Due to the vast body of literature on numerical simulations dealing with the post-recombination epoch, only a very small fraction of published work can be reviewed in this paper. Hence, the following summary is limited to cover just a few aspects of computational physical cosmology, and in particular those that can potentially be used to discriminate between cosmological model parameters, even within the realm of the standard model.
For a general overview of theoretical and
observational issues associated with structure formation, the
reader is referred to
[132, 131], and to
[45
]
for a broad review of numerical simulations (and methods) of
structure formation.
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