Neutrino cooling and spin-down of rapidly rotating compact stars
Abstract
The gravitational-wave instability of r-modes in rapidly rotating compact stars is believed to spin them down to angular frequencies of about a tenth of the Kepler frequency soon after their birth in a Supernova. We point out that the r-mode perturbation also impacts the neutrino cooling and viscosity in hot compact stars via processes that restore weak equilibrium. We illustrate this fact with a simple model of spin-down due to gravitational wave emission in compact stars composed entirely of three-flavor degenerate quark matter (a strange quark star). Non-equilibrium neutrino cooling of this oscillating fluid matter is quantified. Our results imply that a consistent treatment of thermal and spin-frequency evolution of a young and hot compact star is a requisite in estimating the persistence of gravitational waves from such a source.
Keywords
Cite
@article{arxiv.1008.4985,
title = {Neutrino cooling and spin-down of rapidly rotating compact stars},
author = {Prashanth Jaikumar and Stou Sandalski},
journal= {arXiv preprint arXiv:1008.4985},
year = {2010}
}
Comments
10 pages, 1 figure