Reducing eccentricity in black-hole binary evolutions with initial parameters from post-Newtonian inspiral

Simple item page
dc.creatorHusa, Sascha
dc.creatorHannam, Mark
dc.creatorGonzalez, Jose A.
dc.creatorSperhake, Ulrich
dc.creatorBruegmann, Bernd
dc.date2007-06-07
dc.date.accessioned2026-07-07T11:56:55Z
dc.date.available2026-07-07T11:56:55Z
dc.descriptionStandard choices of quasi-circular orbit parameters for black-hole binary evolutions result in eccentric inspiral. We introduce a conceptually simple method, which is to integrate the post-Newtonian equations of motion through hundreds of orbits, and read off the values of the momenta at the separation at which we wish to start a fully general relativistic numerical evolution. For the particular case of non-spinning equal-mass inspiral with an initial coordinate separation of $D = 11M$ we show that this approach reduces the eccentricity by at least a factor of five to $e < 0.002$ as compared to using standard quasi-circular initial parameters.
dc.description6 pages, 3 figures, 1 table
dc.identifierhttps://arxiv.org/abs/0706.0904
dc.identifierhttp://arxiv.org/abs/0706.0904
dc.identifierPhys.Rev.D77:044037,2008
dc.identifierdoi:10.1103/PhysRevD.77.044037
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/205702
dc.subjectGeneral Relativity and Quantum Cosmology
dc.titleReducing eccentricity in black-hole binary evolutions with initial parameters from post-Newtonian inspiral
dc.typetext

Files

Collections

arXiv