Abstract
An implicit, adaptive-mesh numerical technique is described for modeling ultrarelativist ic (Y >> 1) gas flows in flat spacetime in one space dimension. The numerical code is an adaptation of the WH80s Newtonian radiation hydrodynamics code described by Winkler and Norman in these proceedings. Shock fronts are treated by the method of artificial viscosity. We derive the equations of motion for an ideal gas with artificial viscosity in Eulerian and arbitrarily-moving coordinates. We show through numerical examples the systematic errors that result from inconsistently omitting or including the artificial viscous “pressure” in the Eulerian equations of motion. These errors are eliminated in the present code, which gives good results on three test problems involving strong relativistic shock waves.
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Norman, M.L., Winkler, KH.A. (1986). Why Ultrarelativistic Numerical Hydrodynamics is Difficult. In: Winkler, KH.A., Norman, M.L. (eds) Astrophysical Radiation Hydrodynamics. NATO ASI Series, vol 188. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-4754-2_13
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DOI: https://doi.org/10.1007/978-94-009-4754-2_13
Publisher Name: Springer, Dordrecht
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