2006/06/13 by Valeria Ferrari, Leonardo Gualtieri, Luciano Rezzolla
Mathematics · Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Black hole (networking) #Classical mechanics #Computer science #Domain (mathematical analysis) #General relativity #Geometry #Gravitation #Gravitational wave #Mathematical analysis #Mathematics #Nonlinear system #Numerical relativity #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Schwarzschild metric #Schwarzschild radius #Torus #astro-ph #gr-qc
paper · pdf · doi:10.1103/physrevd.73.124028
published as Phys.Rev. D73 (2006) 124028 · 12 pages, 4 figures. Phys. Rev. D, in press
arxiv created 2006/06/13 · openalex publication_date 2006/06/20 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present a new method for the calculation of black hole perturbations induced by extended sources in which the solution of the nonlinear hydrodynamics equations is coupled to a perturbative method based on Regge-Wheeler/Zerilli and Bardeen-Press-Teukolsky equations when these are solved in the frequency domain. In contrast to alternative methods in the time domain which may be unstable for rotating black hole spacetimes, this approach is expected to be stable as long as an accurate evolution of the matter sources is possible. Hence, it could be used under generic conditions and also with sources coming from three-dimensional numerical relativity codes. As an application of this method we compute the gravitational radiation from an oscillating high-density torus orbiting around a Schwarzschild black hole and show that our method is remarkably accurate, capturing both the basic quadrupolar emission of the torus and the excited emission of the black hole.