No cosmological domain wall problem for weakly coupled fields
After inflation occurs, a weakly coupled scalar field will in general not be in thermal equilibrium but have a distribution of values determined by the inflationary Hubble parameter. If such a field subsequently undergoes discrete symmetry breaking, then the different degenerate vacua may not be equ...
| Main Authors: | , |
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| Format: | Journal article |
| Language: | English |
| Published: |
2001
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