prevent (numerical) angular momentum loss at the surface layers of the star a high-resolution grid (or a numerical scheme that retains high order at local extrema) is needed. For non-rotating stars, we compute frequencies of radial and non-radial small-amplitude oscillations, which are in excellent agreement with linear normal mode frequencies computed in the Cowling approximation. As a first application of our code, quasi-radial modes of rapidly rotating relativistic stars are computed. By generalizing our numerical code to 3-D, we plan to study the evolution and non-linear dynamics of toroidal oscillations (r-modes) of rapidly rotating neutron stars, which are a promising source of gravitational waves.
dc.description12 pages, 4 figures, Contribution to the 19th Texas Symposium
dc.identifierhttps://arxiv.org/abs/gr-qc/9904009
dc.identifierhttp://arxiv.org/abs/gr-qc/9904009
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/36492
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.titleNon-linear Evolution of Rotating Relativistic Stars
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