\(S\)-brane to thermal non-singular string cosmology
type: Item
instance of: scholarly article
zbMATH Open document ID: 1247.83279
DOI: 10.1088/0264-9381/29/9/095014
author: Nicolaos Toumbas
author: Costas Kounnas
author: Hervé Partouche
published in: Classical and Quantum Gravity
publication date: 2012-06-18T00:00:00Z
full work available at URL: https://arxiv.org/abs/1111.5816
Mathematics Subject Classification ID: 83F05
Mathematics Subject Classification ID: 83C75
Mathematics Subject Classification ID: 83E30
Mathematics Subject Classification ID: 81T30
Mathematics Subject Classification ID: 83E15
zbMATH DE Number: 6047195
zbMATH Keywords: relativistic cosmology
zbMATH Keywords: string cosmologies
zbMATH Keywords: Sigma-models
zbMATH Keywords: radiative universe
zbMATH Keywords: bouncing universes
zbMATH Keywords: dilatons
zbMATH Keywords: phase transitions
zbMATH Keywords: Hagedorn transition
zbMATH Keywords: branes
MaRDI profile type: Publication
OpenAlex ID: W2001728939
arXiv ID: 1111.5816
title: \(S\)-brane to thermal non-singular string cosmology
review text: The authors present a new class of non-singular string cosmologies in \(d\) spacetime dimensions. At very early times, the Universe is described by a flat sigma-model metric, a constant maximal temperature \(T_c\) and super-weak string interactions. During the evolution, the metric remains flat up to times comparable with the critical time, while the string coupling grows and reaches a critical value. This phase is characterized by a uniform temporal distribution of spacelike branes. At later times (times larger than the critical one), the Universe enters a new phase of expansion, with radiation. The string coupling decreases due to the dilaton motion and asymptotes to a constant for times much larger than the critical time. Throughout the evolution, the string coupling remains smaller than the coupling constant. In the Einstein frame, the cosmologies describe bouncing Universes, where two distinct phases are connected at the critical time. In the initial contracting phase, the evolution of the scale factor is identical to that of a negatively curved Universe filled with radiation. At later times, the Universe enters an expanding thermal phase with a running dilaton. Explicit examples are presented in a large class of thermal (4,0) type II superstring vacua, with non-trivial `gravito-magnetic' fluxes.
reviewed by: Alex B. Gaina
description: scientific article; zbMATH DE number 6047195