2020/04/30 by Marzieh Peyravi, Nematollah Riazi, Francisco S. N. Lobo
Physics and Astronomy · #Black Holes and Theoretical Physics #Brane #Brane cosmology #Cosmology and Gravitation Theories #Degenerate energy levels #Noncommutative and Quantum Gravity Theories #Scalar (mathematics) #Spontaneous symmetry breaking #Symmetry (geometry) #Symmetry breaking #Tensor (intrinsic definition) #Warp drive #astro-ph.HE #gr-qc #hep-th
paper · pdf · doi:10.1140/epjc/s10052-021-08988-y
published as Eur. Phys. J. C 81, 216 (2021) · 14 pages, 9 figures. Comments welcome. V2: discussion and references added. Version to appear in Eur.Phys.J.C
openalex created_date 2020/04/17 · arxiv created 2021/02/19 · openalex publication_date 2021/03/01 · arxiv updated 2021/03/08 · openalex updated_date 2026/08/05
Abstract In this work, using two scalar fields ( φ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>ϕ</mml:mi> </mml:math> , ψ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>ψ</mml:mi> </mml:math> ) coupled to 4 + 1 dimensional gravity, we construct novel topological brane solutions through an explicit U (1) symmetry breaking term. The potential of this model is constructed so that two distinct degenerate vacua in the φ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>ϕ</mml:mi> </mml:math> field exist, in analogy to the φ 4 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msup> <mml:mi>ϕ</mml:mi> <mml:mn>4</mml:mn> </mml:msup> </mml:math> potential. Therefore, brane solutions appear due to the vacuum structure of the φ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>ϕ</mml:mi> </mml:math> field. However, the topology and vacuum structure in the ψ <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mi>ψ</mml:mi> </mml:math> direction depends on the symmetry breaking parameter β 2 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msup> <mml:mi>β</mml:mi> <mml:mn>2</mml:mn> </mml:msup> </mml:math> , which leads to different types of branes. As a result, one can interpret the present model as a combination of a φ 4 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msup> <mml:mi>ϕ</mml:mi> <mml:mn>4</mml:mn> </mml:msup> </mml:math> brane with an auxiliary field, which leads to deviations from the φ 4 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msup> <mml:mi>ϕ</mml:mi> <mml:mn>4</mml:mn> </mml:msup> </mml:math> system with the brane achieving a richer internal structure. Furthermore, we analyse in detail the behaviour of the superpotentials, the warp factors, the Ricci and Kretschmann scalars and the Einstein tensor components. In addition to this, we explore the stability of the brane in terms of the free parameters of the model. The analysis presented here complements previous work and is sufficiently novel to be interesting.