Gravitational self force on a particle in circular orbit
around a Schwarzschild black hole

Gravitational self force on a particle in circular orbit
around a Schwarzschild black hole

We calculate the gravitational self force acting on a pointlike test particle of
mass ?, set in a circular geodesic orbit around a Schwarzschild black hole.
Our calculation is done in the Lorenz gauge: For given orbital radius,
we first solve directly for the Lorenz-gauge metric perturbation using numerical
evolution in the time domain; We then compute the (finite) back-reaction force
from each of the multipole modes of the perturbation; Finally, we apply
the ``mode sum'' method to obtain the total, physical self force.
The temporal component of the self force (which is gauge invariant) describes
the dissipation of orbital energy through gravitational radiation.
Our results for this component are consistent, to within the computational accuracy,
with the total flux of gravitational-wave energy radiated to infinity and through the
event horizon. The radial component of the self force
(which is gauge dependent) is calculated here for the first time. It describes
a conservative shift in the orbital parameters away from their geodesic values.
We thus obtain the O(?) correction to the energy and angular momentum parameters
(in the Lorenz gauge), as well as the O(?) shift in the orbital frequency
(which is gauge invariant).

064021-[25pp]

Barack, Leor

f08e66d4-c2f7-4f2f-91b8-f2c4230d0298

Sago, Norichika

50641559-f289-4ffa-810b-fe4ec8c26e26

March 2007

Barack, Leor

f08e66d4-c2f7-4f2f-91b8-f2c4230d0298

Sago, Norichika

50641559-f289-4ffa-810b-fe4ec8c26e26

Barack, Leor and Sago, Norichika
(2007)
Gravitational self force on a particle in circular orbit
around a Schwarzschild black hole.
*Physical Review D*, 75 (6), .
(doi:10.1103/PhysRevD.75.064021).

## Abstract

We calculate the gravitational self force acting on a pointlike test particle of
mass ?, set in a circular geodesic orbit around a Schwarzschild black hole.
Our calculation is done in the Lorenz gauge: For given orbital radius,
we first solve directly for the Lorenz-gauge metric perturbation using numerical
evolution in the time domain; We then compute the (finite) back-reaction force
from each of the multipole modes of the perturbation; Finally, we apply
the ``mode sum'' method to obtain the total, physical self force.
The temporal component of the self force (which is gauge invariant) describes
the dissipation of orbital energy through gravitational radiation.
Our results for this component are consistent, to within the computational accuracy,
with the total flux of gravitational-wave energy radiated to infinity and through the
event horizon. The radial component of the self force
(which is gauge dependent) is calculated here for the first time. It describes
a conservative shift in the orbital parameters away from their geodesic values.
We thus obtain the O(?) correction to the energy and angular momentum parameters
(in the Lorenz gauge), as well as the O(?) shift in the orbital frequency
(which is gauge invariant).

Full text not available from this repository.

## More information

Submitted date: 15 January 2007

Published date: March 2007

## Identifiers

Local EPrints ID: 43216

URI: https://eprints.soton.ac.uk/id/eprint/43216

ISSN: 1550-7998

PURE UUID: 7a1b1c70-bbcf-4a0c-b2bc-3299a8ae49ff

## Catalogue record

Date deposited: 17 Jan 2007

Last modified: 13 Mar 2019 21:10

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## Contributors

Author:
Norichika Sago

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