Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/3824
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dc.contributor.authorFujita, Ryuichi-
dc.contributor.authorHikida, Wataru-
dc.contributor.authorTagoshi, H.-
dc.date.accessioned2009-07-31T11:09:15Z-
dc.date.available2009-07-31T11:09:15Z-
dc.date.issued2009-04-
dc.identifier.citationProgress of Theoretical Physics, 2009, Vol. 121, p843en
dc.identifier.issn0033-068X-
dc.identifier.issn1347-4081 (online)-
dc.identifier.urihttp://hdl.handle.net/2289/3824-
dc.descriptionRestricted Access. An open-access version is available at arXiv.org (one of the alternative locations)en
dc.description.abstractWe develop a numerical code to compute gravitational waves induced by a particle moving on eccentric inclined orbits around a Kerr black hole. For such systems, the black hole perturbation method is applicable. The gravitational waves can be evaluated by solving the Teukolsky equation with a point like source term, which is computed from the stress-energy tensor of a test particle moving on generic bound geodesic orbits. In our previous papers, we computed the homogeneous solutions of the Teukolsky equation using a formalism developed by Mano, Suzuki and Takasugi and showed that we could compute gravitational waves efficiently and very accurately in the case of circular orbits on the equatorial plane. Here, we apply this method to eccentric inclined orbits. The geodesics around a Kerr black hole have three constants of motion: energy, angular momentum and the Carter constant. We compute the rates of change of the Carter constant as well as those of energy and angular momentum. This is the first time that the rate of change of the Carter constant has been evaluated accurately. We also treat the case of highly eccentric orbits with e = 0.9. To confirm the accuracy of our codes, several tests are performed. We find that the accuracy is only limited by the truncation of \ell-, k- and n-modes, where \ell is the index of the spin-weighted spheroidal harmonics, and n and k are the harmonics of the radial and polar motion, respectively. When we set the maximum of \ell to 20, we obtain a relative accuracy of 10-5 even in the highly eccentric case of e = 0.9. The accuracy is better for lower eccentricity. Our numerical code is expected to be useful for computing templates of the extreme mass ratio inspirals, which is one of the main targets of the Laser Interferometer Space Antenna (LISA).en
dc.language.isoenen
dc.publisherProgress of Theoretical Physicsen
dc.relation.urihttp://arxiv.org/abs/0904.3810en
dc.relation.urihttp://dx.doi.org/10.1143/PTP.121.843en
dc.relation.urihttp://adsabs.harvard.edu/abs/2009PThPh.121..843Fen
dc.rights2009 Progress of Theoretical Physicsen
dc.titleAn efficient numerical method for computing gravitational waves induced by a particle moving on eccentric inclined orbits around a Kerr black holeen
dc.typeArticleen
Appears in Collections:Research Papers (TP)

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