Magnetic fields modify bulk viscous dissipation in post-merger neutron star matter by altering direct and modified Urca rates at finite temperature beyond the Fermi surface approximation.
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Monte Carlo simulation of post-merger remnant shows pair annihilation rates greatly increased in cold low-density regions and inelastic electron scattering important for heavy-lepton neutrino thermalization, processes not included in prior merger simulations.
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.
citing papers explorer
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Thermal and Magnetic effects on Bulk Viscosity in Binary Neutron Star Mergers
Magnetic fields modify bulk viscous dissipation in post-merger neutron star matter by altering direct and modified Urca rates at finite temperature beyond the Fermi surface approximation.
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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.