Gravitational Radiation from a Kerr Black Hole. I : Formulation and a Method for Numerical Analysis
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概要
- 論文の詳細を見る
A class of new inhomogeneous equations governing gravitational perturbations of the Kerr Geometry is presented. It is shown that, contrary to the case of the Teukolsky equation, the perturbation equations have short-range potential and no divergent source terms for large distance. Using one of such equations which seems to be the simplest, we have computed the spectrum and the energy of gravitational radiation induced by a test particle of mass μ falling along the z-axis into a Kerr black hole of mass M(≫μ) and angular momentum Ma(a<M). It is found that the total energy radiated is 0.0170μc^2 (μ/M) when a=0.99M, which is 1.65 times larger than that when a=0, i.e., the Schwarzschild case.
- 理論物理学刊行会の論文
- 1982-06-25
著者
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Sasaki Misao
Research Institute For Fundamental Physics Kyoto University
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Sasaki Masao
Research Institute For Bioresources Okayama University
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NAKAMURA Takashi
Research Institute for Fundamental Physics Kyoto University
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Sasaki Masao
Research Institute For Fumdamental Physics Kyoto University
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