Transition from inspiral to plunge for a compact body in a circular equatorial orbit around a massive, spinning black hole

By A. Ori, K. R. D. O. Physics, T. I. O. Technology, Theoretical Astophysics, C. I. O. Technology.. 2000

133 citations recorded by the source corpus.

There are three regimes of gravitational-radiation-reaction-induced inspiral for a compact body with mass μ, in a circular, equatorial orbit around a Kerr black hole with mass M≫μ: (i) the adiabatic inspiral regime, in which the body gradually descends through a sequence of circular, geodesic orbits; (ii) a transition regime, near the innermost stable circular orbit (isco); (iii) the plunge regime, in which the body travels on a geodesic from slightly below the isco into the hole’s horizon. This paper gives an analytic treatment of the transition regime and shows that, with some luck, gravitational waves from the transition might be measurable by the space-based LISA mission.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/64cc3d7fc8ab24c888224e83fbe47bae1752b232

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. E. Barausse
2. Fabian Hofmann
3. Luciano Rezzolla
4. T. Damour
5. A. Pound
6. B. Wardell
7. A. Buonanno
8. E. Poisson

In Nuclear and High Energy Physics

1. T. Damour
2. B. Wardell
3. A. Pound
4. M. Miller
5. A. Buonanno
6. E. Barausse
7. Luciano Rezzolla
8. E. Colbert

Citations in the corpus

• The Motion of Point Particles in Curved Spacetime (2004, background): “Barack and Sago compare this shift to the ambiguity created by the dissipative piece of the self-force, which was previously investigated by Ori and Thorne [135] and Sundararajan [167]; they find that the conservative shift is very small compared with the dissipative ambiguity.”
• Transition from inspiral to plunge in binary black hole coalescences (2000, background): “The idea here is that numerical relativity will probably not be able, before quite a few years, to accurately evolve binary systems over many (or even ∼ 10) orbits.”
• Intermediate - mass black holes (2003, background): “For a spinning (Kerr) black hole, the last stable circular orbit, and thus the standard inner disk radius, ranges from 0.5 to 4.5 Rs, depending on the black hole spin and the sense of disk rotation (prograde or retrograde, e.g. Ori & Thorne 2000).”
• Black hole perturbation theory and gravitational self-force (2021, background): “In the context of a binary, the small corrections εz(1)(q, p i q) to the trajectory remain uniformly small over the entire inspiral until the transition to plunge [135]; because they are periodic functions of q, they have no large secular terms.”
• THE FINAL SPIN FROM BINARY BLACK HOLES IN QUASI-CIRCULAR ORBITS (2016, background): “Similarly, in the EMRL, the leading contributions to |`| come from the ISCO energy and angular momentum of a test particle in Kerr.”
• The Motion of Point Particles in Curved Spacetime (2003, background): “Barack and Sago compare this shift to the ambiguity created by the dissipative piece of the self-force, which was previously investigated by Ori and Thorne [135] and Sundararajan [167]; they find that the conservative shift is very small compared with the dissipative ambiguity.”
• Gravitational self-force in a Schwarzschild background and the effective one-body formalism (2009, background): “interactions on the location of the LSO it was first studied in [2] (for arbitrary ν ≤ 1/4) and shown there to lead to a “blurring” of the LSO frequency of fractional order ν2/5. [See also the work of [30], restricted to the small mass ratio case ν ≪ 1.] 2 Notation, choice of coordinate system, and p”