Bulletin of the American Physical Society
2008 APS April Meeting and HEDP/HEDLA Meeting
Volume 53, Number 5
Friday–Tuesday, April 11–15, 2008; St. Louis, Missouri
Session X7: Numerical Relativity Meets the Post Newtonian Approximation |
Hide Abstracts |
Sponsoring Units: GGR Chair: Clifford Will, Washington University Room: Hyatt Regency St. Louis Riverfront (formerly Adam's Mark Hotel), Rose Garden |
Tuesday, April 15, 2008 1:30PM - 2:06PM |
X7.00001: Post-Newtonian diagnostics for initial data Invited Speaker: Using a post-Newtonian diagnostic tool developed by Mora and Will, we examine numerically generated quasiequilibrium initial data sets used in numerical evolutions of black hole-black hole, neutron star-neutron star and neutron star-black hole binary systems. The post-Newtonian equations include the effects of tidal interactions, parametrized by the compactness of the neutron stars and by suitable values of ``apsidal'' constants, which measure the degree of distortion of stars subjected to tidal forces. We find that the post-Newtonian diagnostic agrees well with black hole-black hole and neutron star-neutron star initial data, except where tidal distortions are becoming extreme. In comparing the diagnostic with preliminary numerical data on neutron star-black hole binaries, we find less agreement. We show that the differences could be interpreted as representing small residual eccentricity in the initial orbits. [Preview Abstract] |
Tuesday, April 15, 2008 2:06PM - 2:42PM |
X7.00002: Matching of PN Waveforms with long-time numerical evolutions Invited Speaker: Numerical simulations of 15 orbits of an equal-mass binary black hole system are presented. Gravitational waveforms from these simulations, covering more than 30 cycles before merger, are compared with those from quasi-circular zero-spin post-Newtonian (PN) formulae. The cumulative phase uncertainty of these comparisons is about 0.05 radians, dominated by effects arising from the small residual spins of the black holes and the small residual orbital eccentricity in the simulations. Matching numerical results to PN waveforms early in the run yields excellent agreement (within 0.05 radians) over the first 15 cycles, thus validating the numerical simulation and establishing a regime where PN theory is accurate. In the last 15 cycles to merger, however, {\em generic} time-domain Taylor approximants build up phase differences of several radians. I will also discuss preliminary results from more recent simulations with unequal masses and spins. [Preview Abstract] |
Tuesday, April 15, 2008 2:42PM - 3:18PM |
X7.00003: Developing templates for binary black hole coalescences using analytical and numerical relativity Invited Speaker: We shall review the comparisons between analytical and numerical relativity waveforms with the goal of building an analytical template family for inspiral, merger and ring-down phases. The new analytical template family which combines the Post-Newtonian re-summed dynamics a la effective-one-body and non-perturbative numerical relativity information may already be employed for coherent searches and parameter estimation of gravitational waves emitted by non-spinning coalescing binary black holes, and can be extended to binaries with spinning black holes. [Preview Abstract] |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2024 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
100 Motor Pkwy, Suite 110, Hauppauge, NY 11788
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700