Evolution of topological defects during inflation.

Topological defects can be formed during inflation by phase transitions as well as by quantum nucleation. We study the effect of the expansion of the Universe on the internal structure of the defects. We look for stationary solutions to the field equations, i.e., solutions that depend only on the proper distance from the defect core. In the case of very thin defects, whose core dimensions are much smaller than the de Sitter horizon, we find that the solutions are well approximated by the flat space solutions. However, as the flat space thickness parameter ${\mathrm{\ensuremath{\delta}}}_{0}$ increases we notice a deviation from this, an effect that becomes dramatic as ${\mathrm{\ensuremath{\delta}}}_{0}$ approaches ${\mathit{H}}^{\mathrm{\ensuremath{-}}1}$/ \ensuremath{\surd}2 . Beyond this critical value we find no stationary solutions to the field equations. We conclude that only defects that have flat space thicknesses less than the critical value survive, while thicker defects are smeared out by the expansion.