English
 
User Manual Privacy Policy Disclaimer Contact us
  Advanced SearchBrowse

Item

ITEM ACTIONSEXPORT
  Reducing orbital eccentricity of precessing black-hole binaries

Buonanno, A., Kidder, L. E., Mroué, A. H., Pfeiffer, H. P., & Taracchini, A. (2011). Reducing orbital eccentricity of precessing black-hole binaries. Physical Review D, 83(10): 104034. doi:10.1103/PhysRevD.83.104034.

Item is

Basic

show hide
Item Permalink: http://hdl.handle.net/11858/00-001M-0000-0023-F7C9-3 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-0024-2663-4
Genre: Journal Article

Files

show Files
hide Files
:
1012.1549.pdf (Preprint), 586KB
Name:
1012.1549.pdf
Description:
File downloaded from arXiv at 2014-10-21 11:26
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
:
PhysRevD.83.104034.pdf (Any fulltext), 825KB
Name:
PhysRevD.83.104034.pdf
Description:
-
Visibility:
Public
MIME-Type / Checksum:
application/pdf / [MD5]
Technical Metadata:
Copyright Date:
-
Copyright Info:
-
License:
-

Locators

show

Creators

show
hide
 Creators:
Buonanno, A.1, 2, Author              
Kidder, Lawrence E., Author
Mroué, Abdul H., Author
Pfeiffer, Harald P., Author
Taracchini, Andrea, Author
Affiliations:
1Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_1933290              
2University of Maryland, ou_persistent22              

Content

show
hide
Free keywords: General Relativity and Quantum Cosmology, gr-qc
 Abstract: Building initial conditions for generic binary black-hole evolutions without initial spurious eccentricity remains a challenge for numerical-relativity simulations. This problem can be overcome by applying an eccentricity-removal procedure which consists in evolving the binary for a couple of orbits, estimating the eccentricity, and then correcting the initial conditions. The presence of spins can complicate this procedure. As predicted by post-Newtonian theory, spin-spin interactions and precession prevent the binary from moving along an adiabatic sequence of spherical orbits, inducing oscillations in the radial separation and in the orbital frequency. However, spin-induced oscillations occur at approximately twice the orbital frequency, therefore they can be distinguished from the initial spurious eccentricity, which occurs at approximately the orbital frequency. We develop a new removal procedure based on the derivative of the orbital frequency and find that it is successful in reducing the eccentricity measured in the orbital frequency to less than 0.0001 when moderate spins are present. We test this new procedure using numerical-relativity simulations of binary black holes with mass ratios 1.5 and 3, spin magnitude 0.5 and various spin orientations. The numerical simulations exhibit spin-induced oscillations in the dynamics at approximately twice the orbital frequency. Oscillations of similar frequency are also visible in the gravitational-wave phase and frequency of the dominant mode.

Details

show
hide
Language(s):
 Dates: 2010-12-072011-05-312011
 Publication Status: Published in print
 Pages: 17 pages, 11 figures, fixed typos
 Publishing info: -
 Table of Contents: -
 Rev. Method: -
 Identifiers: arXiv: 1012.1549
DOI: 10.1103/PhysRevD.83.104034
URI: http://arxiv.org/abs/1012.1549
 Degree: -

Event

show

Legal Case

show

Project information

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: 83 (10) Sequence Number: 104034 Start / End Page: - Identifier: ISSN: 0556-2821
CoNE: https://pure.mpg.de/cone/journals/resource/111088197762258