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Evolution of thick domain walls in inflationary and p= wρ universe. / Dolgov, A. D.; Godunov, S. I.; Rudenko, A. S.

In: European Physical Journal C, Vol. 78, No. 10, 855, 25.10.2018.

Research output: Contribution to journal › Article › peer-review

Harvard

Dolgov, AD, Godunov, SI & Rudenko, AS 2018, 'Evolution of thick domain walls in inflationary and p= wρ universe', European Physical Journal C, vol. 78, no. 10, 855. https://doi.org/10.1140/epjc/s10052-018-6350-7

APA

Dolgov, A. D., Godunov, S. I., & Rudenko, A. S. (2018). Evolution of thick domain walls in inflationary and p= wρ universe. European Physical Journal C, 78(10), [855]. https://doi.org/10.1140/epjc/s10052-018-6350-7

Vancouver

Dolgov AD, Godunov SI, Rudenko AS. Evolution of thick domain walls in inflationary and p= wρ universe. European Physical Journal C. 2018 Oct 25;78(10):855. doi: 10.1140/epjc/s10052-018-6350-7

Author

Dolgov, A. D. ; Godunov, S. I. ; Rudenko, A. S. / Evolution of thick domain walls in inflationary and p= wρ universe. In: European Physical Journal C. 2018 ; Vol. 78, No. 10.

BibTeX

@article{6009443584f74b2abd3f1822aa2eb882,
title = "Evolution of thick domain walls in inflationary and p= wρ universe",
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= wρ. We have found that the domain wall evolution crucially depends on the time-dependent parameter C(t)=1/(H(t)δ0)2, where H(t) is the Hubble parameter and δ0 is the thickness of the wall in flat space-time. For C(t) > 2 the physical thickness of the wall, a(t) δ(t) , tends with time to δ0, which is microscopically small. Otherwise, when C(t) ≤ 2 , the wall steadily expands and can grow up to a cosmologically large size.",
author = "Dolgov, {A. D.} and Godunov, {S. I.} and Rudenko, {A. S.}",
note = "Publisher Copyright: {\textcopyright} 2018, The Author(s).",
year = "2018",
month = oct,
day = "25",
doi = "10.1140/epjc/s10052-018-6350-7",
language = "English",
volume = "78",
journal = "European Physical Journal C",
issn = "1434-6044",
publisher = "Springer Nature",
number = "10",

}

RIS

TY - JOUR

T1 - Evolution of thick domain walls in inflationary and p= wρ universe

AU - Dolgov, A. D.

AU - Godunov, S. I.

AU - Rudenko, A. S.

N1 - Publisher Copyright: © 2018, The Author(s).

PY - 2018/10/25

Y1 - 2018/10/25

N2 - 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= wρ. We have found that the domain wall evolution crucially depends on the time-dependent parameter C(t)=1/(H(t)δ0)2, where H(t) is the Hubble parameter and δ0 is the thickness of the wall in flat space-time. For C(t) > 2 the physical thickness of the wall, a(t) δ(t) , tends with time to δ0, which is microscopically small. Otherwise, when C(t) ≤ 2 , the wall steadily expands and can grow up to a cosmologically large size.

AB - 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= wρ. We have found that the domain wall evolution crucially depends on the time-dependent parameter C(t)=1/(H(t)δ0)2, where H(t) is the Hubble parameter and δ0 is the thickness of the wall in flat space-time. For C(t) > 2 the physical thickness of the wall, a(t) δ(t) , tends with time to δ0, which is microscopically small. Otherwise, when C(t) ≤ 2 , the wall steadily expands and can grow up to a cosmologically large size.

UR - http://www.scopus.com/inward/record.url?scp=85055737292&partnerID=8YFLogxK

U2 - 10.1140/epjc/s10052-018-6350-7

DO - 10.1140/epjc/s10052-018-6350-7

M3 - Article

AN - SCOPUS:85055737292

VL - 78

JO - European Physical Journal C

JF - European Physical Journal C

SN - 1434-6044

IS - 10

M1 - 855

ER -

ID: 17288165