1988/12/01 by A. E. Evrard, August E. Evrard · 5 citations
Physics and Astronomy · #Gamma-ray bursts and supernovae #Astronomy and Astrophysical Research #Scientific Research and Discoveries
paper · doi:10.1093/mnras/235.3.911
We presents a numerical method for following the hydrodynamics of a gaseous component in 3D cosmological simulations containing both gas and collisionless components. The code is the merged product of two existing approaches – the high-resolution P3M N-body program developed by Efstathiou & Eastwood, and SPH, the smoothed particle hydrodynamics approach of Monaghan & Gingold. The gas physics incorporated within the model includes self-gravity, the gravity from additional collisionless components, adiabatic heating, heating due to shocks, and radiative cooling. The use of variable spatial resolution allows reliable definition of a wide dynamic range. This makes the code optimal for tackling the general problem of clustering from an initially Gaussian random field.