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The Advent of Cosmological Gas Dynamic Simulations

Published online by Cambridge University Press:  03 August 2017

August E. Evrard*
Affiliation:
Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK

Extract

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The next move forward in simulations of cosmological structure is to include the hydrodynamics and thermal history of a gaseous component. The task is not an easy one. The dynamic range is wide in all interesting quantities (density, temperature, length-scales, time-scales, etc.). Generic initial mass distributions sampled from Gaussian random fields will, for many interesting power spectra, lead to a high degree of substructure present at all stages of the evolution. Grid-based hydrodynamic techniques currently lack the resolution necessary to evolve several levels of a clustering hierarchy simultaneously. A particle-based method known as SPH (Smoothed Particle Hydrodynamics, see Monoghan (1985) for a review) appears best suited for cosmological application. I have recently imbedded the technique into the P3M N-body code, described by Efstathiou et al. (1985) and used extensively by Efstathiou and collaborators, most recently in investigations of the cold dark matter scenario.

Type
Appendix 1: Poster Papers
Copyright
Copyright © Reidel 1988 

References

Efstathiou, G., Davis, M., Frenk, C. and White, S. 1985, Ap. J. Supl., 57, 241.Google Scholar
Evrard, A.E. 1987, in preparation.Google Scholar
Monaghan, J.J. 1985 Comp. Phys. Reports, 3, 71.Google Scholar