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

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arxiv astro-ph/0110558 v3 pith:YUAUY5IV submitted 2001-10-25 astro-ph gr-qc

Lee Lindblom (Caltech) , Benjamin J. Owen (U Wisconsin Milwaukee) This is my paper
classification astro-phgr-qc
keywords coresinstabilitystarsbulkneutron-starviscosityexpectedgravitational
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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 10^9 K, but that stars rotating more rapidly than 10-30% of maximum are unstable for temperatures around 10^10 K. Since neutron-star cores are expected to cool to a few times 10^9 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.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Superradiant amplification by rotating viscous compact objects

    gr-qc 2025-06 conditional novelty 7.0 of 10

    Using causal BDNK hydrodynamics, the authors derive coupled gravitational-wave and viscous-mode equations for slowly rotating stars and find superradiant amplification at low frequencies.

  2. Bulk viscosity from neutron decays to dark baryons in neutron star matter

    astro-ph.HE 2025-09 conditional novelty 5.0 of 10

    Neutron dark decays modify the equation of state and either mildly suppress or strongly enhance bulk viscosity in neutron star merger conditions, depending on the in-medium decay rate.

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