The Cosmological

Application of the Theory of General Relativity to the large-scale structure of the Universe leads to various cosmological theories. Of these, the most important are a class of solutions called Friedmann cosmologies that lead to what is termed the hot big bang. The starting point for these theories is what is termed cosmological principle:

Viewed on sufficiently large distance scales, there are no preferred
directions or preferred places in the Universe.
Stated simply, this principle means that averaged over large enough distances, one part of the Universe looks approximately like any other part.

This clearly is not true on short distance scales: your classroom probably looks rather different from your dormitory room, and we certainly see distinguishing structure like galactic superclusters and the Great Wall up to at least 100-200 Mpc scales. However, well beyond those distance scales there is strong observational evidence for the cosmological principle.

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