The University of Southampton
University of Southampton Institutional Repository

r-Mode runaway and rapidly rotating neutron stars

r-Mode runaway and rapidly rotating neutron stars
r-Mode runaway and rapidly rotating neutron stars
We present a simple spin-evolution model that predicts that rapidly rotating accreting neutron stars will be confined mainly to a narrow range of spin frequencies: P = 1.5–5 ms. This is in agreement with current observations of neutron stars in both the low-mass X-ray binaries and the millisecond radio pulsars. The main ingredients in the model are (1) the instability of r-modes above a critical spin rate, (2) the thermal runaway that is due to the heat released as viscous damping mechanisms counteract the r-mode growth, and (3) a revised estimate of the strength of the dissipation that is due to the presence of a viscous boundary layer at the base of the crust in an old and relatively cold neutron star. We discuss the gravitational waves that are radiated during the brief r-mode–driven spin-down phase. We also briefly touch on how the new estimates affect the predicted initial spin periods of hot young neutron stars.
dense matter—gravitation—stars, neutron—stars, oscillations—stars, rotation
0004-637X
L75-L78
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Jones, David Ian
28367a56-e68b-4f44-a08a-65d46db2da93
Kokkotas, Kostas D.
0b8bb98a-a65f-434b-855b-ec5b488b4a96
Stergioulas, Nikolaos
7ff499f3-91e1-497f-bee6-4d8b5ca581da
Andersson, Nils
2dd6d1ee-cefd-478a-b1ac-e6feedafe304
Jones, David Ian
28367a56-e68b-4f44-a08a-65d46db2da93
Kokkotas, Kostas D.
0b8bb98a-a65f-434b-855b-ec5b488b4a96
Stergioulas, Nikolaos
7ff499f3-91e1-497f-bee6-4d8b5ca581da

Andersson, Nils, Jones, David Ian, Kokkotas, Kostas D. and Stergioulas, Nikolaos (2000) r-Mode runaway and rapidly rotating neutron stars. The Astrophysical Journal, 534, L75-L78.

Record type: Article

Abstract

We present a simple spin-evolution model that predicts that rapidly rotating accreting neutron stars will be confined mainly to a narrow range of spin frequencies: P = 1.5–5 ms. This is in agreement with current observations of neutron stars in both the low-mass X-ray binaries and the millisecond radio pulsars. The main ingredients in the model are (1) the instability of r-modes above a critical spin rate, (2) the thermal runaway that is due to the heat released as viscous damping mechanisms counteract the r-mode growth, and (3) a revised estimate of the strength of the dissipation that is due to the presence of a viscous boundary layer at the base of the crust in an old and relatively cold neutron star. We discuss the gravitational waves that are radiated during the brief r-mode–driven spin-down phase. We also briefly touch on how the new estimates affect the predicted initial spin periods of hot young neutron stars.

Full text not available from this repository.

More information

Published date: 2000
Keywords: dense matter—gravitation—stars, neutron—stars, oscillations—stars, rotation

Identifiers

Local EPrints ID: 29433
URI: https://eprints.soton.ac.uk/id/eprint/29433
ISSN: 0004-637X
PURE UUID: 1442ee9d-9858-49ca-9fc8-d059591b066a

Catalogue record

Date deposited: 06 Feb 2007
Last modified: 17 Jul 2017 15:58

Export record

Download statistics

Downloads from ePrints over the past year. Other digital versions may also be available to download e.g. from the publisher's website.

View more statistics

Atom RSS 1.0 RSS 2.0

Contact ePrints Soton: eprints@soton.ac.uk

ePrints Soton supports OAI 2.0 with a base URL of https://eprints.soton.ac.uk/cgi/oai2

This repository has been built using EPrints software, developed at the University of Southampton, but available to everyone to use.

We use cookies to ensure that we give you the best experience on our website. If you continue without changing your settings, we will assume that you are happy to receive cookies on the University of Southampton website.

×