How to Identify a Strange Star
- 19 October 1998
- journal article
- research article
- Published by American Physical Society (APS) in Physical Review Letters
- Vol. 81 (16) , 3311-3314
- https://doi.org/10.1103/physrevlett.81.3311
Abstract
Contrary to young neutron stars, young strange stars are not subject to the -mode instability which slows rapidly rotating, hot neutron stars to rotation periods near 10 ms via gravitational wave emission. Young millisecond pulsars are therefore likely to be strange stars rather than neutron stars, or at least to contain significant quantities of quark matter in the interior.
Keywords
All Related Versions
This publication has 18 references indexed in Scilit:
- A New Class of Unstable Modes of Rotating Relativistic StarsThe Astrophysical Journal, 1998
- Axial Instability of Rotating Relativistic StarsThe Astrophysical Journal, 1998
- Gravitational Radiation Instability in Hot Young Neutron StarsPhysical Review Letters, 1998
- Transport and relaxation in degenerate quark plasmasPhysical Review D, 1993
- Rate of the weak reactionin quark matterPhysical Review D, 1993
- The weak conversion rate in quark matterPhysica Scripta, 1992
- Bulk viscosity of strange quark matter, damping of quark star vibration, and the maximum rotation rate of pulsarsPhysical Review D, 1992
- Strange Quark Decay Rates in Quark Matter at High TemperaturesPhysica Scripta, 1986
- Strange starsThe Astrophysical Journal, 1986
- Cosmic separation of phasesPhysical Review D, 1984