Domain walls in a FRW universe
Abstract
We solve the equations of motion for a scalar field with domain wall boundary conditions in a FriedmannRobertsonWalker (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 energymomentum 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 BunchDavies vacuum in the de Sitter case. Unlike previous analyses, we find that the fluctuations act as zeromass (as opposed to tachyonic) modes. This allows us to calculate the distortion and the normalnormal correlators for the surface. The normalnormal correlator decreases logarithmically with the distance between points for large times and distances, indicating that the interface becomes rougher than in Minkowskimore »
 Authors:

 Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, Pennsylvania 15260 (United States)
 Publication Date:
 Research Org.:
 CarnegieMellon University
 OSTI Identifier:
 130742
 DOE Contract Number:
 FG0291ER40682
 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; SPACETIME; BOUNDARY CONDITIONS; MASS; PERTURBATION THEORY; FIELD EQUATIONS; ENERGYMOMENTUM TENSOR; FLUCTUATIONS; LAGRANGIAN FUNCTION; MINKOWSKI SPACE
Citation Formats
Boyanovsky, D, Brahm, D E, GonzalezRuiz, 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, GonzalezRuiz, 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, GonzalezRuiz, 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 GonzalezRuiz, 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 FriedmannRobertsonWalker (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 energymomentum 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 BunchDavies vacuum in the de Sitter case. Unlike previous analyses, we find that the fluctuations act as zeromass (as opposed to tachyonic) modes. This allows us to calculate the distortion and the normalnormal correlators for the surface. The normalnormal 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}
}