Cosmology of codimension-two braneworlds

Cline, James M.; Descheneau, Julie; Giovannini, Massimo; Vinet, Jérémie

doi:10.1088/1126-6708/2003/06/048

Cited by 158 publications

(205 citation statements)

References 45 publications

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“…T µ ν = {ρ, p, p, p}δ µ ν , then ρ and p must satisfy ρ + p = 0, i.e. it behaves like the brane tension [10]. This forbids us adding dust and radiation on the brane, thus it is cosmologically unrealistic.…”

Section: Secii)mentioning

confidence: 99%

Codimension two branes in Einstein-Gauss-Bonnet gravity

Wang¹,

Meng²

2005

Phys. Rev. D

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Codimension two branes play an interesting role in attacking the cosmological constant problem.Recently, in order to handle some problems in codimension two branes in Einstein gravity, Bostock et al. have proposed using six-dimensional Einstein-Gauss-Bonnet (EGB) gravity instead of sixdimensional Einstein gravity. In this paper, we present the solutions of codimension two branes in six-dimensional EGB gravity. We show that Einstein's equations take a "factorizable" form for a factorized metric tensor ansatz even in the presence of the higher-derivative Gauss-Bonnet term.Especially, a new feature of the solution is that the deficit angle depends on the brane geometry.We discuss the implication of the solution to the cosmological constant problem. We also comment on a possible problem of inflation model building on codimension two branes. *

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Section: Secii)mentioning

confidence: 99%

Codimension two branes in Einstein-Gauss-Bonnet gravity

Wang¹,

Meng²

2005

Phys. Rev. D

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“…Using the particular form of the coset representative described above, the following C-functions take a particularly simple form 20) where |φ| 2 ≡ tr φ † φ. These are the only components we need in order to construct the scalar potential.…”

Section: The Choice Of Lmentioning

confidence: 99%

Scalar potential and dyonic strings in 6D gauged supergravity

RANDJBARDAEMI

2004

Nuclear Physics B

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In this paper we first give a simple parametrization of the scalar coset manifold of the only known anomaly free chiral gauged supergravity in six dimensions in the absence of linear multiplets, namely gauged minimal supergravity coupled to a tensor multiplet, E 6 × E 7 × U (1) R Yang-Mills multiplets and suitable number of hypermultiplets. We then construct the potential for the scalars and show that it has a unique minimum at the origin. We also construct a new BPS dyonic string solution in which U (1) R × U (1) gauge fields, in addition to the metric, dilaton and the 2-form potential, assume nontrivial configurations in any U (1) R gauged 6D minimal supergravity coupled to a tensor multiplet with gauge symmetry G ⊇ U (1). The solution preserves 1/4 of the 6D supersymmetries and can be trivially embedded in the anomaly free model, in which case the U (1) activated in our solution resides in E 7 .

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“…Whilst Weinberg's no-go theorem makes self tuning impossible for constant field configurations, it does not rule out more general scenarios [31]. Indeed, co-dimension two braneworld models offer some hope for developing a successful self-tuning mechanism [20][21][22][23][24][25][26][27]. The reason is that adding vacuum energy to a co-dimension two brane merely alters the bulk deficit angle and not the brane geometry.…”

Section: Introductionmentioning

confidence: 99%

“…The reason is that adding vacuum energy to a co-dimension two brane merely alters the bulk deficit angle and not the brane geometry. Difficulties arise when one tries to study nontrivial branes geometries as this can sometimes introduce problems with singularities [24] and perturbative ghosts [32]. Furthermore, on a technical level, going beyond the vacua, even perturbatively, can be quite challenging in co-dimension two models.…”

Section: Introductionmentioning

confidence: 99%

Bi-galileon theory II: phenomenology

Padilla

Saffin

Zhou

2011

J. High Energ. Phys.

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We continue to introduce bi-galileon theory, the generalisation of the single galileon model introduced by Nicolis et al. The theory contains two coupled scalar fields and is described by a Lagrangian that is invariant under Galilean shifts in those fields. This paper is the second of two, and focuses on the phenomenology of the theory. We are particularly interesting in models that admit solutions that are asymptotically self accelerating or asymptotically self tuning. In contrast to the single galileon theories, we find examples of self accelerating models that are simultaneously free from ghosts, tachyons and tadpoles, able to pass solar system constraints through Vainshtein screening, and do not suffer from problems with superluminality, Cerenkov emission or strong coupling. We also find self tuning models and discuss how Weinberg's no go theorem is evaded by breaking Poincaré invariance in the scalar sector. Whereas the galileon description is valid all the way down to solar system scales for the self-accelerating models, unfortunately the same cannot be said for self tuning models owing to the scalars backreacting strongly on to the geometry.

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Cosmology of codimension-two braneworlds

Cited by 158 publications

References 45 publications

Codimension two branes in Einstein-Gauss-Bonnet gravity

Codimension two branes in Einstein-Gauss-Bonnet gravity

Scalar potential and dyonic strings in 6D gauged supergravity

Bi-galileon theory II: phenomenology

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