Three Dimensional Numerical General Relativistic Hydrodynamics I: Formulations, Methods, and Code Tests

Details Three Dimensional Numerical General Relativistic Hydrodynamics I: Formulations, Methods, and Code Tests Three Dimensional Numerical General Relativistic Hydrodynamics I: Formulations, Methods, and Code Tests

1998-11-04

arxiv.org/abs/gr-qc/9811015v1

Phys.Rev. D61 (2000) 044011

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

45 pages RevTeX, 34 figures

Scientific paper

10.1103/PhysRevD.61.044011

This is the first in a series of papers on the construction and validation of a three-dimensional code for general relativistic hydrodynamics, and its application to general relativistic astrophysics. This paper studies the consistency and convergence of our general relativistic hydrodynamic treatment and its coupling to the spacetime evolutions described by the full set of Einstein equations with a perfect fluid source. The numerical treatment of the general relativistic hydrodynamic equations is based on high resolution shock capturing schemes. These schemes rely on the characteristic information of the system. A spectral decomposition for general relativistic hydrodynamics suitable for a general spacetime metric is presented. Evolutions based on three different approximate Riemann solvers coupled to four different discretizations of the Einstein equations are studied and compared. The coupling between the hydrodynamics and the spacetime (the right and left hand side of the Einstein equations) is carried out in a treatment which is second order accurate in {\it both} space and time. Convergence tests for all twelve combinations with a variety of test beds are studied, showing consistency with the differential equations and correct convergence properties. The test-beds examined include shocktubes, Friedmann-Robertson-Walker cosmology tests, evolutions of self-gravitating compact (TOV) stars, and evolutions of relativistically boosted TOV stars. Special attention is paid to the numerical evolution of strongly gravitating objects, e.g., neutron stars, in the full theory of general relativity, including a simple, yet effective treatment for the surface region of the star (where the rest mass density is abruptly dropping to zero).

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