On general conditions for inflation

Details On general conditions for inflation On general conditions for inflation

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986phlb..181..238p&link_type=abstract

Physics Letters B, Volume 181, Issue 3-4, p. 238-243.

Physics

38

Scientific paper

The classical evolution of a Friedmann universe, coupled to a scalar field, is examined in an attempt to find under which initial conditions chaotic inflation occurs. It is shown that if φ>mpl/√4π this universe enters naturally into and exits out of an inflationary phase. This behavior takes place under a large variety of scalar potentials including polynomial, logarithmic and exponential potentials. Within the context of our approximation, deviation from homogeneity still leads to an inflationary phase. It is also shown that a scalar field is essential as a source for inflation. Other fields like the massive vector field are unlikely to cause an inflationary phase.
I am grateful to Avishai Dekel and Nathan Seiberg and to the participants of the Aspen Workshops on inflation and strings for many helpful comments and to Jeremey Goodman for helpful discussion which led to the argument about the impossibility of inflation which nonscalar fields. I would like to thank the Aspen Center for Physics for hospitality while a revised version of the paper was written.

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