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.
Bulk viscosity in superfluid neutron star cores. I. Direct Urca processes in npe\mu matter
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abstract
The bulk viscosity of the neutron star matter due to the direct Urca processes involving nucleons, electrons and muons is studied taking into account possible superfluidity of nucleons in the neutron star cores. The cases of singlet-state pairing or triplet-state pairing (without and with nodes of the superfluid gap at the Fermi surface) of nucleons are considered. It is shown that the superfluidity may strongly reduce the bulk viscosity. The practical expressions for the superfluid reduction factors are obtained. For illustration, the bulk viscosity is calculated for two models of dense matter composed of neutrons, protons,electrons and muons. The presence of muons affects the bulk viscosity due to the direct Urca reactions involving electrons and produces additional comparable contribution due to the direct Urca reactions involving muons. The results can be useful for studying damping of vibrations of neutron stars with superfluid cores.
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Steep matter-density gradients in neutron stars can produce neutrino-antineutrino pairs analogous to the Schwinger effect.
The routine model with bulk viscosity best reproduces the Crab pulsar's magnetic inclination angle, spin period, and derivative, while electromagnetic torque and accretion suppress inclination growth and most other effects are negligible.
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Bulk viscosity from neutron decays to dark baryons in neutron star matter
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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Gradient-Produced Neutrinos
Steep matter-density gradients in neutron stars can produce neutrino-antineutrino pairs analogous to the Schwinger effect.
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The routine model with bulk viscosity best reproduces the Crab pulsar's magnetic inclination angle, spin period, and derivative, while electromagnetic torque and accretion suppress inclination growth and most other effects are negligible.