Kinematical classification of evolving loops and bubbles

Details Kinematical classification of evolving loops and bubbles Kinematical classification of evolving loops and bubbles

Jan 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994nuphb.412..391d&link_type=abstract

Nuclear Physics B, Volume 412, Issue 1-2, p. 391-405.

Physics

Nuclear Physics

4

Scientific paper

The evolution of cosmic loops (and bubbles) in an inflationary background is governed by a hyperbolic fixed point. Associated with the four distinguished kinematical categories are loops which have or could not have undergone a world-sheet big bang, and which eventually collapse or else keep growing. In particular we discuss spontaneous creation of baby loops, and quantum nucleation of horizon-size loops. World-sheet scalar potentials are invoked to account for the electromagnetic self-interactions of charged and/or superconducting loops. The electromagnetic repulsion at short distances then acts to exclude stationary breathing configurations provided their total charge Q is above a certain critical value set by the string tension/Hubble scale ratio. However, below that critical value there exist charged loops which classically are not inflated by inflation. Quantum-mechanical tunneling renders the classically stable charged loops unstable, and the associated Basu-Guth-Vilenkin amplitude gets a contribution proportional to Q2 log Q2 for small Q.

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