40 research outputs found
A symmetry for vanishing cosmological constant
Two different realizations of a symmetry principle that impose a zero
cosmological constant in an extra-dimensional set-up are studied. The symmetry
is identified by multiplication of the metric by minus one. In the first
realization of the symmetry this is provided by a symmetry transformation that
multiplies the coordinates by the imaginary number i. In the second realization
this is accomplished by a symmetry transformation that multiplies the metric
tensor by minus one. In both realizations of the symmetry the requirement of
the invariance of the gravitational action under the symmetry selects out the
dimensions given by D = 2(2n+1), n=0,1,2,... and forbids a bulk cosmological
constant. Another attractive aspect of the symmetry is that it seems to be more
promising for quantization when compared to the usual scale symmetry. The
second realization of the symmetry is more attractive in that it is posible to
make a possible brane cosmological constant zero in a simple way by using the
same symmetry, and the symmetry may be identified by reflection symmetry in
extra dimensions.Comment: Talk in the conference IRGAC 2006, 2nd International Conference on
Quantum Theories and Renormalization Group in Gravity and Cosmology,
Barcelon
What is there in the black box of dark energy: variable cosmological parameters or multiple (interacting) components?
The coincidence problems and other dynamical features of dark energy are
studied in cosmological models with variable cosmological parameters and in
models with the composite dark energy. It is found that many of the problems
usually considered to be cosmological coincidences can be explained or
significantly alleviated in the aforementioned models.Comment: 6 pages, 1 figure, talk given at IRGAC2006 (Barcelona, July 11-15,
2006), to appear in J. Phys.
What is needed of a tachyon if it is to be the dark energy?
We study a dark energy scenario in the presence of a tachyon field
with potential and a barotropic perfect fluid. The cosmological
dynamics crucially depends on the asymptotic behavior of the quantity
. If is a constant, which corresponds to
an inverse square potential , there exists one
stable critical point that gives an acceleration of the universe at late times.
When asymptotically, we can have a viable dark energy scenario
in which the system approaches an ``instantaneous'' critical point that
dynamically changes with . If approaches infinity
asymptotically, the universe does not exhibit an acceleration at late times. In
this case, however, we find an interesting possibility that a transient
acceleration occurs in a regime where is smaller than of order
unity.Comment: 11 pages and 3 figures, minor clarifications added; final version to
appear in PR
String-inspired cosmology: Late time transition from scaling matter era to dark energy universe caused by a Gauss-Bonnet coupling
The Gauss-Bonnet (GB) curvature invariant coupled to a scalar field
can lead to an exit from a scaling matter-dominated epoch to a late-time
accelerated expansion, which is attractive to alleviate the coincident problem
of dark energy. We derive the condition for the existence of cosmological
scaling solutions in the presence of the GB coupling for a general scalar-field
Lagrangian density , where is a kinematic
term of the scalar field. The GB coupling and the Lagrangian density are
restricted to be in the form and , respectively, where is a constant and is an
arbitrary function. We also derive fixed points for such a scaling Lagrangian
with a GB coupling and clarify the conditions
under which the scaling matter era is followed by a de-Sitter solution which
can appear in the presence of the GB coupling. Among scaling models proposed in
the current literature, we find that the models which allow such a cosmological
evolution are an ordinary scalar field with an exponential potential and a
tachyon field with an inverse square potential, although the latter requires a
coupling between dark energy and dark matter.Comment: 18 pages, 4 figures, version to appear in JCA
Scaling solutions and geodesics in moduli space
In this paper we consider cosmological scaling solutions in general
relativity coupled to scalar fields with a non-trivial moduli space metric. We
discover that the scaling property of the cosmology is synonymous with the
scalar fields tracing out a particular class of geodesics in moduli space -
those which are constructed as integral curves of the gradient of the log of
the potential. Given a generic scalar potential we explicitly construct a
moduli metric that allows scaling solutions, and we show the converse - how one
can construct a potential that allows scaling once the moduli metric is known.Comment: 10 pages, 3 figure
Accelerated expansion of a universe containing a self-interacting Bose-Einstein gas
Acceleration of the universe is obtained from a model of non-relativistic
particles with a short-range attractive interaction, at low enough temperature
to produce a Bose-Einstein condensate. Conditions are derived for
negative-pressure behavior. In particular, we show that a phantom-accelerated
regime at the beginning of the universe solves the horizon problem,
consistently with nucleosynthesis.Comment: 18 pages, 4 figure
DGP Cosmology with a Non-Minimally Coupled Scalar Field on the Brane
We construct a DGP inspired braneworld scenario where a scalar field
non-minimally coupled to the induced Ricci curvature is present on the brane.
First we investigate the status of gravitational potential with non-minimal
coupling and observational constraints on this non-minimal model. Then we
further deepen the idea of embedding of FRW cosmology in this non-minimal
setup. Cosmological implications of this scenario are examined with details and
the quintessence and late-time expansion of the universe within this framework
are examined. Some observational constraints imposed on this non-minimal
scenario are studied and relation of this model with dark radiation formalism
is determined with details.Comment: 26 pages, 3 eps figure
On compatibility of string effective action with an accelerating universe
In this paper, we fully investigate the cosmological effects of the moduli
dependent one-loop corrections to the gravitational couplings of the string
effective action to explain the cosmic acceleration problem in early (and/or
late) universe. These corrections comprise a Gauss-Bonnet (GB) invariant
multiplied by universal non-trivial functions of the common modulus
and the dilaton . The model exhibits several features of cosmological
interest, including the transition between deceleration and acceleration
phases. By considering some phenomenologically motivated ansatzs for one of the
scalars and/or the scale factor (of the universe), we also construct a number
of interesting inflationary potentials. In all examples under consideration, we
find that the model leads only to a standard inflation () when the
numerical coefficient associated with modulus-GB coupling is positive,
while the model can lead also to a non-standard inflation (), if
is negative. In the absence of (or trivial) coupling between the GB term and
the scalars, there is no crossing between the phases, while
this is possible with non-trivial GB couplings, even for constant dilaton phase
of the standard picture. Within our model, after a sufficient amount of e-folds
of expansion, the rolling of both fields and can be small. In
turn, any possible violation of equivalence principle or deviations from the
standard general relativity may be small enough to easily satisfy all
astrophysical and cosmological constraints.Comment: 30 pages, 8 figures; v2 significant changes in notations, appendix
and refs added; v3 significant revisions, refs added; v4 appendix extended,
new refs, published versio
Determination of the UV cut-off from the observed value of the Universe acceleration
It is shown that using of the equation of motion of the Universe scale factor
allows calculation of the contribution of the vacuum fluctuations to the
acceleration of the Universe expansion. Renormalization of the equation is
needed only in the case of massive particles. Under a known number of the
different kinds of fundamental fields, this provides determination of momentum
of the ultraviolet cut-off from the observed value of acceleration.Comment: 10 pages, 1 figur
Brane Cosmology with a Non-Minimally Coupled Bulk-Scalar Field
We consider the cosmological evolution of a brane in the presence of a bulk
scalar field coupled to the Ricci scalar through a term f(\phi)R. We derive the
generalized Friedmann equation on the brane in the presence of arbitrary brane
and bulk-matter, as well as the scalar field equation, allowing for a general
scalar potential V(phi). We focus on a quadratic form of the above non-minimal
coupling and obtain a class of late-time solutions for the scale factor and the
scalar field on the brane that exhibit accelerated expansion for a range of the
non-minimal coupling parameter.Comment: 15 page