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Gravitational Radiation from a Kerr Black Hole. I. Formulation and a Method for Numerical Analysis
Open accessAbstract
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 0.0170µc2 (µ/M) when a = 0.99M, which is 1.65 times larger than that when a = 0, i.e., the Schwarzschild case.
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Citations
Cited by
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Metadata
- Authors
- Sasaki, M., & Nakamura, T.
- Venue
- Progress of Theoretical Physics
- Publisher
- Oxford University Press (OUP)
- Published
- 1982-06-01
- Volume
- 67
- Issue
- 6
- Pages
- 1788-1809
- ISSN
- 0033-068X (ISSN-L)
- 1347-4081
- OpenAlex
- W2013856706
- Cited by
- 197
- References
- 0
- FWCI
- 1.82
- Type
- journal article
- Language
- en
- Open access
- bronze
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- Sasaki, M., & Nakamura, T. (1982). Gravitational Radiation from a Kerr Black Hole. I. Formulation and a Method for Numerical Analysis. Progress of Theoretical Physics. https://doi.org/10.1143/ptp.67.1788
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