General relativistic smoothed particle hydrodynamics
arXiv:1901.08064 · doi:10.1093/mnras/stz111
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 (38)
- GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
- Multi-messenger Observations of a Binary Neutron Star Merger
- The Dynamics of General Relativity
- Cosmological SPH simulations: The entropy equation
- HARM: A Numerical Scheme for General Relativistic Magnetohydrodynamics
- Smoothed Particle Hydrodynamics and Magnetohydrodynamics
- Rotating Stars in Relativity
- Kilonovae
- Phantom: A smoothed particle hydrodynamics and magnetohydrodynamics code for astrophysics
- Accretion during the merger of supermassive black holes
- Modelling discontinuities and Kelvin-Helmholtz instabilities in SPH
- Relativistic Fluid Dynamics: Physics for Many Different Scales
- An energy-conserving formalism for adaptive gravitational force softening in SPH and N-body codes
- Inviscid SPH
- The Afterglow of Massive Black Hole Coalescence
- Disc formation from tidal disruptions of stars on eccentric orbits by Schwarzschild black holes
- SPH compressible turbulence
- An efficient shock-capturing central-type scheme for multidimensional relativistic flows. I. Hydrodynamics
- Circularization of Tidally Disrupted Stars around Spinning Supermassive Black Holes
- Finite, Intense Accretion Bursts from Tidal Disruption of Stars on Bound Orbits
- Astrophysical Smooth Particle Hydrodynamics
- Imaging the Schwarzschild-radius-scale Structure of M87 with the Event Horizon Telescope using Sparse Modeling
- RAM: A Relativistic Adaptive Mesh Refinement Hydrodynamics Code
- On the Bardeen-Petterson Effect in black hole accretion discs
- Tearing up the disc: how black holes accrete
- Conformally Flat Smoothed Particle Hydrodynamics: Application to Neutron Star Mergers
- The Exact Solution of the Riemann Problem in Relativistic MHD
- The evolution of a warped disc around a Kerr black hole
- Discriminating Strange Star Mergers from Neutron Star Mergers by Gravitational-Wave Measurements
- An accurate Newtonian description of particle motion around a Schwarzschild black hole
- Tidal disruptions by rotating black holes: relativistic hydrodynamics with Newtonian codes
- Hydrodynamic Interaction between the Be Star and the Pulsar in the TeV Binary PSR B1259-63/LS 2883
- Conservative, special-relativistic smoothed particle hydrodynamics
- Smoothed Particle Hydrodynamics Simulations of Ultra-Relativistic Shocks with Artificial Viscosity
- A physical model for state transitions in black hole X-ray binaries
- Mergers of Irrotational Neutron Star Binaries in Conformally Flat Gravity
- Gas squeezing during the merger of a supermassive black hole binary
- Pseudo-Newtonian Potentials for Nearly Parabolic Orbits
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- The Lunar Gravitational-wave Antenna: Mission Studies and Science Case
- The Cosmological Simulation Code OpenGadget3 -- Implementation of Meshless Finite Mass
- SPHINCS_BSSN: A general relativistic Smooth Particle Hydrodynamics code for dynamical spacetimes
- Electromagnetic Signatures from the Tidal Tail of a Black Hole - Neutron Star Merger
- Emission signatures from sub-pc Post-Newtonian binaries embedded in circumbinary discs
- Gravitational waves from tidal disruption events: an open and comprehensive catalogue
- Simulating neutron star mergers with the Lagrangian Numerical Relativity code SPHINCS_BSSN
- Radio emission from tidal disruption events produced by the collision between super-Eddington outflows and the circumnuclear medium
- Optical Appearance of Eccentric Tidal Disruption Events
- Simulations of Tidal Disruption Events
- Astrophysics with the Laser Interferometer Space Antenna
- Converged simulations of the nozzle shock in tidal disruption events
- Future Simulations of Tidal Disruption Events
- A general relativistic extension to mesh-free methods for hydrodynamics
- Stars Crushed by Black Holes. III. Mild Compression of Radiative Stars by Supermassive Black Holes
- A general relativistic magnetohydrodynamics extension to mesh-less schemes in the code GIZMO
- Scattering of massive particles from black holes and naked singularities
- Special Relativistic Smoothed Particle Hydrodynamics Based on Riemann Solver