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Title: Domain walls in a FRW universe

Abstract

We solve the equations of motion for a scalar field with domain wall boundary conditions in a Friedmann-Robertson-Walker (FRW) spacetime. We find (in agreement with Basu and Vilenkin) that no domain wall solutions exist in de Sitter spacetime for {ital H}{equivalent_to}{ital H}/{ital m}{ge}1/2, where {ital H} is the Hubble parameter and {ital m} is the scalar mass. In the general FRW case we develop a systematic perturbative expansion in {ital h} to arrive at an approximate solution to the field equations. We calculate the energy-momentum tensor of the domain wall configuration, and show that the energy density can become {ital negative} at the core of the defect for some values of the nonminimal coupling parameter {xi}. We develop a translationally invariant theory for fluctuations of the wall, obtain the effective Lagrangian for these fluctuations, and quantize them using the Bunch-Davies vacuum in the de Sitter case. Unlike previous analyses, we find that the fluctuations act as zero-mass (as opposed to tachyonic) modes. This allows us to calculate the distortion and the normal-normal correlators for the surface. The normal-normal correlator decreases logarithmically with the distance between points for large times and distances, indicating that the interface becomes rougher than in Minkowskimore » spacetime.« less

Authors:
; ; ; ;  [1]
  1. Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, Pennsylvania 15260 (United States)
Publication Date:
Research Org.:
Carnegie-Mellon University
OSTI Identifier:
130742
DOE Contract Number:  
FG02-91ER40682
Resource Type:
Journal Article
Journal Name:
Physical Review, D
Additional Journal Information:
Journal Volume: 52; Journal Issue: 10; Other Information: PBD: 15 Nov 1995
Country of Publication:
United States
Language:
English
Subject:
66 PHYSICS; UNIVERSE; SCALAR FIELDS; EQUATIONS OF MOTION; SPACE-TIME; BOUNDARY CONDITIONS; MASS; PERTURBATION THEORY; FIELD EQUATIONS; ENERGY-MOMENTUM TENSOR; FLUCTUATIONS; LAGRANGIAN FUNCTION; MINKOWSKI SPACE

Citation Formats

Boyanovsky, D, Brahm, D E, Gonzalez-Ruiz, A, Holman, R, Takakura, F I, and Carnegie Mellon Physics Department, Carnegie Mellon University, Pittsburgh, Pennsylvania 15213. Domain walls in a FRW universe. United States: N. p., 1995. Web. doi:10.1103/PhysRevD.52.5516.
Boyanovsky, D, Brahm, D E, Gonzalez-Ruiz, A, Holman, R, Takakura, F I, & Carnegie Mellon Physics Department, Carnegie Mellon University, Pittsburgh, Pennsylvania 15213. Domain walls in a FRW universe. United States. doi:10.1103/PhysRevD.52.5516.
Boyanovsky, D, Brahm, D E, Gonzalez-Ruiz, A, Holman, R, Takakura, F I, and Carnegie Mellon Physics Department, Carnegie Mellon University, Pittsburgh, Pennsylvania 15213. Wed . "Domain walls in a FRW universe". United States. doi:10.1103/PhysRevD.52.5516.
@article{osti_130742,
title = {Domain walls in a FRW universe},
author = {Boyanovsky, D and Brahm, D E and Gonzalez-Ruiz, A and Holman, R and Takakura, F I and Carnegie Mellon Physics Department, Carnegie Mellon University, Pittsburgh, Pennsylvania 15213},
abstractNote = {We solve the equations of motion for a scalar field with domain wall boundary conditions in a Friedmann-Robertson-Walker (FRW) spacetime. We find (in agreement with Basu and Vilenkin) that no domain wall solutions exist in de Sitter spacetime for {ital H}{equivalent_to}{ital H}/{ital m}{ge}1/2, where {ital H} is the Hubble parameter and {ital m} is the scalar mass. In the general FRW case we develop a systematic perturbative expansion in {ital h} to arrive at an approximate solution to the field equations. We calculate the energy-momentum tensor of the domain wall configuration, and show that the energy density can become {ital negative} at the core of the defect for some values of the nonminimal coupling parameter {xi}. We develop a translationally invariant theory for fluctuations of the wall, obtain the effective Lagrangian for these fluctuations, and quantize them using the Bunch-Davies vacuum in the de Sitter case. Unlike previous analyses, we find that the fluctuations act as zero-mass (as opposed to tachyonic) modes. This allows us to calculate the distortion and the normal-normal correlators for the surface. The normal-normal correlator decreases logarithmically with the distance between points for large times and distances, indicating that the interface becomes rougher than in Minkowski spacetime.},
doi = {10.1103/PhysRevD.52.5516},
journal = {Physical Review, D},
number = 10,
volume = 52,
place = {United States},
year = {1995},
month = {11}
}