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Numerical modelling of bulk viscosity in neutron stars
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Numerical modelling of bulk viscosity in neutron stars
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The early post-merger phase of a binary neutron-star coalescence is shaped by characteristic rotational velocities as well as violent density oscillations and offers the possibility to constrain the properties of neutron star matter by observing the gravitational wave emission. One possibility to do so is the investigation of gravitational wave damping through the bulk viscosity which originates from violations of weak chemical equilibrium. Motivated by these prospects, we present a comprehensive report about the implementation of the self-consistent and second-order formulation of the equations of relativistic hydrodynamics for dissipative fluids proposed by M\"uller, Israel and Stewart. Furthermore, we report on the results of two test problems, namely the viscous damping of linear density oscillations of isolated nonrotating neutron stars and the viscous migration test, both of which confirm our implementation and can be used for future code tests. Finally, we present fully general-relativistic simulations of viscous binary neutron-star mergers. We explore the structural and thermal properties of binary neutron-star mergers with a constant bulk-viscosity prescription and investigate the impact of bulk viscosity on dynamical mass ejection. We find that inverse Reynolds numbers $\sim 1\%$ can be achieved for the highest employed viscosity thereby suppressing the dynamically ejected mass by a factor of $\sim 5$ compared to the inviscid case.
Forward citations
Cited by 7 Pith papers
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Out-of-Equilibrium Effects in Non-Radial Relativistic Stellar Perturbations: A Model-Agnostic Formulation and Mode Analysis
A general framework for incorporating arbitrary nonequilibrium corrections into linear non-radial relativistic stellar perturbations without specifying constitutive relations.
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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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Dynamical response of twin stars to perturbations
Twin-star configurations on the hadronic branch are dynamically favored over hybrid twins because they tolerate stronger perturbations before migrating, with binding energies serving as a proxy for this preference.
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Radial Oscillations of Viscous Stars at Finite Temperature
Heat diffusion introduces a distinct thermal mode sector in viscous star oscillations that transitions to propagating behavior above a critical overtone, realizing finite-size relativistic second sound.
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Axial Oscillations of Viscous Neutron Stars
Causal viscous relativistic hydrodynamics applied to neutron stars yields new axial mode families without perfect-fluid counterparts, including mode avoidance and long-lived modes.
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Radial Oscillations of Viscous Stars
Viscosity damps neutron-star radial modes on ms timescales, shifts frequencies by up to ~1% at ζ∼10^30 g/cm/s, produces overdamped modes above ∼10^31, and cannot stabilize unstable stars in Eckart or BDNK theory.
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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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