Evolution of thick domain walls in inflationary and universe

A. D. Dolgov; S. I. Godunov; A. S. Rudenko

doi:10.1140/epjc/s10052-018-6350-7

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2024 Impact factor 4.8

Particles and Fields

Open Access

Eur. Phys. J. C (2018) 78: 855
https://doi.org/10.1140/epjc/s10052-018-6350-7

Regular Article - Theoretical Physics

Evolution of thick domain walls in inflationary and $p=w\rho$ universe

A. D. Dolgov¹^,2, S. I. Godunov¹^,2 and A. S. Rudenko¹^,3^*

¹ Novosibirsk State University, Novosibirsk, 630090, Russia
² Institute for Theoretical and Experimental Physics, Moscow, 117218, Russia
³ Budker Institute of Nuclear Physics, Novosibirsk, 630090, Russia

^* e-mail: a.s.rudenko@inp.nsk.su

Received: 17 August 2018
Accepted: 12 October 2018
Published online: 25 October 2018

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 $p=w\rho$ . 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.