English

# Item

ITEM ACTIONSEXPORT
Lorenz gauge gravitational self-force calculations of eccentric binaries using a frequency domain procedure

Osburn, T., Forseth, E., Evans, C., & Hopper, S. (2014). Lorenz gauge gravitational self-force calculations of eccentric binaries using a frequency domain procedure. Physical Review D, 90: 104031. doi:10.1103/PhysRevD.90.104031.

Item is

### Basic

show hide
Genre: Journal Article

### Files

show Files
hide Files
:
1409.4419.pdf (Preprint), 899KB
Name:
1409.4419.pdf
Description:
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
-
-
:
PRD90_104031.pdf (Any fulltext), 775KB
Name:
PRD90_104031.pdf
Description:
-
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
-
-
-

show

### Creators

show
hide
Creators:
Osburn, Thomas, Author
Forseth, Erik, Author
Evans, Charles, Author
Hopper, Seth1, Author
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013

### Content

show
hide
Free keywords: General Relativity and Quantum Cosmology, gr-qc
Abstract: We present an algorithm for calculating the metric perturbations and gravitational self-force for extreme-mass-ratio inspirals (EMRIs) with eccentric orbits. The massive black hole is taken to be Schwarzschild and metric perturbations are computed in Lorenz gauge. The perturbation equations are solved as coupled systems of ordinary differential equations in the frequency domain. Accurate local behavior of the metric is attained through use of the method of extended homogeneous solutions and mode-sum regularization is used to find the self-force. We focus on calculating the self-force with sufficient accuracy to ensure its error contributions to the phase in a long term orbital evolution will be $\delta\Phi \lesssim 10^{-2}$ radians. This requires the orbit-averaged force to have fractional errors $\lesssim 10^{-8}$ and the oscillatory part of the self-force to have errors $\lesssim 10^{-3}$ (a level frequently easily exceeded). Our code meets this error requirement in the oscillatory part, extending the reach to EMRIs with eccentricities of $e \lesssim 0.8$, if augmented by use of fluxes for the orbit-averaged force, or to eccentricities of $e \lesssim 0.5$ when used as a stand-alone code. Further, we demonstrate accurate calculations up to orbital separations of $a \simeq 100 M$, beyond that required for EMRI models and useful for comparison with post-Newtonian theory. Our principal developments include (1) use of fully constrained field equations, (2) discovery of analytic solutions for even-parity static modes, (3) finding a pre-conditioning technique for outer homogeneous solutions, (4) adaptive use of quad-precision and (5) jump conditions to handle near-static modes, and (6) a hybrid scheme for high eccentricities.

### Details

show
hide
Language(s):
Dates: 2014-09-152014-12-112014
Publication Status: Published in print
Pages: Updated to more closely reflect published version
Publishing info: -
Rev. Method: -
Identifiers: arXiv: 1409.4419
DOI: 10.1103/PhysRevD.90.104031
URI: http://arxiv.org/abs/1409.4419
Degree: -

show

show

show

### Source 1

show
hide
Title: Physical Review D
Other : Phys. Rev. D.
Source Genre: Journal
Creator(s):
Affiliations:
Publ. Info: Lancaster, Pa. : American Physical Society
Pages: - Volume / Issue: 90 Sequence Number: 104031 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: /journals/resource/111088197762258