R-mode runaway and rapidly rotating neutron stars

Details R-mode runaway and rapidly rotating neutron stars R-mode runaway and rapidly rotating neutron stars

2000-02-04

arxiv.org/abs/astro-ph/0002114v2

Astrophys.J. 534 (2000) L75

Astronomy and Astrophysics

Astrophysics

5 pages incl. 2 figures, minor changes, accepted for publication in ApJ Letters

Scientific paper

10.1086/312643

We present a simple spin evolution model that predicts that rapidly rotating accreting neutron stars will mainly be confined to a narrow range of spin-frequencies; P= 1.5-5 ms. This is in agreement with current observations of both neutron stars in the Low-Mass X-ray Binaries and millisecond radiopulsars. The main ingredients in the model are; i) the instability of r-modes above a critical spin rate, ii) thermal runaway due to heat released as viscous damping mechanisms counteract the r-mode growth, and iii) a revised estimate of the strength of dissipation 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 affects the predicted initial spin periods of hot young neutron stars.

Affiliated with

Also associated with

No associations

Rating

R-mode runaway and rapidly rotating neutron stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with R-mode runaway and rapidly rotating neutron stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and R-mode runaway and rapidly rotating neutron stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-232817