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The runaway instability in general relativistic accretion discs

Korobkin, O. and Abdikamalov, E. and Stergioulas, N. and Schnetter, E. and Zink, B. and Rosswog, S. and Ott, C. D. (2013) The runaway instability in general relativistic accretion discs. Monthly Notices of the Royal Astronomical Society, 431 (1). pp. 349-354. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20130613-111038739

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Abstract

When an accretion disc falls prey to the runaway instability, a large portion of its mass is devoured by the black hole within a few dynamical times. Despite decades of effort, it is still unclear under what conditions such an instability can occur. The technically most advanced relativistic simulations to date were unable to find a clear sign for the onset of the instability. In this work, we present three-dimensional relativistic hydrodynamics simulations of accretion discs around black holes in dynamical space–time. We focus on the configurations that are expected to be particularly prone to the development of this instability. We demonstrate, for the first time, that the fully self-consistent general relativistic evolution does indeed produce a runaway instability.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1093/mnras/stt166DOIUNSPECIFIED
http://mnras.oxfordjournals.org/content/431/1/349PublisherUNSPECIFIED
Additional Information:© 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2013 January 27. Received 2013 January 24; in original form 2012 October 1. First published online: February 23, 2013. We acknowledge stimulating discussions with P. Diener, P. Montero, C. Reisswig, M. Scheel, B. Szilágyi and J. Tohline. This work is supported by the National Science Foundation under grant numbers AST-1212170, PHY-1151197, PHY-1212460 and OCI-0905046, by the German Research Foundation grant DFGRO-3399, AOBJ-584282 and by the Sherman Fairchild and Alfred P. Sloan Foundation. NS acknowledges support by an Excellence Grant of the research committee of the Aristotle University of Thessaloniki. Supercomputing simulations for this paper were performed on the Compute Canada SHARCNET cluster ‘Orca’ (project CFZ-411-AA), Caltech compute cluster ‘Zwicky’ (NSF MRI award No. PHY-0960291), on the NSF XSEDE network under grant TG-PHY100033, on machines of the Louisiana Optical Network Initiative under grant loni_numrel07 and at the National Energy Research Scientific Computing Center (NERSC), which is supported by the Office of Science of the US Department of Energy under contract DE-AC03-76SF00098.
Funders:
Funding AgencyGrant Number
NSFAST-1212170
NSFPHY-1151197
NSFPHY-1212460
NSFOCI- 0905046
German Research FoundationRO-3399
German Research FoundationAOBJ-584282
Sherman Fairchild FoundationUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
Aristotle University of Thessaloniki Excellence GrantUNSPECIFIED
Compute Canada SHARCNET cluster “Orca”CFZ-411-AA
NSF MRIPHY-0960291
NSF XSEDE network grantTG-PHY100033
Louisiana Optical Network Initiativeloni_numrel07
Department of Energy (DOE) Office of ScienceDE-AC03-76SF00098
Subject Keywords: accretion, accretion disks black hole physics gravitation instabilities
Record Number:CaltechAUTHORS:20130613-111038739
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20130613-111038739
Official Citation: O. Korobkin, E. Abdikamalov, N. Stergioulas, E. Schnetter, B. Zink, S. Rosswog, and C. D. Ott The runaway instability in general relativistic accretion discs MNRAS (May 1, 2013) Vol. 431 349-354 first published online February 23, 2013 doi:10.1093/mnras/stt166
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:38944
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:13 Jun 2013 18:32
Last Modified:13 Jun 2013 18:32

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