CaltechAUTHORS
  A Caltech Library Service

Gravitational waves from hot young rapidly rotating neutron stars

Owen, Benjamin and Lindblom, Lee and Cutler, Curt and Schutz, Bernard and Vecchio, Alberto and Andersson, Nils (1998) Gravitational waves from hot young rapidly rotating neutron stars. Physical Review D, 58 (8). Art. No. 84020. ISSN 1550-7998. http://resolver.caltech.edu/CaltechAUTHORS:20170408-143147342

[img] PDF - Published Version
See Usage Policy.

279Kb
[img] PDF - Submitted Version
See Usage Policy.

352Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20170408-143147342

Abstract

Gravitational radiation drives an instability in the r-modes of young rapidly rotating neutron stars. This instability is expected to carry away most of the angular momentum of the star by gravitational radiation emission, leaving a star rotating at about 100 Hz. In this paper we model in a simple way the development of the instability and evolution of the neutron star during the year-long spindown phase. This allows us to predict the general features of the resulting gravitational waveform. We show that a neutron star formed in the Virgo cluster could be detected by the LIGO and VIRGO gravitational wave detectors when they reach their “enhanced” level of sensitivity, with an amplitude signal-to-noise ratio that could be as large as about 8 if near-optimal data analysis techniques are developed. We also analyze the stochastic background of gravitational waves produced by the r-mode radiation from neutron-star formation throughout the universe. Assuming a substantial fraction of neutron stars are born with spin frequencies near their maximum values, this stochastic background is shown to have an energy density of about 10^(−9) of the cosmological closure density, in the range 20 Hz to 1 kHz. This radiation should be detectable by “advanced” LIGO as well.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1103/PhysRevD.58.084020DOIArticle
http://arxiv.org/abs/gr-qc/9804044arXivDiscussion Paper
Additional Information:© 1998 American Physical Society. (Received 20 April 1998; published 14 September 1998) We thank Patrick Brady, Jolien Creighton, Teviet Creighton, Scott Hughes, Sterl Phinney, Joseph Romano, and Kip Thorne for helpful discussions. This research was supported by NSF Grant No. AST-9417371 and Grant No. PHY-9796079, by the NSF, and by NASA Grant No. NAG5-4093.
Group:LIGO, TAPIR
Funders:
Funding AgencyGrant Number
NSFAST-9417371
NSFPHY-9796079
NASANAG5-4093
Classification Code:PACS numbers: 04.30.Db, 04.40.Dg, 97.60.Jd
Record Number:CaltechAUTHORS:20170408-143147342
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170408-143147342
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:75959
Collection:CaltechAUTHORS
Deposited By: 1Science Import
Deposited On:25 Apr 2017 21:20
Last Modified:25 Apr 2017 21:20

Repository Staff Only: item control page