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Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/3935
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dc.contributor.authorArun, K.G.-
dc.contributor.authorBlanchet, Luc-
dc.contributor.authorIyer, B.R.-
dc.contributor.authorSinha, Siddhartha-
dc.date.accessioned2010-07-22T08:45:07Z-
dc.date.available2010-07-22T08:45:07Z-
dc.date.issued2009-12-11-
dc.identifier.citationPhysical Review D, 2009, Vol.80, p124018en
dc.identifier.issn1550-2368 (Online)-
dc.identifier.issn1550-7998-
dc.identifier.urihttp://hdl.handle.net/2289/3935-
dc.descriptionOpen Access.en
dc.description.abstractThe angular-momentum flux from an inspiralling binary system of compact objects moving in quasi-elliptical orbits is computed at the third post-Newtonian (3PN) order using the multipolar post-Minkowskian wave generation formalism. The 3PN angular-momentum flux involves the instantaneous, tail, and tail-of-tails contributions as for the 3PN energy flux, and in addition a contribution due to nonlinear memory. We average the angular-momentum flux over the binary’s orbit using the 3PN quasi-Keplerian representation of elliptical orbits. The averaged angular-momentum flux provides the final input needed for gravitational-wave phasing of binaries moving in quasi-elliptical orbits. We obtain the evolution of orbital elements under 3PN gravitational radiation reaction in the quasi-elliptic case. For small eccentricities, we give simpler limiting expressions relevant for phasing up to order e2. This work is important for the construction of templates for quasi-eccentric binaries, and for the comparison of post-Newtonian results with the numerical relativity simulations of the plunge and merger of eccentric binaries.en
dc.language.isoenen
dc.publisherAmerican Physical Societyen
dc.relation.urihttp://arxiv.org/abs/0908.3854en
dc.relation.urihttp://dx.doi.org/ 10.1103/PhysRevD.80.124018en
dc.relation.urihttp://adsabs.harvard.edu/abs/2009PhRvD..80l4018Aen
dc.rights2009 The American Physical Societyen
dc.titleThird post-Newtonian angular momentum flux and the secular evolution of orbital elements for inspiralling compact binaries in quasi-elliptical orbitsen
dc.typeArticleen
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