Bulletin of the American Physical Society
2006 APS April Meeting
Saturday–Tuesday, April 22–25, 2006; Dallas, TX
Session Q11: Simulations of Binary Black Hole Mergers |
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Sponsoring Units: GGR Chair: Carlos Lousto, The University of Texas at Brownsville Room: Hyatt Regency Dallas Cumberland E |
Monday, April 24, 2006 1:30PM - 1:42PM |
Q11.00001: Accurate Evolutions of Orbiting Black Hole Binaries Without Excision Yosef Zlochower, Manuela Campanelli, Carlos Lousto We present a new technique for evolving moving black holes without excision. Our technique, which is based on a regularization of the standard `puncture' approach to the BSSN evolution system, allows for stable evolution of orbiting black-hole binaries. We used this technique to evolve a set of pre-ISCO binaries and show the resulting waveforms as well as the tracks of the individual horizons. [Preview Abstract] |
Monday, April 24, 2006 1:42PM - 1:54PM |
Q11.00002: Unequal-Mass Binary Black Hole Inspirals Deirdre Shoemaker, Frank Herrmann, Pablo Laguna We present results from fully nonlinear simulations of inspiralling, unequal mass binary black holes. We show waveforms of the dominant $l=2,3$ modes. The power spectrum of these modes yields insight on how the mass ratio in a binary impacts the degree of complexity of the emitted waveforms. In addition, we provide approximate estimates of energy and angular momentum radiated as well as kick velocities from gravitational radiation recoil. [Preview Abstract] |
Monday, April 24, 2006 1:54PM - 2:06PM |
Q11.00003: Binary Black Hole Evolutions with Moving Punctures: Methods and Numerical Codes. Pedro Marronetti, Wolfgang Tichy, Bernd Bruegmann Binary Black Holes are strong emitters of gravitational waves and their behavior during the last few orbits can only be accurately described by full general relativistic simulations. Here we present the numerical techniques and programs used for the simulation of such binaries. Our evolutions are performed using the BSSN formulation and the recently introduced ``moving punctures'' technique. We present the details of our numerical setup, as well as gauge choices and boundary conditions. [Preview Abstract] |
Monday, April 24, 2006 2:06PM - 2:18PM |
Q11.00004: Binary Black Hole Evolutions with Moving Punctures: Final orbits, merger and ringdown. Wolfgang Tichy, Pedro Marronetti, Bernd Bruegmann We present results of simulations of black hole binaries in circular orbits covering the last orbit and the merger and ringdown phases. These simulations are performed using the BSSN formulation and the recently introduced ``moving punctures'' technique. We compare different implementations of this technique and discuss how they affect convergence. We also cover in detail the results of our orbiting punctures simulations and their dependence on grid size and resolution. In addition, we discuss quality control curves and constraint satisfaction. [Preview Abstract] |
Monday, April 24, 2006 2:18PM - 2:30PM |
Q11.00005: How to move a black hole James van Meter, John Baker, Joan Centrella, Dae-Il Choi, Michael Koppitz Recent demonstrations of uncexcised, puncture black holes traversing freely across computational grids represent a revolutionary advance in numerical relativity. Stable and accurate simulations of multiple orbits, and their radiated waves, have resulted. This capability is critically undergirded by careful choices of gauge and formulation of the evolution equations. Here we describe the relevant techniques, analytically justify their necessity, and numerically demonstrate their efficacy. [Preview Abstract] |
Monday, April 24, 2006 2:30PM - 2:42PM |
Q11.00006: Gravitational waveforms from equal mass binary black hole systems Michael Koppitz, John Baker, Dae-Il Choi, Joan Centrella, James van Meter Using recently developed techniques for evolving binary black hole systems we report on evolutions of black holes through orbits, merger, and subsequent ringdown. The evolutions show stability and accuracy such that we can report convergent waveforms and energy conservation. The influence of the initial data is evaluated, the dependency of the dynamics from the initial separation tested, and a heuristic waveform template presented. [Preview Abstract] |
Monday, April 24, 2006 2:42PM - 2:54PM |
Q11.00007: Gravitational Radiation Recoil from Merging Massive Black Hole Binaries Dae-Il Choi, John Baker, Joan Centrella, Michael Koppitz, Jim van Meter One key area of interest for numerical relativity is calculation of kicks in merging massive black hole binaries where linear momentum, as well as energy and angular momentum, is lost due to asymmetric radiation of gravitational waves. As a result, the merger remnant receives a kick also known as gravitational rocket effect. High kick velocities, comparable or higher than escape velocites of the host structures, will provide a critical input to our understanding of various aspects of massive black hole evolutions in the universe. I describe a recent calculation of the kick velocities from simulations of the merging massive black hole binaries. Starting from reasonable initial data for quasi-circular configurations of non-equal mass and non-spinning black hole binary, simulations are carried out through merger and ringdown. From mergers with different mass ratio and different initial separations, kick velocities are estimated based on gravitational waveforms extracted in the wave-zone. I discuss astrophysical implications of the magnitude of the kicks. [Preview Abstract] |
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