Modeling gravitational radiation from coalescing binary black holes

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With the goal of bringing theory, particularly numerical relativity, to bear on an astrophysical problem of critical interest to gravitational wave observers we introduce a model for coalescence radiation from binary black hole systems. We build our model using the Lazarus approach, a technique that...

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Detalles Bibliográficos
Autor principal: Baker, J.
Otros Autores: Campanelli, M., Lousto, C.O, Takahashi, R.
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2002
Acceso en línea:Registro en Scopus
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Registro en la Biblioteca Digital
Aporte de:Registro referencial: Solicitar el recurso aquí
Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Baker, J. 
245 1 0 |a Modeling gravitational radiation from coalescing binary black holes 
260 |c 2002 
270 1 0 |m Baker, J.; Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States 
506 |2 openaire  |e Política editorial 
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504 |a note 
520 3 |a With the goal of bringing theory, particularly numerical relativity, to bear on an astrophysical problem of critical interest to gravitational wave observers we introduce a model for coalescence radiation from binary black hole systems. We build our model using the Lazarus approach, a technique that bridges far and close limit approaches with full numerical relativity to solve Einstein equations applied in the truly nonlinear dynamical regime. We specifically study the post-orbital radiation from a system of equal-mass non-spinning black holes, deriving waveforms which indicate strongly circularly polarized radiation of roughly 3% of the system's total energy and 12% of its total angular momentum in just a few cycles. To support this result we first establish the reliability of the late-time part of our model, including the numerical relativity and close-limit components, with a thorough study of waveforms from a sequence of black hole configurations that varies from previously treated head-on collisions to a representative target for "ISCO" data corresponding to the end of the inspiral period. We then complete our model with a simple treatment for the early part of the spacetime based on a standard family of initial data for binary black holes in circular orbit. A detailed analysis shows strong robustness in the results as the initial separation of the black holes is increased from 5.0 to 7.8M supporting our waveforms as a suitable basic description of the astrophysical radiation from this system. Finally, a simple fitting of the plunge waveforms is introduced as a first attempt to facilitate the task of analyzing data from gravitational wave detectors. © 2002 The American Physical Society.  |l eng 
593 |a Laboratory for High Energy Astrophysics, NASA Goddard Space Flight Center, Greenbelt, MD 20771, United States 
593 |a Department of Physics and Astronomy, University of Texas at Brownsville, Brownsville, TX 78520, United States 
593 |a Instituto de Astronomía y Física del Espacio, CONICET, Buenos Aires, Argentina 
593 |a Theoretical Astrophysics Center, Dk-2100 Køabenhavn Ø, Denmark 
690 1 0 |a ARTICLE 
690 1 0 |a COSMIC RADIATION 
690 1 0 |a COSMOS 
690 1 0 |a ENERGY 
690 1 0 |a GRAVITY 
690 1 0 |a MATHEMATICAL MODEL 
690 1 0 |a NONLINEAR SYSTEM 
690 1 0 |a QUANTUM THEORY 
690 1 0 |a SPACE 
690 1 0 |a TIME 
690 1 0 |a WAVEFORM 
700 1 |a Campanelli, M. 
700 1 |a Lousto, C.O. 
700 1 |a Takahashi, R. 
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