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.
Numerical viscosity in hydrodynamics simulations in general relativity
1 Pith paper cite this work. Polarity classification is still indexing.
1
Pith paper citing it
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.
fields
gr-qc 1years
2026 1verdicts
UNVERDICTED 1representative citing papers
citing papers explorer
-
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.