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Dynamical evolution of quasi-circular binary black hole data

Dynamical evolution of quasi-circular binary black hole data
Dynamical evolution of quasi-circular binary black hole data
We study the fully nonlinear dynamical evolution of binary black hole data, whose orbital parameters are specified via the effective potential method for determining quasicircular orbits. The cases studied range from the Cook-Baumgarte innermost stable circular orbit (ISCO) to significantly beyond that separation. In all cases we find the black holes to coalesce (as determined by the appearance of a common apparent horizon) in less than half an orbital period. The results of the numerical simulations indicate that the initial holes are not actually in quasicircular orbits, but that they are in fact nearly plunging together. The dynamics of the final horizon are studied to determine physical parameters of the final black hole, such as its spin, mass, and oscillation frequency, revealing information about the inspiral process. We show that considerable resolution is required to extract accurate physical information from the final black hole formed in the merger process, and that the quasinormal modes of the final hole are strongly excited in the merger process. For the ISCO case, by comparing physical measurements of the final black hole formed to the initial data, we estimate that less than 3% of the total energy is radiated in the merger process.
black holes general relativity, gravitation
1550-7998
044004-[14pp]
Alcubierre, Miguel
2ee2ed0c-724d-4187-8a26-714d9b9a0412
Brügmann, Bernd
9424ecb8-7385-4d05-93ec-f63be05e3326
Diener, Peter
62485bb0-81d7-49df-b5ad-8f66610efc55
Guzmán, F. Siddhartha
6b413744-af94-4d63-aaac-12aa33158133
Hawke, Ian
fc964672-c794-4260-a972-eaf818e7c9f4
Hawley, Scott
6aaa8998-732f-4792-9983-9e64fb058cd7
Herrmann, Frank
5976ca5e-ac4a-4d57-b082-2ad0a610d0a3
Koppitz, Michael
059b34af-e573-4af7-b31a-161f192643d7
Pollney, Denis
a78b371e-934f-4fed-8754-91db5cdeb23e
Seidel, Edward
d58d753d-3707-4ae5-8227-92ed69a122ac
Thornburg, Jonathan
7164281d-b614-40e4-a27f-c89e874a7b9b
Alcubierre, Miguel
2ee2ed0c-724d-4187-8a26-714d9b9a0412
Brügmann, Bernd
9424ecb8-7385-4d05-93ec-f63be05e3326
Diener, Peter
62485bb0-81d7-49df-b5ad-8f66610efc55
Guzmán, F. Siddhartha
6b413744-af94-4d63-aaac-12aa33158133
Hawke, Ian
fc964672-c794-4260-a972-eaf818e7c9f4
Hawley, Scott
6aaa8998-732f-4792-9983-9e64fb058cd7
Herrmann, Frank
5976ca5e-ac4a-4d57-b082-2ad0a610d0a3
Koppitz, Michael
059b34af-e573-4af7-b31a-161f192643d7
Pollney, Denis
a78b371e-934f-4fed-8754-91db5cdeb23e
Seidel, Edward
d58d753d-3707-4ae5-8227-92ed69a122ac
Thornburg, Jonathan
7164281d-b614-40e4-a27f-c89e874a7b9b

Alcubierre, Miguel, Brügmann, Bernd, Diener, Peter, Guzmán, F. Siddhartha, Hawke, Ian, Hawley, Scott, Herrmann, Frank, Koppitz, Michael, Pollney, Denis, Seidel, Edward and Thornburg, Jonathan (2005) Dynamical evolution of quasi-circular binary black hole data. Physical Review D, 72 (4), 044004-[14pp]. (doi:10.1103/PhysRevD.72.044004).

Record type: Article

Abstract

We study the fully nonlinear dynamical evolution of binary black hole data, whose orbital parameters are specified via the effective potential method for determining quasicircular orbits. The cases studied range from the Cook-Baumgarte innermost stable circular orbit (ISCO) to significantly beyond that separation. In all cases we find the black holes to coalesce (as determined by the appearance of a common apparent horizon) in less than half an orbital period. The results of the numerical simulations indicate that the initial holes are not actually in quasicircular orbits, but that they are in fact nearly plunging together. The dynamics of the final horizon are studied to determine physical parameters of the final black hole, such as its spin, mass, and oscillation frequency, revealing information about the inspiral process. We show that considerable resolution is required to extract accurate physical information from the final black hole formed in the merger process, and that the quasinormal modes of the final hole are strongly excited in the merger process. For the ISCO case, by comparing physical measurements of the final black hole formed to the initial data, we estimate that less than 3% of the total energy is radiated in the merger process.

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More information

Published date: August 2005
Keywords: black holes general relativity, gravitation

Identifiers

Local EPrints ID: 29317
URI: http://eprints.soton.ac.uk/id/eprint/29317
ISSN: 1550-7998
PURE UUID: 84077bca-df13-477b-9b0a-9ca37fd23383
ORCID for Ian Hawke: ORCID iD orcid.org/0000-0003-4805-0309

Catalogue record

Date deposited: 11 May 2006
Last modified: 10 Dec 2019 01:44

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Contributors

Author: Miguel Alcubierre
Author: Bernd Brügmann
Author: Peter Diener
Author: F. Siddhartha Guzmán
Author: Ian Hawke ORCID iD
Author: Scott Hawley
Author: Frank Herrmann
Author: Michael Koppitz
Author: Denis Pollney
Author: Edward Seidel
Author: Jonathan Thornburg

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