Abstract
We study the evolution of thick domain walls in the different models of cosmological inflation, in the matter-dominated and radiation-dominated universe, or more generally in the universe with the equation of state p=wrho . We have found that the domain wall evolution crucially depends on the time-dependent parameter C(t)=1/(H(t)delta _0)^2, where H(t) is the Hubble parameter and delta _0 is the thickness of the wall in flat space-time. For C(t)>2 the physical thickness of the wall, a(t)delta (t), tends with time to delta _0, which is microscopically small. Otherwise, when C(t) le 2, the wall steadily expands and can grow up to a cosmologically large size.
Highlights
Another problem of the baryogenesis based on spontaneous C P violation is the thickness of the wall
In this work we studied the evolution of thick domain walls in the different models of inflation, as well as for arbitrary cosmological expansion regimes with the matter satisfying the equation of state p = wρ with constant parameter w
We have shown that there exists some range of the inflation parameters leading to a large domain separation prior to successful baryogenesis
Summary
Another problem of the baryogenesis based on spontaneous C P violation is the thickness of the wall. In flat spacetime the thickness of the wall is microscopically small and if the walls with such or similar thicknesses were created in the cosmological situation, the matter-antimatter domains would be in close contact with each other. The cosmological expansion may lead to much larger separation of the domains eliminating or smoothing down this problem. In this work we studied the evolution of thick domain walls in the different models of inflation, as well as for arbitrary cosmological expansion regimes with the matter satisfying the equation of state p = wρ with constant parameter w. We have shown that there exists some range of the inflation parameters leading to a large domain separation prior to successful baryogenesis
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