Post-Newtonian Expansion of Gravitational Waves from a Particle in Circular Orbits around a Rotating Black Hole: Effects of Black Hole Absorption

Tagoshi, Hideyuki; Mano, Shuhei; Takasugi, Eiichi

doi:10.1017/s0074180900132437

Cited by 5 publications

(8 citation statements)

References 6 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The tidal heating of black holes was recently investigated by Alvi [40], Poisson [9,39], Taylor and Poisson [6], and Comeau and Poisson [3], building on earlier work by Poisson and Sasaki [41] and Tagoshi, Mano, and Takasugi [42]. The notion of tidal work, tidal torque, and tidal heating was put on a firm relativistic footing by Purdue [43], Favata [44], and Booth and Creighton [45].…”

Section: Tidal Heatingmentioning

confidence: 99%

Geometry and dynamics of a tidally deformed black hole

2010

View full text Add to dashboard Cite

The metric of a nonrotating black hole deformed by a tidal interaction is calculated and expressed as an expansion in the strength of the tidal coupling. The expansion parameter is the inverse length scale R^{-1}, where R is the radius of curvature of the external spacetime in which the black hole moves. The expansion begins at order R^{-2}, and it is carried out through order R^{-4}. The metric is parameterized by a number of tidal multipole moments, which specify the black hole's tidal environment. The tidal moments are freely-specifiable functions of time that are related to the Weyl tensor of the external spacetime. The metric is presented in a light-cone coordinate system that possesses a clear geometrical meaning: The advanced-time coordinate $v$ is constant on past light cones that converge toward the black hole; the angles theta and phi are constant on the null generators of each light cone; and the radial coordinate r is an affine parameter on each generator, which decreases as the light cones converge toward the black hole. The coordinates are well-behaved on the black-hole horizon, and they are adjusted so that the coordinate description of the horizon is the same as in the Schwarzschild geometry: r = 2M. At the order of accuracy maintained in this work, the horizon is a stationary null hypersurface foliated by apparent horizons; it is an isolated horizon in the sense of Ashtekar and Krishnan. As an application of our results we examine the induced geometry and dynamics of the horizon, and calculate the rate at which the black-hole surface area increases as a result of the tidal interaction.Comment: 43 pages, 2 figure

show abstract

Section: Tidal Heatingmentioning

confidence: 99%

Geometry and dynamics of a tidally deformed black hole

2010

View full text Add to dashboard Cite

show abstract

“…Actually, this is not completely true, as realistic black holes usually have non-zero spin, and the inclusion of spin tends to enhance finite size effects [25]. Also, absorption by the black hole horizon, which necessitates the introduction of additional worldline modes in the EFT [30] arises at order v 8 for non-spinning black holes [31] and at order v 5 [32] when the black hole has spin.…”

Section: )mentioning

confidence: 99%

Effective Field Theories and Gravitational Radiation

Goldberger

2007

Particle Physics and Cosmology: The Fabric of Spacetime

140

View full text Add to dashboard Cite

“…The black hole absorption in the case of a rotating black hole appears at 2.5PN order [ 46 ]. Using a new analytic method to solve the homogeneous Teukolsky equation found by Mano, Suzuki, and Takasugi [ 68 ], the black hole absorption in the Kerr case was calculated by Tagoshi, Mano, and Takasugi [ 98 ] to 6.5PN order beyond the quadrupole formula.…”

Section: Introductionmentioning

confidence: 99%

Analytic Black Hole Perturbation Approach to Gravitational Radiation

Sasaki

Tagoshi

2003

Living Rev. Relativ.

Self Cite

326

422

View full text Add to dashboard Cite

We review the analytic methods used to perform the post-Newtonian expansion of gravitational waves induced by a particle orbiting a massive, compact body, based on black hole perturbation theory. There exist two different methods of performing the post-Newtonian expansion. Both are based on the Teukolsky equation. In one method, the Teukolsky equation is transformed into a Regge-Wheeler type equation that reduces to the standard Klein Gordon equation in the flat-space limit, while in the other method (which was introduced by Mano, Suzuki, and Takasugi relatively recently, the Teukolsky equation is used directly in its original form. The former’s advantage is that it is intuitively easy to understand how various curved space effects come into play. However, it becomes increasingly complicated when one goes to higher and higher post-Newtonian orders. In contrast, the latter’s advantage is that a systematic calculation to higher post-Newtonian orders can be implemented relatively easily, but otherwise, it is so mathematical that it is hard to understand the interplay of higher order terms. In this paper, we review both methods so that their pros and cons may be seen clearly. We also review some results of calculations of gravitational radiation emitted by a particle orbiting a black hole.

show abstract

Post-Newtonian Expansion of Gravitational Waves from a Particle in Circular Orbits around a Rotating Black Hole: Effects of Black Hole Absorption

Cited by 5 publications

References 6 publications

Geometry and dynamics of a tidally deformed black hole

Geometry and dynamics of a tidally deformed black hole

Effective Field Theories and Gravitational Radiation

Analytic Black Hole Perturbation Approach to Gravitational Radiation

Contact Info

Product

Resources

About