Erratum: Evolution of circular, nonequatorial orbits of Kerr black holes due to gravitational-wave emission [Phys. Rev. D61, 084004 (2000)]
نویسندگان
چکیده
منابع مشابه
The evolution of circular, non-equatorial orbits of Kerr black holes due to gravitational-wave emission
An outstanding problem in general relativity is the evolution of binary systems with strong gravity and compact bodies. Although post-Newtonian approximations very successfully describe the evolution of such binaries when the bodies are widely separated [1], no approximation schemes work well when the bodies are close: in general, there is no small parameter that can be used to develop any appr...
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The effect of gravitational radiation reaction on orbits around a spinning black hole is analyzed. Such orbits possess three constants of motion: i , e , and a , which correspond, in the Newtonian limit of the orbit being an ellipse, to the inclination angle of the orbital plane to the hole’s equatorial plane, the eccentricity, and the semimajor axis length, respectively. First, it is argued th...
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It is demonstrated that, in the adiabatic approximation, nonequatorial circular orbits of particles in the Kerr metric ~i.e., orbits of constant Boyer-Lindquist radius! remain circular under the influence of gravitational radiation reaction. A brief discussion is given of conditions for breakdown of adiabaticity and of whether slightly noncircular orbits are stable against the growth of eccentr...
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Article history: Received 29 August 2017 Accepted 17 September 2017 Available online 25 September 2017 Editor: M. Trodden We calculate the absorption cross section for planar waves incident upon Kerr black holes, and present a unified picture for scalar, electromagnetic and gravitational waves. We highlight the spin-helicity effect that arises from a coupling between the rotation of the black h...
متن کاملGravitational shock waves for Schwarzschild and Kerr black holes.
The metrics of gravitational shock waves for a Schwarzschild black hole in ordinary coordinates and for a Kerr black hole in BoyerLindquist coordinates are derived. The Kerr metric is discussed for two cases: the case of a Kerr black hole moving parallel to the rotational axis, and moving perpendicular to the rotational axis. Then, two properties from the derived metrics are investigated: the s...
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ژورنال
عنوان ژورنال: Physical Review D
سال: 2008
ISSN: 1550-7998,1550-2368
DOI: 10.1103/physrevd.78.109902