Numerical viscosity in hydrodynamics simulations in general relativity

Abstract

We present an alternative method to estimate the numerical viscosity in simulations of astrophysical objects, which is based in the damping of fluid oscillations. We apply the method to general relativistic hydrodynamic simulations using a spherical coordinates. We perform 1D-spherical and 2D- axisymmetric simulations of radial oscillations in spherical systems. We calibrate first the method with simulations with added bulk viscosity and study the differences between different numerical schemes. We apply the method to radial oscillations of neutron stars and we conclude that the main source of numerical viscosity in this case is the surface of the star. We expect that this method could be useful to compute the resolution requirements and limitations of the numerical simulations in different astrophysical scenarios in the future.

Accepted for publication in Class. Quantum Grav. 15 pages, 3 figures

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• Coherent magneto-elastic oscillations in superfluid magnetars
• Numerical modelling of bulk viscosity in neutron stars
• A hybrid approach to long-term binary neutron-star simulations
• Neutron star evolution with the Bemfica-Disconzi-Noronha-Kovtun viscous hydrodynamics framework
• Gauge-invariant perturbations of relativistic non-perfect fluids in spherical spacetime
• Projecting the likely importance of weak-interaction-driven bulk viscosity in neutron star mergers