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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/5401
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dc.contributor.authorMarsat, Sylvain-
dc.contributor.authorFaye, Guillaume-
dc.contributor.authorBlanchet, Luc-
dc.contributor.authorIyer, B.R.-
dc.date.accessioned2013-02-27T13:42:04Z-
dc.date.available2013-02-27T13:42:04Z-
dc.date.issued2012-
dc.identifier.citationASP Conference Series, 2012, Vol.467, p197 (Book Chapter)en
dc.identifier.issn978-1-58381-816-9-
dc.identifier.urihttp://hdl.handle.net/2289/5401-
dc.descriptionRestricted Access. Proceedings of 9th LISA Symposium Paris, France from 21-25 may 2012. Edited by Gerard Auger, Pierre Binétruy, and Eric Plagnol (en
dc.description.abstractWe present our 3.5PN computation of the (2,2) mode of the gravitational wave amplitude emitted by compact binaries, on quasi-circular orbits and in the absence of spins. We use the multipolar post-Newtonian wave generation formalism, extending and building on previous works which computed the 3PN order. This calculation required the extension of the multipolar post-Minkowskian algorithm, as well as the computation of the mass source quadrupole at 3.5PN order. Our result will allow more accurate comparisons to numerical relativity, and is a first step towards the computation of the full 3.5PN waveform amplitude, which would improve the estimation of the source parameters by gravitational wave detectorsen
dc.language.isoenen
dc.relation.urihttp://arxiv.org/abs/1210.2339en
dc.relation.urihttp://adsabs.harvard.edu/abs/bib_query?arXiv:1210.2339en
dc.rights2012 Astronomical Society of the Pacificen
dc.titlePost-Newtonian prediction for the (2,2) mode of the gravitational wave emitted by compact binariesen
dc.typeBook chapteren
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