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          Institute: MPI für Gravitationsphysik     Collection: Astrophysical Relativity     Display Documents



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ID: 433311.0, MPI für Gravitationsphysik / Astrophysical Relativity
Gravitational-wave detectability of equal-mass black-hole binaries with aligned spins
Authors:Reisswig, Christian; Husa, Sascha; Rezzolla, Luciano; Dorband, Ernst Nils; Pollney, Denis; Seiler, Jennifer
Date of Publication (YYYY-MM-DD):2009
Title of Journal:Physical Review D
Volume:80
Sequence Number of Article:124026
Review Status:not specified
Audience:Not Specified
Abstract / Description:Binary black-hole systems with spins aligned or anti-aligned to the orbital angular momentum provide the natural ground to start detailed studies of the influence of strong-field spin effects on gravitational wave observations of coalescing binaries. Furthermore, such systems may be the preferred end-state of the inspiral of generic supermassive binary black-hole systems. In view of this, we have computed the inspiral and merger of a large set of binary systems of equal-mass black holes with spins parallel to the orbital angular momentum but otherwise arbitrary. Our attention is particularly focused on the gravitational-wave emission so as to quantify how much spin effects contribute to the signal-to-noise ratio, to the horizon distances, and to the relative event rates for the representative ranges in masses and detectors. As expected, the signal-to-noise ratio increases with the projection of the total black hole spin in the direction of the orbital momentum. We find that equal-spin binaries with maximum spin aligned with the orbital angular momentum are more than ``three times as loud'' as the corresponding binaries with anti-aligned spins, thus corresponding to event rates up to 30 times larger. We also consider the waveform mismatch between the different spinning configurations and find that, within our numerical accuracy, binaries with opposite spins S_1=-S_2 cannot be distinguished whereas binaries with spin S_1=S_2 have clearly distinct gravitational-wave emissions. Finally, we derive a simple expression for the energy radiated in gravitational waves and find that the binaries always have efficiencies E_rad/M > 3.6%, which can become as large as E_rad/M = 10% for maximally spinning binaries with spins aligned with the orbital angular momentum.
External Publication Status:published
Document Type:Article
Communicated by:Bernhard F. Schutz
Affiliations:MPI für Gravitationsphysik/Astrophysical Relativity
Identifiers:LOCALID:arXiv:0907.0462
DOI:10.1103/PhysRevD.80.124026
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