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General relativistic smoothed particle hydrodynamics
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General relativistic smoothed particle hydrodynamics
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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.
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Cited by 1 Pith paper
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Are most detected tidal disruption events partial?
SPH simulations of zero-energy partial TDEs find fallback ~t^{-9/4}, optical luminosities 10^{42-44} erg/s at 10^4 K and radii 10-100 au, indicating many detected TDEs may be partial rather than full.
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