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
Geodesic motion around a supersymmetric $$\hbox {AdS}_5$$AdS5 black hole
TL;DR: In this article, the geodesic motion of test particles in the spacetime of a supersymmetric AdS 5$ black hole is studied and the equations of motion are derived and solved in terms of the Weierstrass $$\wp $$, $$\sigma $$, and $$\zeta $$ functions.
Motion of the charged test particles in Kerr-Newman-Taub-NUT spacetime and analytical solutions
TL;DR: In this paper, the motion of charged test particles in Kerr-Newman-Taub-NUT spacetime was studied and the angular and radial parts of the orbit equations were analyzed.
Particle Dynamics Around the Black String.
TL;DR: In this paper, the escape velocity of neutral and charged particles around a five-dimensional static black string was derived and the analytical solutions of the equations of motion were discussed and some possible orbits for particles in the space-time were plotted.
Elementary Development of the Gravitational Self-Force
Steven Detweiler
- 31 Aug 2009
TL;DR: In this paper, the motion of a small mass m moving through curved spacetime, with metric g ab, is naturally and easily decomposed into two parts each of which satisfies the perturbed Einstein equations through O(m), one part is an inhomogeneous field h ab S which, near the particle, looks like the Coulomb m ∕ r field with tidal distortion from the local Riemann tensor.
Analytical solution of the geodesic equation in Kerr-(anti) de Sitter space-times
TL;DR: In this article, the complete analytical solutions of the geodesic equations in Kerr-de Sitter and Kerr-anti de Sitter space-times are presented in terms of Weierstrass elliptic and hyperelliptic Kleinian functions restricted to the one-dimensional $\ensuremath{\theta}$ divisor.
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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