No cosmological domain wall problem for weakly coupled fields

Details No cosmological domain wall problem for weakly coupled fields No cosmological domain wall problem for weakly coupled fields

2001-06-25

arxiv.org/abs/hep-ph/0106272v2

Phys.Rev.D65:025002,2002

Physics

High Energy Physics

High Energy Physics - Phenomenology

17 pages, 4 figures (Revtex), clarifying Comments added in Introduction; to appear in Phys. Rev D

Scientific paper

10.1103/PhysRevD.65.025002

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 equally populated so the domain walls which form will be `biased' and the wall network will subsequently collapse. Thus the cosmological domain wall problem may be solved for sufficiently weakly coupled fields in a post-inflationary universe. We quantify the criteria for determining whether this does happen, using a Higgs-like potential with a spontaneously broken $Z_2$ symmetry.

Affiliated with

Also associated with

No associations

Rating

No cosmological domain wall problem for weakly coupled fields does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with No cosmological domain wall problem for weakly coupled fields, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and No cosmological domain wall problem for weakly coupled fields will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-194102