Perturbative approach to an orbital evolution around a supermassive black hole

Abstract: Efforts are underway to accurately model extreme-mass-ratio inspirals for binaries with a spinning (Kerr) primary. At lowest order the adiabatic evolution depends on the radiation fluxes. Fluxes and other self-force quantities can be expanded analytically in post-Newtonian (PN) series allowing the early evolutionary phase to be understood. When it comes to more complicated background geodesic orbits, it proves useful to use the scalar field model problem to guide development and testing of techniques. In this paper, we present analytical expressions for the scalar fluxes from a scalar point charge in inclined-spherical orbit about a Kerr black hole up to 12PN relative order, with expressions that are exact in terms of the inclination parameter x and black hole spin a . The expressions are constructed using the Mano, Suzuki, and Takasugi method of solving the scalar wave equation in a Kerr background. We compare the numerical evaluation of these flux expressions to full numerical ( s = 0 ) eukolsky code results, examining their degree of utility as the strong-field region is approached.

TL;DR: Analytic solutions for spinning particle motion near black holes and exotic compact objects are derived in closed form, capturing the spin-curvature force.

TL;DR: In this article, the authors show that there is a region of the parameter space in which pairs of physically distinct geodesic orbits can have the same three frequencies, related to the radial, longitudinal, and (mean) azimuthal motions.

TL;DR: In this paper, the authors considered the timelike and null geodesics around the static (GMGHS, magnetically charged GMGHS), electrically charged and the rotating (Kerr-Sen dilaton-axion) dilaton black holes.

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.

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.

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.

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.