@MISC{Mezhlumian94stationaryuniverse, author = {Arthur Mezhlumian}, title = {Stationary Universe Model: Inputs and Outputs 1}, year = {1994} }

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Abstract

This talk presents the recent progress achieved in collaboration with A.Linde and D.Linde 1,2,3 towards understanding the true nature of the global spatial structure of the universe as well as the most general stationary characteristics of its time-dependent state with eternally growing total volume. In our opinion, the simplest and, simultaneously, the most general version of inflationary cosmology is the chaotic inflation scenario. It can be realized in all models were the other versions of inflationary theory can be realized (see [4] for detailed account). Several years ago it was realized that inflation in these theories has a very interesting property 5,6 which will be discussed in this talk. If the universe contains at least one inflationary domain of a size of horizon (h-region) with a sufficiently large and homogeneous scalar field φ, then this domain will permanently produce new h-regions of a similar type. During this process the total physical volume of the inflationary universe (which is proportional to the total number of h-regions) will grow indefinitely. Fortunately, some kind of stationarity may exist in many models of inflationary universe due to the process of the universe self-reproduction 4. The properties of inflationary domains formed during the process of the self-reproduction of the universe do not depend on the moment of time at which each such domain is formed; they depend only on the value of the scalar fields inside each domain, on the average density of matter in this domain and on the physical length scale. This talk will describe what assumptions and approximations are made in order to get this picture of the universe and what consequences they bear. Let us consider the simplest model of chaotic inflation based on the theory of a scalar