First neural-network subgrid model for special relativistic MHD reproduces 4x-higher-resolution magnetic field amplification in 3D Kelvin-Helmholtz tests at 44x speedup.
Neutron star evolution with the Bemfica-Disconzi-Noronha-Kovtun viscous hydrodynamics framework
5 Pith papers cite this work. Polarity classification is still indexing.
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abstract
The recently proposed first-order viscous relativistic hydrodynamics formulation by Bemfica, Disconzi, Noronha, and Kovtun (commonly known as the BDNK formulation) has been shown to be causal, stable, strongly hyperbolic, and thus locally well-posed. It is now a viable new option for modelling out-of-equilibrium effects in fluids, and has attracted wide attention in its potential applications to astrophysical systems. In this work, we present the first non-linear numerical simulation of spherically symmetric neutron stars using the BDNK formulation under the Cowling approximation. Using a simplified equation of state, we show that stable evolutions can be constructed within a restricted parameter space up to the simulation time we explored. From these simulations, we analyse the frequency content of the quasi-normal modes and the decay rate of the fundamental mode. This analysis serves as a first step towards constructing a fully consistent model of neutron stars using the BDNK formulation.
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A general framework for incorporating arbitrary nonequilibrium corrections into linear non-radial relativistic stellar perturbations without specifying constitutive relations.
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.
Causal viscous relativistic hydrodynamics applied to neutron stars yields new axial mode families without perfect-fluid counterparts, including mode avoidance and long-lived modes.
A finite-volume scheme for causal viscoresistive relativistic MHD is developed with an extra correction needed in the ultra-relativistic limit, plus a primitive recovery method validated on benchmarks and 2D simulations.
citing papers explorer
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Subgrid Modelling for Relativistic Magnetohydrodynamics with Machine Learning
First neural-network subgrid model for special relativistic MHD reproduces 4x-higher-resolution magnetic field amplification in 3D Kelvin-Helmholtz tests at 44x speedup.
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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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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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Finite-volume scheme for first-order viscoresistive relativistic magnetohydrodynamics
A finite-volume scheme for causal viscoresistive relativistic MHD is developed with an extra correction needed in the ultra-relativistic limit, plus a primitive recovery method validated on benchmarks and 2D simulations.