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.
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A. E. Evrard (1988) studied this question.