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Accuracy of gravitational waveform models for observing neutron-star–black-hole binaries in Advanced LIGO

Nitz, Alexander H. and Lundgren, Andrew and Brown, Duncan A. and Ochsner, Evan and Keppel, Drew and Harry, Ian W. (2013) Accuracy of gravitational waveform models for observing neutron-star–black-hole binaries in Advanced LIGO. Physical Review D, 88 (12). Art. No. 124039. ISSN 2470-0010. doi:10.1103/PhysRevD.88.124039. https://resolver.caltech.edu/CaltechAUTHORS:20140402-093450958

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Abstract

Gravitational waves radiated by the coalescence of compact-object binaries containing a neutron star and a black hole are one of the most interesting sources for the ground-based gravitational-wave observatories Advanced LIGO and Advanced Virgo. Advanced LIGO will be sensitive to the inspiral of a 1.4M⊙ neutron star into a 10M⊙ black hole to a maximum distance of ∼900  Mpc. Achieving this sensitivity and extracting the physics imprinted in observed signals requires accurate modeling of the binary to construct template waveforms. In a neutron-star–black-hole binary, the black hole may have significant angular momentum (spin), which affects the phase evolution of the emitted gravitational waves. We investigate the ability of currently available post-Newtonian templates to model the gravitational waves emitted during the inspiral phase of neutron-star–black-hole binaries. We restrict to the case where the spin of the black hole is aligned with the orbital angular momentum and compare several post-Newtonian approximants. We examine restricted amplitude post-Newtonian waveforms that are accurate to third-and-a-half post-Newtonian order in the orbital dynamics and complete to second-and-a-half post-Newtonian order in the spin dynamics. We also consider post-Newtonian waveforms that include the recently derived third-and-a-half post-Newtonian order spin-orbit correction and the third post-Newtonian order spin-orbit tail correction. We compare these post-Newtonian approximants to the effective-one-body waveforms for spin-aligned binaries. For all of these waveform families, we find that there is a large disagreement between different waveform approximants, starting at low to moderate black hole spins, particularly for binaries where the spin is antialigned with the orbital angular momentum. The match between the TaylorT4 and TaylorF2 approximants is ∼0.8 for a binary with m_BH/m_NS∼4 and χ_BH = cJ_BH/Gm^(2)_(BH)∼0.4. We show that the divergence between the gravitational waveforms begins in the early inspiral at v∼0.2 for χ_BH∼0.4. Post-Newtonian spin corrections beyond those currently known will be required for optimal detection searches and to measure the parameters of neutron-star–black-hole binaries. The strong dependence of the gravitational-wave signal on the spin dynamics will make it possible to extract significant astrophysical information from detected systems with Advanced LIGO and Advanced Virgo.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1103/PhysRevD.88.124039 DOIArticle
http://journals.aps.org/prd/abstract/10.1103/PhysRevD.88.124039PublisherArticle
http://arxiv.org/abs/1307.1757arXivWorking Paper
ORCID:
AuthorORCID
Brown, Duncan A.0000-0002-9180-5765
Additional Information:© 2013 American Physical Society. Received 6 July 2013; published 26 December 2013. We thank Stefan Ballmer, Alessandra Buonanno, Eliu Huerta, Prayush Kumar, Richard O’Shaughnessy, B. S. Sathyaprakash, Peter Saulson, and Matt West for useful discussions. This work is supported by National Science Foundation Awards No. PHY-0847611 (DAB, AHN), No. PHY-1205835 (AHN, IWH), No. PHY-0970074 (EO), and No. PHY-0855589 (AL). D. A. B., I.W. H., A. L., and E. O. thank the Kavli Institute for Theoretical Physics at Santa Barbara University, supported in part by NSF Grant No. PHY-0551164, for hospitality during this work. D. A. B. thanks the LIGO Laboratory Visitors Program, supported by NSF cooperative agreement No. PHY-0757058, for hospitality. D. K. and A.L. thank the Max Planck Gesellschaft for support. D.A.B. is supported by a Cottrell Scholar award from the Research Corporation for Science Advancement. Computations used in this work were performed on the Syracuse University Gravitation and Relativity cluster, which is supported by NSF Awards No. PHY-1040231 and No. PHY-1104371.
Funders:
Funding AgencyGrant Number
NSFPHY-0847611
NSFPHY-1205835
NSFPHY-0970074
NSFPHY-0855589
NSFPHY-0551164
NSF Cooperative AgreementPHY-0757058
Max Planck GesellschaftUNSPECIFIED
Research Corporation for Science Advancement Cottrell Scholar awardUNSPECIFIED
NSFPHY-1040231
NSFPHY-1104371
Issue or Number:12
Classification Code:PACS: 04.30.Db
DOI:10.1103/PhysRevD.88.124039
Record Number:CaltechAUTHORS:20140402-093450958
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20140402-093450958
Official Citation:Nitz, A. H., Lundgren, A., Brown, D. A., Ochsner, E., Keppel, D., & Harry, I. W. (2013). Accuracy of gravitational waveform models for observing neutron-star–black-hole binaries in Advanced LIGO. Physical Review D, 88(12), 124039.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:44599
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:02 Apr 2014 23:10
Last Modified:10 Nov 2021 16:54

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