Damping of vibrations and of the secular instability in quark stars

Details Damping of vibrations and of the secular instability in quark stars Damping of vibrations and of the secular instability in quark stars

Dec 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989phlb..233..412s&link_type=abstract

Physics Letters B, Volume 233, Issue 3-4, p. 412-416.

Physics

56

Scientific paper

We calculate the bulk viscosity of hot quark matter, or ``strange'' matter, which could be present in neutron stars. In the temperature range characteristic of young neutron stars, the bulk viscosity arising from non-leptonic strangeness-changing quark-quark interactions is orders of magnitude larger than that which has been calculated for ordinary nuclear matter. The gravitational wave secular instability should be completely suppressed for quark stars, and the damping times for pulsations will be very short.
The author has benefited from conversations with Josh Frieman, Jorge Horvath, and Angela Olinto.

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