Non-axisymmetric instability and fragmentation of general relativistic quasi-toroidal stars

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dc.creatorZink, Burkhard
dc.creatorStergioulas, Nikolaos
dc.creatorHawke, Ian
dc.creatorOtt, Christian D.
dc.creatorSchnetter, Erik
dc.creatorMueller, Ewald
dc.date2006-11-19
dc.date.accessioned2026-07-07T11:00:14Z
dc.date.available2026-07-07T11:00:14Z
dc.descriptionIn a recent publication, we have demonstrated that differentially rotating stars admit new channels of black hole formation via fragmentation instabilities. Since a higher order instability of this kind could potentially transform a differentially rotating supermassive star into a multiple black hole system embedded in a massive accretion disk, we investigate the dependence of the instability on parameters of the equilibrium model. We find that many of the models constructed exhibit non-axisymmetric instabilities with corotation points, even for low values of T/|W|, which lead to a fission of the stars into one, two or three fragments, depending on the initial perturbation. At least in the models selected here, an m=1 mode becomes unstable at lower values of T/|W|, which would seem to favor a scenario where one black hole with a massive accretion disk forms. In this case, we have gained evidence that low values of compactness of the initial model can lead to a stabilization of the resulting fragment, thus preventing black hole formation in this scenario.
dc.description30 pages, 36 figures. A version with high-resolution color figures can be found at http://www.cct.lsu.edu/~bzink/material/qts_instability.pdf
dc.identifierhttps://arxiv.org/abs/astro-ph/0611601
dc.identifierhttp://arxiv.org/abs/astro-ph/0611601
dc.identifierPhys.Rev.D76:024019,2007
dc.identifierdoi:10.1103/PhysRevD.76.024019
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/187640
dc.subjectAstrophysics
dc.titleNon-axisymmetric instability and fragmentation of general relativistic quasi-toroidal stars
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