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

Non-axisymmetric instability and fragmentation of general relativistic quasi-toroidal stars
Non-axisymmetric instability and fragmentation of general relativistic quasi-toroidal stars
In 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.
1550-7998
24019
Zink, B.
09c0bc5c-8f86-4668-bb83-7adbd2f58482
Stergioulas, N.
ccca6b37-49a6-41e6-9447-59af0073af4e
Hawke, I.
fc964672-c794-4260-a972-eaf818e7c9f4
Ott, C.
55df56da-1987-44bd-867e-4a6ab1b0b4fa
Schnetter, E.
544c2aff-bf71-45af-8d32-230f486eb837
Muller, E.
7a49be0a-3dbe-4e0d-9b00-5daa874f5762
Zink, B.
09c0bc5c-8f86-4668-bb83-7adbd2f58482
Stergioulas, N.
ccca6b37-49a6-41e6-9447-59af0073af4e
Hawke, I.
fc964672-c794-4260-a972-eaf818e7c9f4
Ott, C.
55df56da-1987-44bd-867e-4a6ab1b0b4fa
Schnetter, E.
544c2aff-bf71-45af-8d32-230f486eb837
Muller, E.
7a49be0a-3dbe-4e0d-9b00-5daa874f5762

Zink, B., Stergioulas, N., Hawke, I., Ott, C., Schnetter, E. and Muller, E. (2007) Non-axisymmetric instability and fragmentation of general relativistic quasi-toroidal stars. Physical Review D, 76 (2), 24019. (doi:10.1103/PhysRevD.76.024019).

Record type: Article

Abstract

In 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.

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More information

Submitted date: 19 November 2006
Published date: 31 July 2007

Identifiers

Local EPrints ID: 45408
URI: http://eprints.soton.ac.uk/id/eprint/45408
ISSN: 1550-7998
PURE UUID: b8e1fe5e-5803-4cf3-8ef5-751259a80247
ORCID for I. Hawke: ORCID iD orcid.org/0000-0003-4805-0309

Catalogue record

Date deposited: 03 Apr 2007
Last modified: 28 Jun 2022 01:41

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Contributors

Author: B. Zink
Author: N. Stergioulas
Author: I. Hawke ORCID iD
Author: C. Ott
Author: E. Schnetter
Author: E. Muller

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