Abstract
The problem of vacuum stability for interacting scalar fields is studied at the one-loop level in situations where the effective potential may not be used. The method described here involves a calculation of the one-loop effective action using the background-field method. Specific examples discussed are interacting twisted and untwisted scalar fields in S/sup 1/ x R/sup 3/, and self-interacting scalar fields in the static Einstein universe and in flat space-time with topology R/sup 1/ x S/sup 1/ x S/sup 1/ x S/sup 1/. It is shown that in some cases radiative corrections can lead to a phase transition where the classical vacuum state becomes unstable.
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