Inflation with $\Omega \neq 1$

Linde, Andrei D.; Mezhlumian, Arthur

doi:10.1103/PhysRevD.52.6789

Inflation with $\Omega \neq 1$

Jun, 1995

19 pages

Published in:

Phys.Rev.D 52 (1995) 6789-6804

e-Print:

astro-ph/9506017 [astro-ph]

DOI:

10.1103/PhysRevD.52.6789

Report number:

SU-ITP-95-11

View in:

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Abstract: (arXiv)

We discuss various models of inflationary universe with

\Omega \not = 1

. A homogeneous universe with

\Omega > 1

may appear due to creation of the universe "from nothing" in the theories where the effective potential becomes very steep at large

\phi

, or in the theories where the inflaton field

\phi

nonminimally couples to gravity. Inflation with

\Omega < 1

generally requires intermediate first order phase transition with the bubble formation, and with a second stage of inflation inside the bubble. It is possible to realize this scenario in the context of a theory of one scalar field, but typically it requires artificially bent effective potentials and/or nonminimal kinetic terms. It is much easier to obtain an open universe in the models involving two scalar fields. However, these models have their own specific problems. We propose three different models of this type which can describe an open homogeneous inflationary universe.

Note:

29 pages, LaTeX, parameters of one of the models are slightly modified

inflation
matter: density
field theory: scalar
effective potential
tunneling
bubble: production
production: bubble
critical phenomena
bibliography

References(67)

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Inflation with Ω≠1\Omega \neq 1Ω=1

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Inflation with $\Omega \neq 1$