Ushomirsky, Greg (2001) R-modes in accreting and young neutron stars. In: Astrophysical Sources for Ground-Based Gravitational Wave Detectors. AIP Conference Proceedings. No.575. American Institute of Physics , Melville, NY, pp. 284-295. ISBN 0-7354-0014-8 http://resolver.caltech.edu/CaltechAUTHORS:20111118-100300999
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Recent work has raised the exciting possibility that r-mode pulsations (Rossby waves) in rotating neutron star cores may be strong gravitational wave sources. Rapidly rotating young neutron stars born in supernovae enter the r-mode instability region within the first minutes of their lives and may spin down by substantial amounts due to gravitational radiation from r-modes. Accreting neutron stars in low-mass X-ray binaries (LMXBs) are spun up by accretion to such short rotation periods that they may be unstable to r-mode pulsations as well. Gravitational waves from these neutron stars are strong enough to be detectable by second-generation, "enhanced" gravitational wave interferometers. I review the recent progress in understanding the r-mode instability in young and accreting neutron stars, with the focus on the issues of the coupling of the pulsations to the crust and nonlinear saturation amplitudes.
|Item Type:||Book Section|
|Additional Information:||© 2001 American Institute of Physics. Issue Date: 22 June 2001.|
|Subject Keywords:||neutron stars; stellar pulsations; stellar evolution; stellar rotation; accretion; gravitational waves; astrophysical radiation mechanisms|
|Classification Code:||PACS: 97.60.Jd; 97.10.Sj; 95.30.Sf; 04.30.Db|
|Official Citation:||R-modes in accreting and young neutron stars Greg Ushomirsky, AIP Conf. Proc. 575, 284 (2001), DOI:10.1063/1.1387319|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||21 Nov 2011 00:11|
|Last Modified:||26 Dec 2012 14:25|
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