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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/6126
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dc.contributor.authorFaye, Guillaume-
dc.contributor.authorMarsat, Sylvain-
dc.contributor.authorBlanchet, Luc-
dc.contributor.authorIyer, B.R.-
dc.date.accessioned2015-01-05T04:56:05Z-
dc.date.available2015-01-05T04:56:05Z-
dc.date.issued2012-09-07-
dc.identifier.citationClassical and Quantum Gravity, 2012, Vol.29, P 175004en
dc.identifier.issn0264-9381-
dc.identifier.issn1361-6382 (E)-
dc.identifier.urihttp://hdl.handle.net/2289/6126-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractWe compute the quadrupole mode of the gravitational waveform of inspiralling compact binaries at the third and half-post-Newtonian (3.5PN) approximation of general relativity. The computation is performed using the multipolar post-Newtonian formalism, and restricted to binaries without spins moving on quasi-circular orbits. The new inputs mainly include the 3.5PN terms in the mass quadrupole moment of the source, and the control of required subdominant corrections to the contributions of hereditary integrals (tails and nonlinear memory effect). The result is given in the form of the quadrupolar mode (2, 2) in a spin-weighted spherical harmonic decomposition of the waveform, and may be used for comparison with the counterpart quantity computed in numerical relativity. It is a step towards the computation of the full 3.5PN waveform, whose knowledge is expected to reduce the errors on the location parameters of the source.en
dc.language.isoenen
dc.publisherIOP Publishingen
dc.relation.urihttp://arxiv.org/abs/1204.1043en
dc.relation.urihttp://dx.doi.org/10.1088/0264-9381/29/17/175004en
dc.relation.urihttp://adsabs.harvard.edu/abs/2012CQGra..29q5004Fen
dc.rights2012 IOP Publishing Ltd.en
dc.titleThe third and a half post-Newtonian gravitational wave quadrupole mode for quasi-circular inspiralling compact binariesen
dc.typeArticleen
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