The r-mode instability windows of hybrid stars

Details The r-mode instability windows of hybrid stars The r-mode instability windows of hybrid stars

Jan 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005cha%26a..29...53p&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 29, Issue 1, p. 53-60.

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Taking into account the peculiar properties of hybrid stars, stars containing both a core of strange quark matter and the solid crust of a neutron star, and employing a fully self-consistent second-order correction technique, we study the time scale of bulk viscosity dissipation at the low temperature limit (T < 109 K) and with this time scale we calculate the critical spin frequency of the hybrid star. It is found that its minimal value is 704.42 Hz (corresponding to a pulse period of 1.42 ms). When this is compared with the periods of neutron and strange stars, a better interpretation of the observational data is obtained.

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