Torsional Oscillations of Slowly Rotating Relativistic Stars

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dc.creatorVavoulidis, M.
dc.creatorStavridis, A.
dc.creatorKokkotas, K. D.
dc.creatorBeyer, H.
dc.date2007-03-06
dc.date.accessioned2026-07-07T11:01:47Z
dc.date.available2026-07-07T11:01:47Z
dc.descriptionWe study the effects of rotation on the torsional modes of oscillating relativistic stars with a solid crust. Earlier works in Newtonian theory provided estimates of the rotational corrections for the torsional modes and suggested that they should become CFS unstable, even for quite low rotation rates. In this work, we study the effect of rotation in the context of general relativity using elasticity theory and in the slow-rotation approximation. We find that the Newtonian picture does not change considerably. The inclusion of relativistic effects leads only to quantitative corrections. The degeneracy of modes for different values of $m$ is removed, and modes with $\ell=m$ are shifted towards zero frequencies and become secularly unstable at stellar rotational frequencies $\sim$ 20-30 Hz.
dc.description6 pages, 1 figure. Accepted for publication to MNRAS
dc.identifierhttps://arxiv.org/abs/gr-qc/0703039
dc.identifierhttp://arxiv.org/abs/gr-qc/0703039
dc.identifierMon.Not.Roy.Astron.Soc.377:1553-1556,2007
dc.identifierdoi:10.1111/j.1365-2966.2007.11706.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/188055
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.titleTorsional Oscillations of Slowly Rotating Relativistic Stars
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