scholarly journals BRANE-WORLD COSMOLOGY AND VARYING G

2010 ◽  
Vol 25 (18n19) ◽  
pp. 3835-3856 ◽  
Author(s):  
LEONARDO AMARILLA ◽  
HÉCTOR VUCETICH
Keyword(s):  
Scalar Field ◽  
Cosmological Model ◽  
Time Variation ◽  
Brane World ◽  
Brane Tension ◽  
Bulk Scalar Field

We consider a brane-world cosmological model coupled to a bulk scalar field. Since the brane tension turns out to be proportional to Newton's coupling G, in such a model a time variation of G naturally occurs. By resorting to available bounds on the variation of G, the parameters of the model are constrained. The constraints coming from nucleosynthesis and CMB result to be the severest ones.

scholarly journals Vacuum Expectation Value Profiles of the Bulk Scalar Field in the Generalized Randall-Sundrum Model

2015 ◽  
Vol 2015 ◽  
pp. 1-10
Author(s):  
A. Tofighi ◽  
M. Moazzen ◽  
A. Farokhtabar
Keyword(s):  
Scalar Field ◽  
Boundary Conditions ◽  
Cosmological Constant ◽  
Vacuum Expectation ◽  
Vacuum Expectation Value ◽  
Brane World ◽  
Dirichlet Boundary Conditions ◽  
World Model ◽  
Expectation Value ◽  
Bulk Scalar Field

In the generalized Randall-Sundrum warped brane-world model the cosmological constant induced on the visible brane can be positive or negative. In this paper we investigate profiles of vacuum expectation value of the bulk scalar field under general Dirichlet and Neumann boundary conditions in the generalized warped brane-world model. We show that the VEV profiles generally depend on the value of the brane cosmological constant. We find that the VEV profiles of the bulk scalar field for a visible brane with negative cosmological constant and positive tension are quite distinct from those of Randall-Sundrum model. In addition we show that the VEV profiles for a visible brane with large positive cosmological constant are also different from those of the Randall-Sundrum model. We also verify that Goldberger and Wise mechanism can work under nonzero Dirichlet boundary conditions in the generalized Randall-Sundrum model.

scholarly journals Creation of a brane world with a bulk scalar field

2006 ◽  
Vol 31 ◽  
pp. 219-220
Author(s):  
Koh-suke Aoyanagi ◽  
Kei-ichi Maeda
Keyword(s):  
Scalar Field ◽  
Brane World ◽  
Bulk Scalar Field

scholarly journals Creation of a brane world with a bulk scalar field

2006 ◽  
Vol 2006 (03) ◽  
pp. 012-012 ◽  
Author(s):  
Koh-suke Aoyanagi ◽  
Kei-ichi Maeda
Keyword(s):  
Scalar Field ◽  
Brane World ◽  
Bulk Scalar Field

scholarly journals BRANE WORLD IN A TOPOLOGICAL BLACK HOLES IN ASYMPTOTICALLY FLAT SPACE–TIME

2001 ◽  
Vol 16 (26) ◽  
pp. 1703-1710 ◽  
Author(s):  
DONAM YOUM
Keyword(s):  
Black Holes ◽  
Black Hole ◽  
Scalar Field ◽  
Flat Space ◽  
Space Time ◽  
Brane World ◽  
Black Hole Horizon ◽  
World Model ◽  
Asymptotically Flat ◽  
Bulk Scalar Field

We study static brane configurations in the bulk background of the topological black holes in asymptotically flat space–time and find that such configurations are possible even for flat black hole horizon, unlike the AdS black hole case. We construct the brane world model with an orbifold structure S1/Z2 in such bulk background and study massless bulk scalar field.

scholarly journals SELF-TUNING DARK ENERGY IN BRANE WORLD COSMOLOGY

2001 ◽  
Vol 16 (17) ◽  
pp. 1089-1099 ◽  
Author(s):  
KUNIHITO UZAWA ◽  
JIRO SODA
Keyword(s):  
Dark Energy ◽  
Scalar Field ◽  
Vacuum Energy ◽  
Friedmann Equation ◽  
Brane World ◽  
Tuning Mechanism ◽  
Enormous Amount ◽  
Self Tuning ◽  
Bulk Scalar Field

In this letter, the self-tuning mechanism of dark energy is proposed by considering the cosmological matter in the brane world. In the first part of this letter, the effective four-dimensional Friedmann equation in the presence of the bulk scalar field is derived. In our model, the bulk scalar field takes the role of the dark energy and its value is slowly varying in time. The claim is that, even if the enormous amount of vacuum energy exists on the brane, the present value of the dark energy is self-tuned to be consistent with the current observations. This result will open the possibility to discuss the dark energy in the brane world in the context of the anthropic principle or quantum cosmology.

scholarly journals CHAOTIC INFLATION ON THE RANDALL–SUNDRUM TWO-BRANE MODEL

2010 ◽  
Vol 25 (31) ◽  
pp. 2697-2713
Author(s):  
KOUROSH NOZARI ◽  
SIAMAK AKHSHABI
Keyword(s):  
Scalar Field ◽  
Field Potential ◽  
Friedmann Equation ◽  
Warp Factor ◽  
Model Parameters ◽  
Stabilization Mechanism ◽  
Brane Model ◽  
Inflation Model ◽  
Bulk Scalar Field ◽  
Chaotic Inflation

We construct an inflation model on the Randall–Sundrum I (RSI) brane where a bulk scalar field stabilizes the inter-brane separation. We study impact of the bulk scalar field on the inflationary dynamics on the brane. We proceed in two different approaches: in the first approach, the stabilizing field potential is directly appeared in the Friedmann equation and the resulting scenario is effectively a two-field inflation. In the second approach, the stabilization mechanism is considered in the context of a warp factor so that there is just one field present that plays the roles of both inflaton and stabilizer. We study constraints imposed on the model parameters from recent observations.

scholarly journals Dressing bulk fields in AdS3

2020 ◽  
Vol 2020 (10) ◽  
Author(s):  
Daniel Kabat ◽  
Gilad Lifschytz
Keyword(s):  
Scalar Field ◽  
Wilson Line ◽  
Bulk Scalar Field

Abstract We study a set of CFT operators suitable for reconstructing a charged bulk scalar field ϕ in AdS3 (dual to an operator $$ \mathcal{O} $$ O of dimension ∆ in the CFT) in the presence of a conserved spin-n current in the CFT. One has to sum a tower of smeared non-primary scalars $$ {\partial}_{+}^m{J}^{(m)} $$ ∂ + m J m , where J(m) are primaries with twist ∆ and spin m built from $$ \mathcal{O} $$ O and the current. The coefficients of these operators can be fixed by demanding that bulk correlators are well-defined: with a simple ansatz this requirement allows us to calculate bulk correlators directly from the CFT. They are built from specific polynomials of the kinematic invariants up to a freedom to make field redefinitions. To order 1/N this procedure captures the dressing of the bulk scalar field by a radial generalized Wilson line.

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