Cosmological evolution of a purely conical codimension-2 brane world

Papantonopoulos, E; Papazoglou, A

dc.contributor.author	Papantonopoulos, E	en
dc.contributor.author	Papazoglou, A	en
dc.date.accessioned	2014-03-01T01:22:02Z
dc.date.available	2014-03-01T01:22:02Z
dc.date.issued	2005	en
dc.identifier.issn	1126-6708	en
dc.identifier.uri	https://dspace.lib.ntua.gr/xmlui/handle/123456789/16451
dc.subject	Classical Theories of Gravity	en
dc.subject	Cosmology of Theories beyond the SM	en
dc.subject	Large Extra Dimensions	en
dc.subject	P-branes	en
dc.subject.classification	Physics, Particles & Fields	en
dc.subject.other	CONSTANT	en
dc.subject.other	SUPERGRAVITY	en
dc.subject.other	BULK	en
dc.title	Cosmological evolution of a purely conical codimension-2 brane world	en
heal.type	journalArticle	en
heal.identifier.primary	10.1088/1126-6708/2005/09/012	en
heal.identifier.secondary	http://dx.doi.org/10.1088/1126-6708/2005/09/012	en
heal.identifier.secondary	012	en
heal.language	English	en
heal.publicationDate	2005	en
heal.abstract	We study the cosmological evolution of isotropic matter on an infinitely thin conical codimension-two brane-world. Our analysis is based on the boundary dynamics of a six-dimensional model in the presence of an induced gravity term on the brane and a Gauss-Bonnet term in the bulk. With the assumption that the bulk contains only a cosmological constant Lambda(B), we find that the isotropic evolution of the brane-universe imposes a tuned relation between the energy density and the brane equation of state. The evolution of the system has fixed points (attractors), which correspond to a final state of radiation for Lambda(B) = 0 and to de Sitter state for Lambda(B) > 0. Furthermore, considering anisotropic matter on the brane, the tuning of the parameters is lifted, and new regions of the parametric space are available for the cosmological evolution of the brane-universe. The analysis of the dynamics of the system shows that, the isotropic fixed points remain attractors of the system, and for values of Lambda(B) which give acceptable cosmological evolution of the equation of state, the line of isotropic tuning is a very weak attractor. The initial conditions, in this case, need to be fine tuned to have an evolution with acceptably small anisotropy.	en
heal.publisher	INT SCHOOL ADVANCED STUDIES	en
heal.journalName	Journal of High Energy Physics	en
dc.identifier.doi	10.1088/1126-6708/2005/09/012	en
dc.identifier.isi	ISI:000232334600012	en
dc.identifier.issue	9	en
dc.identifier.spage	297	en
dc.identifier.epage	318	en