27 research outputs found
DGP specteroscopy
We systematically explore the spectrum of gravitational perturbations in codimension-1 DGP braneworlds, and find a 4D ghost on the self-accelerating branch of solutions. The ghost appears for any value of the brane tension, although depending on the sign of the tension it is either the helicity-0 component of the lightest localized massive tensor of mass
Synergistic Gravity and the Role of Resonances in GRS-Inspired Braneworlds
We consider 5D braneworld models of quasi-localized gravity in which 4D
gravity is reproduced at intermediate scales while the extra dimension opens up
at both the very short and the very long distances, where the geometry is flat.
Our main interest is the interplay between the zero mode of these models,
whenever a normalizable zero mode exists, and the effects of zero energy
graviton resonant modes coming from the contributions of massive KK modes. We
first consider a compactified version of the GRS model and find that
quasi-localized gravity is characterized by a scale for which both the
resonance and the zero mode have significant contribution to 4D gravity. Above
this scale, gravity is primarily mediated by the zero mode, while the resonance
gives only minor corrections. Next, we consider an asymmetric version of the
standard non-compact GRS model, characterized by different cosmological
constants on each AdS side. We show that a resonance is present but the
asymmetry, through the form of the localizing potential, can weaken it,
resulting in a shorter lifetime and, thus, in a shorter distance scale for 4D
gravity. As a third model exhibiting quasi-localization, we consider a version
of the GRS model in which the central positive tension brane has been replaced
by a configuration of a scalar field propagating in the bulk.Comment: 18 pages, 3 figures, added 1 figure, revised version as published in
Class. Quant. Gra
Ghosts in asymmetric brane gravity and the decoupled stealth limit
We study the spectrum of gravitational perturbations around a vacuum de
Sitter brane in a 5D asymmetric braneworld model, with induced curvature on the
brane. This generalises the stealth acceleration model proposed by Charmousis,
Gregory and Padilla (CGP) which realises the Cardassian cosmology in which
power law cosmic acceleration can be driven by ordinary matter. Whenever the
bulk has infinite volume we find that there is always a perturbative ghost
propagating on the de Sitter brane, in contrast to the Minkowski brane case
analysed by CGP. We discuss the implication of this ghost for the stealth
acceleration model, and identify a limiting case where the ghost decouples as
the de Sitter curvature vanishes.Comment: 21 page
Stealth Acceleration and Modified Gravity
We show how to construct consistent braneworld models which exhibit late time
acceleration. Unlike self-acceleration, which has a de Sitter vacuum state, our
models have the standard Minkowski vacuum and accelerate only in the presence
of matter, which we dub ``stealth-acceleration''. We use an effective action
for the brane which includes an induced gravity term, and allow for an
asymmetric set-up. We study the linear stability of flat brane vacua and find
the regions of parameter space where the set-up is stable. The 4-dimensional
graviton is only quasi-localised in this set-up and as a result gravity is
modified at late times. One of the two regions is strongly coupled and the
scalar mode is eaten up by an extra symmetry that arises in this limit. Having
filtered the well-defined theories we then focus on their cosmology. When the
graviton is quasi-localised we find two main examples of acceleration. In each
case, we provide an illustrative model and compare it to LambdaCDM.Comment: 32 pages, 5 figure
Gauss-Bonnet brane-world cosmology without -symmetry
We consider a single 3-brane situated between two bulk spacetimes that posses
the same cosmological constant, but whose metrics do not posses a
-symmetry. On each side of the brane, the bulk is a solution to
Gauss-Bonnet gravity. This asymmetry modifies junction conditions, and so new
terms arise in the Friedmann equation. If these terms become dominant, these
behave cosmological constant at early times for some case, and might remove the
initial singularity for other case. However, we show that these new terms can
not become dominant ones under usual conditions when our brane is outside an
event horizon. We also show that any brane-world scenarios of this type revert
to a -symmetric form at late times, and hence rule out certain proposed
scenarios.Comment: 8 pages, 3 figures; Minor typos corrected. References added. V3:
Numerical errors are corrected. Fig.1 and Fig.3 are replaced. V4: published
versio
A short review of "DGP Specteroscopy"
In this paper we provide a short review of the main results developed in
hep-th/0604086. We focus on linearised vacuum perturbations about the
self-accelerating branch of solutions in the DGP model. These are shown to
contain a ghost in the spectrum for any value of the brane tension. We also
comment on hep-th/0607099, where some counter arguments have been presented.Comment: Minor typos correcte
Cosmic acceleration from asymmetric branes
We consider a single 3-brane sitting in between two different five
dimensional spacetimes. On each side of the brane, the bulk is a solution to
Gauss-Bonnet gravity, although the bare cosmological constant, funda mental
Planck scale, and Gauss-Bonnet coupling can differ. This asymmetry leads to
weighted junction conditions across the brane and interesting brane cosmology.
We focus on two special cases: a generalized Randall-Sundrum model without any
Gauss-Bonnet terms, and a stringy model, without any bare cosmological
constants, and positive Gauss-Bonnet coupling. Even though we assume there is
no vacuum energy on the brane, we find late time de Sitter cosmologies can
occur. Remarkably, in certain parameter regions, this acceleration is preceded
by a period of matter/radiation domination, with , all the
way back to nucleosynthesis.Comment: Version appearing in CQ
Lessons from the decoupling limit of Horava gravity
We consider the so-called "healthy" extension of Horava gravity in the limit
where the Stuckelberg field decouples from the graviton. We verify the alleged
strong coupling problem in this limit, under the assumption that no large
dimensionless parameters are put in by hand. This follows from the fact that
the dispersion relation for the Stuckelberg field does not have the desired z =
3 anisotropic scaling in the UV. To get the desired scaling and avoid strong
coupling one has to introduce a low scale of Lorentz violation and retain some
coupling between the graviton and the Stuckelberg field. We also make use of
the foliation preserving symmetry to show how the Stuckelberg field couples to
some violation of energy conservation. We source the Stuckelberg field using a
point particle with a slowly varying mass and show that two such particles feel
a constant attractive force. In this particular example, we see no Vainshtein
effect, and violations of the Equivalence Principle. The latter is probably
generic to other types of source and could potentially be used to place lower
bounds on the scale of Lorentz violation.Comment: 18 pages, 1 figure. Version to appear in JHEP. Conclusions with
respect to strong coupling modified - our strong coupling analysis does not
apply to a low scale of Lorentz violation. Expanded Equivalence Principle
violation discussion, noting it presents a challenge to low scale Lorentz
violation, exactly the scenario designed to cure strong coupling. Other minor
corrections and references adde
Galileon Hairs of Dyson Spheres, Vainshtein's Coiffure and Hirsute Bubbles
We study the fields of spherically symmetric thin shell sources, a.k.a. Dyson
spheres, in a {\it fully nonlinear covariant} theory of gravity with the
simplest galileon field. We integrate exactly all the field equations once,
reducing them to first order nonlinear equations. For the simplest galileon,
static solutions come on {\it six} distinct branches. On one, a Dyson sphere
surrounds itself with a galileon hair, which far away looks like a hair of any
Brans-Dicke field. The hair changes below the Vainshtein scale, where the extra
galileon terms dominate the minimal gradients of the field. Their hair looks
more like a fuzz, because the galileon terms are suppressed by the derivative
of the volume determinant. It shuts off the `hair bunching' over the `angular'
2-sphere. Hence the fuzz remains dilute even close to the source. This is
really why the Vainshtein's suppression of the modifications of gravity works
close to the source. On the other five branches, the static solutions are all
{\it singular} far from the source, and shuttered off from asymptotic infinity.
One of them, however, is really the self-accelerating branch, and the
singularity is removed by turning on time dependence. We give examples of
regulated solutions, where the Dyson sphere explodes outward, and its
self-accelerating side is nonsingular. These constructions may open channels
for nonperturbative transitions between branches, which need to be addressed
further to determine phenomenological viability of multi-branch gravities.Comment: 29+1 pages, LaTeX, 2 .pdf figure
Bi-galileon theory II: phenomenology
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 Poincar\'e 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