The R-mode instability window of the hybrid stars

Details The R-mode instability window of the hybrid stars The R-mode instability window of the hybrid stars

Aug 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004acasn..45..272p&link_type=abstract

Acta Astronomica Sinica, vol. 45, no. 3, p. 272-278

Astronomy and Astrophysics

Astronomy

Dense Matter, Gravitation, Stars: Oscillations, Stars: Rotation

Scientific paper

The hybrid star contains both a strange quark matter core and a solid crust of the neutron star. Considering this kind of particular structure, we utilize the fully self-consistent second-order correction technique to estimate the bulk viscosity damping timescale of the hybrid star at low temperature (T<109K), as well as the critical spin frequency which bases on the timescale. Compared with the neutron star and the strange star, we find that its minimum frequency rises to 704.42Hz(that is 1.42ms pulsar period),which can explain the observed data better.

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