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.
Viscous Dis- sipation and Heat Conduction in Binary Neutron- Star Mergers
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abstract
Inferring the properties of dense matter is one of the most exciting prospects from the measurement of gravitational waves from neutron star mergers. However, it will require reliable numerical simulations that incorporate viscous dissipation and energy transport if these can play a significant role within the survival time of the post-merger object. We calculate timescales for typical forms of dissipation and find that thermal transport and shear viscosity will not be important unless neutrino trapping occurs, which requires temperatures above about 10 MeV and gradients over lengthscales of 0.1 km or less. On the other hand, if direct-Urca processes remain suppressed, leaving modified-Urca processes to establish flavor equilibrium, then bulk viscous dissipation could provide significant damping to density oscillations observed right after the merger. When comparing with data from a state-of-the-art merger simulation we find that the bulk viscosity takes values close to its resonant maximum in a typical neutron-star merger, motivating a more careful assessment of the role of bulk viscous dissipation in the gravitational-wave signal from merging neutron stars.
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Viscous neutron stars have new families of axial oscillation modes without perfect-fluid counterparts, featuring mode avoidance and long-lived modes.
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.
The paper evaluates how triangular versus two-L-shaped geometries, arm lengths, and presence of low-frequency instruments affect the science reach of the Einstein Telescope for compact binaries, multi-messenger events, and stochastic backgrounds.
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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Axial Oscillations of Viscous Neutron Stars
Viscous neutron stars have new families of axial oscillation modes without perfect-fluid counterparts, featuring mode avoidance and long-lived modes.
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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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Science with the Einstein Telescope: a comparison of different designs
The paper evaluates how triangular versus two-L-shaped geometries, arm lengths, and presence of low-frequency instruments affect the science reach of the Einstein Telescope for compact binaries, multi-messenger events, and stochastic backgrounds.