TY - JOUR

T1 - Self-force effects on the marginally bound zoom-whirl orbit in Schwarzschild spacetime

AU - Barack, Leor

AU - Colleoni, Marta

AU - Damour, Thibault

AU - Isoyama, Soichiro

AU - Sago, Norichika

N1 - Publisher Copyright:
© 2019 American Physical Society.
Copyright:
Copyright 2019 Elsevier B.V., All rights reserved.

PY - 2019/12/6

Y1 - 2019/12/6

N2 - For a Schwarzchild black hole of mass M, we consider a test particle falling from rest at infinity and becoming trapped, at late time, on the unstable circular orbit of radius r=4GM/c2. When the particle is endowed with a small mass, μ M, it experiences an effective gravitational self-force, whose conservative piece shifts the critical value of the angular momentum and the frequency of the asymptotic circular orbit away from their geodesic values. By directly integrating the self-force along the orbit (ignoring radiative dissipation), we numerically calculate these shifts to O(μ/M). Our numerical values are found to be in agreement with estimates first made within the effective one-body formalism and with predictions of the first law of black-hole-binary mechanics (as applied to the asymptotic circular orbit). Our calculation is based on a time-domain integration of the Lorenz-gauge perturbation equations, and it is a first such calculation for an unbound orbit. We tackle several technical difficulties specific to unbound orbits, illustrating how these may be handled in more general cases of unbound motion. Our method paves the way to calculations of the self-force along hyperbolic-type scattering orbits. Such orbits can probe the two-body potential down to the "light ring" and could thus supply strong-field calibration data for eccentricity-dependent terms in the effective one-body model of merging binaries.

AB - For a Schwarzchild black hole of mass M, we consider a test particle falling from rest at infinity and becoming trapped, at late time, on the unstable circular orbit of radius r=4GM/c2. When the particle is endowed with a small mass, μ M, it experiences an effective gravitational self-force, whose conservative piece shifts the critical value of the angular momentum and the frequency of the asymptotic circular orbit away from their geodesic values. By directly integrating the self-force along the orbit (ignoring radiative dissipation), we numerically calculate these shifts to O(μ/M). Our numerical values are found to be in agreement with estimates first made within the effective one-body formalism and with predictions of the first law of black-hole-binary mechanics (as applied to the asymptotic circular orbit). Our calculation is based on a time-domain integration of the Lorenz-gauge perturbation equations, and it is a first such calculation for an unbound orbit. We tackle several technical difficulties specific to unbound orbits, illustrating how these may be handled in more general cases of unbound motion. Our method paves the way to calculations of the self-force along hyperbolic-type scattering orbits. Such orbits can probe the two-body potential down to the "light ring" and could thus supply strong-field calibration data for eccentricity-dependent terms in the effective one-body model of merging binaries.

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U2 - 10.1103/PhysRevD.100.124015

DO - 10.1103/PhysRevD.100.124015

M3 - Article

AN - SCOPUS:85076820206

VL - 100

JO - Physical Review D

JF - Physical Review D

SN - 2470-0010

IS - 12

M1 - 124015

ER -