Structure Formation in the Universe by Exact Methods

Details Structure Formation in the Universe by Exact Methods Structure Formation in the Universe by Exact Methods

Feb 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005tmgm.meet...80k&link_type=abstract

The Tenth Marcel Grossmann Meeting. Proceedings of the MG10 Meeting held at Brazilian Center for Research in Physics (CBPF), Rio

Physics

1

Scientific paper

The evolution equations of the Lemaître-Tolman (LT) model are reformulated in such a way that the distributions of matter density ρi or matter velocity υi at two different times ti, i = 1, 2 are the input data (any two of the four quantities uniquely determine an LT model). This formulation is better suited to observational practice in cosmology. Then, numerical examples of the LT models are constructed that evolve between a certain density or velocity distribution at t1 = last scattering epoch and a model of a modern structure at t2 = the present time. The amplitude of the inhomogeneity at t1 is kept within the limits implied by observations, and the final modern structures are galaxy clusters, voids or galaxies with a central black hole. Among other things, it is shown that the initial velocity distribution plays an essential role in the formation of structures, the density distribution alone does not even determine whether the final structure will be a void or a condensation.

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