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 J10: Numerical Simulations of Black Hole Binaries |
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Sponsoring Units: GGR Chair: Frans Pretorius, Princeton University Room: Hyatt Regency St. Louis Riverfront (formerly Adam's Mark Hotel), St. Louis A |
Sunday, April 13, 2008 10:45AM - 10:57AM |
J10.00001: Highly-Spinning-Black-Hole Binaries Yosef Zlochower, Carlos Lousto, Manuela Campanelli In this talk I will show recent results obtained by the RIT group from simulations of highly-spinning-black-hole binaries using the moving puncture approach; paying particular attention to the phenomena of superkicks, orbital hangup, and cosmic censorship. Simulations of highly spinning binaries are challenging both due to the amount of spurious radiation introduced by the initial data choice, which introduces unwanted eccentricity, and the smallness of the horizons. Accurate results can be obtained with long evolutions and very fine central resolutions. [Preview Abstract] |
Sunday, April 13, 2008 10:57AM - 11:09AM |
J10.00002: Further insight into gravitational recoil Carlos Lousto, Yosef Zlochower, Manuela Campanelli We test the accuracy of our recently proposed empirical formula to model the recoil velocity imparted to the merger remnant of spinning, unequal-mass black-hole binaries. We study three families of black-hole binary configurations, all with mass ratio q=3/8 (to maximize the unequal-mass contribution to the kick) and spins aligned (or counter aligned) with the orbital angular momentum, two with spin configurations chosen to minimize the spin-induced tangential and radial accelerations of the trajectories respectively, and a third family where the trajectories are significantly altered by spin-orbit coupling. We find good agreement between the measured and predicted recoil velocities for the first two families, and reasonable agreement for the third. We also re-examine our original generic binary configuration that led to the discovery of extremely large spin-driven recoil velocities and inspired our empirical formula, and find reasonable agreement between the predicted and measured recoil speeds. [Preview Abstract] |
Sunday, April 13, 2008 11:09AM - 11:21AM |
J10.00003: The final spin in unbound black hole mergers Pablo Laguna, Matthew Washik, Richard Matzner, Deirdre Shoemaker, Frank Herrmann, Ian Hinder The spin of the final black hole produced by the merger of a binary black hole system is approximately determined by the combination of orbital angular momentum, spins of the coalescing black holes and radiated angular momentum at the point when the binary enters the plunge. In circular or low eccentricity inspirals, numerical simulations have shown that, although there is a substantial amount ($\sim 20\%$) of angular momentum radiated, the spin of the final black hole is dominated by the orbital angular momentum. To further explore the role played by the orbital angular momentum, we present results from \emph{parabolic} and \emph{hyperbolic} encounters. Because the radiated angular momentum for these mergers is significantly lower, we are able to construct initial configurations that yield spin flipping as well as spinning-up of the final black hole significantly different from those in circular orbits. [Preview Abstract] |
Sunday, April 13, 2008 11:21AM - 11:33AM |
J10.00004: Robustness of Binary Black Hole Mergers in the Presence of Spurious Radiation Tanja Bode, Deirdre Shoemaker, Frank Herrmann, Ian Hinder We present an investigation into how sensitive the last orbits and merger of binary black hole systems are to the presence of spurious radiation in the initial data. Our numerical experiments consist of a binary black hole system starting the last couple of orbits before merger with additional spurious radiation centered at the origin and fixed initial angular momentum. As the energy in the added spurious radiation increases, the binary is invariably hardened for the cases we tested, i.e. the merger of the two black holes is hastened. The change in merger time becomes significant when the additional energy provided by the spurious radiation increases the $M_{\mathrm{ADM}}$ of the spacetime by about 1\%. While the final masses of the black holes increase due to partial absorption of the radiation, the final spins remain constant to within our numerical accuracy. We conjecture that the spurious radiation is primarily increasing the eccentricity of the orbit and secondarily increasing the mass of the black holes while propagating out to infinity. [Preview Abstract] |
Sunday, April 13, 2008 11:33AM - 11:45AM |
J10.00005: High-spin binary black hole mergers Pedro Marronetti, Wolfgang Tichy, Bernd Br\"ugmann, Ulrich Sperhake, Jos\'e Gonz\'alez We study identical mass black hole binaries with spins perpendicular to the binary's orbital plane. These binaries have individual spins ranging from $s/m^2=-0.90$ to $0.90$, ($s_1 = s_2$ in all cases) which is near the limit possible with standard Bowen-York puncture initial data. The extreme cases correspond to the largest initial spin simulations to date. Our results expand the parameter space covered by Rezzolla {\it et al}. and, when combining both data sets, we obtain estimations for the minimum and maximum values for the intrinsic angular momenta of the remnant of binary black hole mergers of $J/M^2=0.341(4)$ and $0.951(4)$ respectively. [Preview Abstract] |
Sunday, April 13, 2008 11:45AM - 11:57AM |
J10.00006: The Final Spin of Black Hole Binaries Erik Schnetter The evolution from the initial to the final state of a generic binary black hole system can be viewed as black box, with just a few input and output parameters such as masses and spins. Combining a series of numerical simulations and certain reasonable assumptions, we derive accurate analytic expressions describing the final state after the merger process, for the case of aligned spins and non-eccentric orbits. [Preview Abstract] |
Sunday, April 13, 2008 11:57AM - 12:09PM |
J10.00007: Simulations of binary black holes with spin Wolfgang Tichy, Pedro Marronetti We present results of simulations of spinning black hole binaries on initially quasi-circular orbits. Our simulations cover several orbits as well as the merger and ringdown phases. We compare the initial and final mass and angular momentum of each system, and give error estimates for our results. [Preview Abstract] |
Sunday, April 13, 2008 12:09PM - 12:21PM |
J10.00008: Describing Waveforms from Nonspinning Black Hole Binaries William Darian Boggs, John G. Baker, Joan Centrella, Bernard J. Kelly, Sean T. McWilliams, James R. van Meter Following successful simulations of the inspiral and merger of a black hole binary, the parameter space survey of black hole binary simulations is underway. Equal-mass simulations and waveforms have been studied thoroughly. Mergers with various spins on the individual black holes have been simulated. We have simulated the last several orbits of nonspinning mergers with mass ratios up to 1:6. We focus on the waveforms from such mergers, with an emphasis on interpreting the phase evolution by a simple heuristic model. [Preview Abstract] |
Sunday, April 13, 2008 12:21PM - 12:33PM |
J10.00009: Comparison of numerical relativity simulations with post-Newtonian expansions, Pade and EOB models Abdul Hussein Mroue, Saul Teukolsky, Lawrence Kidder, Harald Pfeiffer, Michael Boyle, Mark Scheel, Alessandra Buonanno, Yi Pan In order to detect GWs and measure the physical parameters of coalescing black hole binaries, a large bank of templates is required to accurately represent the GW waveforms emitted by these binaries. Since Numerical Relativity cannot densely sample the parameter space, different analytical methods are developed to compute these waveforms. We compare our recent numerical gravitational waveforms with those from post-Newtonian formulae, their various Pade transforms, and the different Effective-One-Body models. [Preview Abstract] |
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