Phys. Rev. Lett. 81, 3311–3314 (1998)How to Identify a Strange StarReceived 2 June 1998; published in the issue dated 19 October 1998 Contrary to young neutron stars, young strange stars are not subject to the r-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. © 1998 The American Physical Society URL:
http://link.aps.org/doi/10.1103/PhysRevLett.81.3311
DOI:
10.1103/PhysRevLett.81.3311
PACS:
97.60.Jd, 04.40.Dg, 12.38.Mh, 97.60.Gb
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