Perturbative approach to an orbital evolution around a supermassive black hole
TL;DR: In this paper, the authors assume that the deviation is small and show that the half-advanced minus half-retarded field surprisingly provides the correct radiation reaction force, in a time-averaged sense, and determines the orbit of the particle.
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Abstract: A charge-free, point particle of infinitesimal mass orbiting a Kerr black hole is known to move along a geodesic. When the particle has a finite mass or charge, it emits radiation which carries away orbital energy and angular momentum, and the orbit deviates from a geodesic. In this paper we assume that the deviation is small and show that the half-advanced minus half-retarded field surprisingly provides the correct radiation reaction force, in a time-averaged sense, and determines the orbit of the particle.
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Citations
The Overlap of Numerical Relativity, Perturbation Theory and Post-Newtonian Theory in the Binary Black Hole Problem
TL;DR: In this article, a comparison of various analytical and numerical methods for the orbital motion and gravitational-wave emission of binary black hole systems is presented, emphasizing the use of coordinate-invariant relationships to perform meaningful comparisons.
4
Lindblad resonance torques in relativistic discs: II. Computation of resonance strengths
TL;DR: In this article, a fully relativistic computation of the torques due to Lindblad resonances from perturbers on circular, equatorial orbits on discs around Schwarzschild and Kerr black holes is presented.
4
Kerr Geodesics in Terms of Weierstrass Elliptic Functions
Eva Hackmann,Patryk Mach +1 more
- 12 May 2023
TL;DR: In this paper , the authors derive analytical solutions for timelike and null geodesics in the Kerr spacetime, where the solutions are parameterized explicitly by constants of motion, such as energy, angular momentum, and the Carter constant.
Rotating dyonic black hole in $N = 2, U(1)^2$ gauged supergravity as natural laboratory for high energy particle collisions
TL;DR: In this paper, the influence of the rotation parameter (a) and the gauge coupling constant (g) on the behavior of the horizon and ergoregion of the BH is investigated.
4
The equatorial motion of the charged test particles in Kerr-Newman-Taub-NUT spacetime
TL;DR: In this article, a detailed analysis of the equatorial motion of the charged test particles in Kerr-Newman-Taub-NUT spacetime was performed, by working out the orbit equation in the radial direction.
4
References
Radiation damping in a gravitational field
Bryce S. DeWitt,Robert W. Brehme +1 more
TL;DR: In this paper, the validity of equivalence is examined from the point of view of a charged mass point moving in an externally given gravitational field, and a covariant generalization of Dirac's work on the classical radiating electron is presented.
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Axiomatic approach to electromagnetic and gravitational radiation reaction of particles in curved spacetime
Theodore C. Quinn,Robert M. Wald +1 more
TL;DR: In this paper, the authors derive an expression for the electromagnetic self-force which agrees with that of DeWitt and Brehme as corrected by Hobbs, and show that the deviation from geodesic motion arises entirely from a tail term, in agreement with recent results of Mino et al.
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Calculating the gravitational self-force in Schwarzschild spacetime.
TL;DR: Here the values of all the "regularization parameters" required for implementing this regularization procedure, for any geodesic orbit in Schwarzschild spacetime, are given.
Approximating the inspiral of test bodies into Kerr black holes
TL;DR: In this paper, a new approximate method for constructing gravitational radiation driven inspirals of test bodies orbiting Kerr black holes is presented, which can be used for constructing approximate waveforms that can be applied to study data analysis problems for the future Laser Interferometer Space Antenna gravitational-wave observatory.
Black Hole Perturbation
TL;DR: In this paper, the energy flux and angular momentum flux formulas for a particle orbiting a black hole were derived using the Teukolsky formalism for dealing with the gravitational perturbation of the particle, and a systematic method to calculate higher order post-Newtonian corrections to the gravitational waves emitted by an orbiting particle.
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