We have developed a fully general relativistic hydrodynamics code (thorn_MAHC) based on high resolution shock capturing methods as a general-purpose tool for research in relativistic astrophysics. The hydrodynamic evolution is coupled to the spacetime evolution through the cactus code. A version of the general relativistic hydro plus spacetime code (GR3D) has recently been submitted to NASA with full documentation as the second milestone code of the Neutron Star Coalescence Grand Challenge Project. The code has been tested to run at over 140GFlops on a 1024 node T3E. To obtain a copy of the code and see some of the general relativistic hydro simulations carried out with it, please visit GR3D Code .Currently, the code has passed convergence tests on Friedmann-Robertson-Walker cosmologies containing dust, Oppenhiemer-Snyder dust collapse, shocktube problems, Tolman-Oppenheimer-Volkoff (TOV) static stars, and boosted TOV stars. We also have run neutron star head-on collisions and brill wave collisions with neutron stars. Together with many other members of the NCSA/Potsdam/Wash U hydro team, we are studying the long term stability of general relativistic hydro simulations, the comparison of 3D simulations with 1D and 2D simulations, and convergence tests of rotating neutron stars. We will also be comparing 3D simulations to perturbation studies.
A series of papers on our general relativistic hydro formulation, the numerical treatments and the results of testbeds is currently in preparation.
Mark Miller / mamiller@void.wustl.edu
Last updated: June 9, 1998