By Alan H. Guth (auth.), T. Shanks, A. J. Banday, R. S. Ellis, C. S. Frenk, A. W. Wolfendale (eds.)

This publication represents the court cases from the NATO subsidized complicated learn Workshop entitled "Observational checks of Inflation" held on the collage of Durham, England at the 10th-14th December, 1990. in recent times, the cosmological inflation version has drawn jointly the worlds of particle physics, theoretical cosmology and observational astronomy. the purpose of the workshop was once to compile specialists in all of those fields to debate the present prestige of the inflation conception and its observational predictions. the easiest inflation version makes transparent predictions that are testable by way of astronomical commentary. most excellent is the prediction that the cosmological density parameter, no, must have a price negligibly assorted from the severe, Einstein-de Sitter price of 00=1. the opposite major prediction is that the spectrum of primordial density fluctuations could be Gaussian and take the Harrison-Zeldovich shape. The prediction that n =l, in patticular, results in numerous vital results o for cosmology. to begin with, there's the plain contradiction with the bounds on baryon density from monstrous Bang nucleosynthesis which has ended in the typical conjecture that weakly interacting debris instead of baryons may well shape the dominant mass constituent of the Universe. Secondly, with n =l, the age of the Universe is uncomfortably brief if o the Hubble consistent and the a long time of the oldest famous person clusters lie inside their presently believed limits.

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**Observational Tests of Cosmological Inflation**

This booklet represents the court cases from the NATO subsidized complicated examine Workshop entitled "Observational checks of Inflation" held on the collage of Durham, England at the 10th-14th December, 1990. in recent times, the cosmological inflation version has drawn jointly the worlds of particle physics, theoretical cosmology and observational astronomy.

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N =1 (± '" 10- 4 ) : A quick glance at the contents of this volume will rapidly convince the reader that this is an extremely important prediction. 01 < n < 10, inflation is much more stringent, and in the process of solving the other cosmological problems adequately n is forced very close to 1 [25). ) As we shall shortly see, quantum effects during inflation can also give rise to density perturbations which are constrained by current observations to be no larger than say 10- 4 . These are superimposed on the 'classical' value of 1, which would be obtained to a much higher degree of accuracy even than this if density perturbations were not generated.

Thus it would require an infinite energy density to have excitations down to arbitrarily small wavelengths, so I think it's reasonable to assume that this is impossible. As long as the energy density is finite, there must be some wavelength below which there are no excitations at all. There are, however, also quantum zero point fluctuations, and the story about them is a bit more complicated. These zero point fluctuations do persist down to arbitrarily small wavelength, at least in the context of a quantum field theory, but the fluctuations are not arbitrarythey are completely controlled by the theory.

So will our descendents eventually see the edge of our domain? Guth: Yes, in principle our ancestors will at some time in the distant future be able to see the edge of our domain. It is possible even that the domain is closed, in which case the wall will hit them in the face. The time for this to happen, however, is proportional to the cube of the overall expansion factor, and so it will not happen until the extremely distant future. Sarkar: You suggested that the entropy of the universe is large.