Physics
Scientific paper
May 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987sccs.conf..403t&link_type=abstract
Superstrings, Cosmology Composite Structures; proceedings from the international workshop held March 11-18, 1987, at the Center
Physics
Big Bang Cosmology, Galactic Evolution, Relativity, Space-Time Functions, String Theory, Hubble Constant, Interstellar Magnetic Fields, Scalars, Stellar Evolution
Scientific paper
The big bang cosmology is a highly successful model, providing a reliable and tested accounting of the Universe from 0.01 sec after the bang until today, some 15 Gyr later. However, very special initial data seem to be required in order to account for the observed smoothness and flatness of our Hubble volume and for the existence of the small primeval density inhomogeneities required for the formation of structure in the Universe. Inflation offers a means of accounting for these special initial data, which is based on physics at sub-planck energy scales (much less than mpl approx. = 10 to the 19th power GeV) and is motivated by contemporary ideas in particle theory. Here the status of the Inflationary Paradigm is reviewed. At present essentially all inflationary models involve a very weakly-coupled (quantified by the presence of a dimensionless parameter of order 10 to the -12 or so) scalar field which is displaced from the minimum of its potential. Regions of the Universe where the scalar field is initially displaced from its minimum undergo inflation as the scalar field relaxes, resulting in a Universe today which resembles ours in regions much larger than our present Hubble volume (approx. = 10 to the 28 cm), may be highly irregular. The most conspicuous blemish on the paradigm is the lack of a compelling particle physics model to implement it. Also reviewed are some other unresolved issues, and the all important confrontation between inflation and observational data is fully discussed. Finally, the possibility that inflation leads to large-scale, primeval magnetic fields of sufficient strength to be of astrophysical interest is covered.
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