Effect of hyperon bulk viscosity on neutron-star r-modes

Lee Lindblom, Benjamin J. Owen

Research output: Contribution to journalArticle

132 Scopus citations

Abstract

Neutron stars are expected to contain a significant number of hyperons in addition to protons and neutrons in the highest density portions of their cores. Following the work of Jones, we calculate the coefficient of bulk viscosity due to nonleptonic weak interactions involving hyperons in neutron-star cores, including new relativistic and superfluid effects. We evaluate the influence of this new bulk viscosity on the gravitational radiation driven instability in the r-modes. We find that the instability is completely suppressed in stars with cores cooler than a few times 109 K, but that stars rotating more rapidly than 10-30% of maximum are unstable for temperatures around 1010 K. Since neutron-star cores are expected to cool to a few times 109 K within seconds (much shorter than the r-mode instability growth time) due to direct Urca processes, we conclude that the gravitational radiation instability will be suppressed in young neutron stars before it can significantly change the angular momentum of the star.

Original languageEnglish
Article number063006
Pages (from-to)630061-6300615
Number of pages5670555
JournalPhysical Review D
Volume65
Issue number6
StatePublished - Mar 15 2002

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