General relativistic smoothed particle hydrodynamics

Abstract

We present a method for general relativistic smoothed particle hydrodynamics (GRSPH), based on an entropy-conservative form of the general relativistic hydrodynamic equations for a perfect fluid. We aim to replace approximate treatments of general relativity in current SPH simulations of tidal disruption events and accretion discs. We develop an improved shock capturing formulation that distinguishes between shock viscosity and conductivity in relativity. We also describe a new Hamiltonian time integration algorithm for relativistic orbital dynamics and GRSPH. Our method correctly captures both Einstein and spin-induced precession around black holes. We benchmark our scheme in 1D and 3D against mildly and ultra relativistic shock tubes, exact solutions for epicyclic and vertical oscillation frequencies, and Bondi accretion. We assume fixed background metrics (Minkowski, Schwarzschild and Kerr in Cartesian Boyer-Lindquist coordinates) but the method lays the foundation for future direct coupling with numerical relativity.

23 pages, 22 figures, accepted to MNRAS

References in corpus (8)

• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• Multi-messenger Observations of a Binary Neutron Star Merger
• Smoothed Particle Hydrodynamics and Magnetohydrodynamics
• Modelling discontinuities and Kelvin-Helmholtz instabilities in SPH
• Inviscid SPH
• Astrophysical Smooth Particle Hydrodynamics
• Imaging the Schwarzschild-radius-scale Structure of M87 with the Event Horizon Telescope using Sparse Modeling
• On the Bardeen-Petterson Effect in black hole accretion discs

Cited by in corpus (2)

• Simulations of Tidal Disruption Events
• Future Simulations of Tidal Disruption Events