1,465 research outputs found
Reconstruction of general scalar-field dark energy models
The reconstruction of scalar-field dark energy models is studied for a
general Lagrangian density , where is a kinematic term of a
scalar field . We implement the coupling between dark energy and dark
matter and express reconstruction equations using two observables: the Hubble
parameter and the matter density perturbation . This allows us to
determine the structure of corresponding theoretical Lagrangian together with
the coupling from observations. We apply our formula to several forms of
Lagrangian and present concrete examples of reconstruction by using the recent
Gold dataset of supernovae measurements. This analysis includes a generalized
ghost condensate model as a way to cross a cosmological-constant boundary even
for a single-field case.Comment: 8 pages, 2 figure
Evolution of perturbations in distinct classes of canonical scalar field models of dark energy
Dark energy must cluster in order to be consistent with the equivalence
principle. The background evolution can be effectively modelled by either a
scalar field or by a barotropic fluid.The fluid model can be used to emulate
perturbations in a scalar field model of dark energy, though this model breaks
down at large scales. In this paper we study evolution of dark energy
perturbations in canonical scalar field models: the classes of thawing and
freezing models.The dark energy equation of state evolves differently in these
classes.In freezing models, the equation of state deviates from that of a
cosmological constant at early times.For thawing models, the dark energy
equation of state remains near that of the cosmological constant at early times
and begins to deviate from it only at late times.Since the dark energy equation
of state evolves differently in these classes,the dark energy perturbations too
evolve differently. In freezing models, since the equation of state deviates
from that of a cosmological constant at early times, there is a significant
difference in evolution of matter perturbations from those in the cosmological
constant model.In comparison, matter perturbations in thawing models differ
from the cosmological constant only at late times. This difference provides an
additional handle to distinguish between these classes of models and this
difference should manifest itself in the ISW effect.Comment: 11 pages, 6 figures, accepted for publication in Phys. Rev.
APSIS - an Artificial Planetary System in Space to probe extra-dimensional gravity and MOND
A proposal is made to test Newton's inverse-square law using the perihelion
shift of test masses (planets) in free fall within a spacecraft located at the
Earth-Sun L2 point. Such an Artificial Planetary System In Space (APSIS) will
operate in a drag-free environment with controlled experimental conditions and
minimal interference from terrestrial sources of contamination. We demonstrate
that such a space experiment can probe the presence of a "hidden" fifth
dimension on the scale of a micron, if the perihelion shift of a "planet" can
be measured to sub-arc-second accuracy. Some suggestions for spacecraft design
are made.Comment: 17 pages, revtex, references added. To appear in Special issue of
IJMP
Scalar Field Dark Energy Perturbations and their Scale Dependence
We estimate the amplitude of perturbation in dark energy at different length
scales for a quintessence model with an exponential potential. It is shown that
on length scales much smaller than hubble radius, perturbation in dark energy
is negligible in comparison to that in in dark matter. However, on scales
comparable to the hubble radius () the
perturbation in dark energy in general cannot be neglected. As compared to the
CDM model, large scale matter power spectrum is suppressed in a
generic quintessence dark energy model. We show that on scales , this suppression is primarily due to different background
evolution compared to CDM model. However, on much larger scales
perturbation in dark energy can effect matter power spectrum significantly.
Hence this analysis can act as a discriminator between CDM model and
other generic dark energy models with .Comment: 12 pages, 13 figures, added new section, accepted for publication in
Phys. Rev.
Quantum effects, soft singularities and the fate of the universe in a braneworld cosmology
We examine a class of braneworld models in which the expanding universe
encounters a "quiescent" future singularity. At a quiescent singularity, the
energy density and pressure of the cosmic fluid as well as the Hubble parameter
remain finite while all derivatives of the Hubble parameter diverge (i.e.,
, , etc. ). Since the Kretschmann invariant
diverges () at the singularity, one expects
quantum effects to play an important role as the quiescent singularity is
approached. We explore the effects of vacuum polarization due to massless
conformally coupled fields near the singularity and show that these can either
cause the universe to recollapse or, else, lead to a softer singularity at
which , , and remain finite while {\dddot H} and
higher derivatives of the Hubble parameter diverge. An important aspect of the
quiescent singularity is that it is encountered in regions of low density,
which has obvious implications for a universe consisting of a cosmic web of
high and low density regions -- superclusters and voids. In addition to vacuum
polarization, the effects of quantum particle production of non-conformal
fields are also likely to be important. A preliminary examination shows that
intense particle production can lead to an accelerating universe whose Hubble
parameter shows oscillations about a constant value.Comment: 19 pages, 3 figures, text slightly improved and references added.
Accepted for publication in Classical and Quantum Gravit
Structure formation on the brane: A mimicry
We show how braneworld cosmology with bulk matter can explain structure
formation. In this scenario, the nonlocal corrections to the Friedmann
equations supply a Weyl fluid that can dominate over matter at late times due
to the energy exchange between the brane and the bulk. We demonstrate that the
presence of the Weyl fluid radically changes the perturbation equations, which
can take care of the fluctuations required to account for the large amount of
inhomogeneities observed in the local universe. Further, we show how this Weyl
fluid can mimic dark matter. We also investigate the bulk geometry responsible
for the scenario.Comment: 7 pages. Matches published versio
Curvature driven acceleration : a utopia or a reality ?
The present work shows that a combination of nonlinear contribution from the
Ricci curvature in Einstein field equations can drive a late time acceleration
of expansion of the universe. The transit from the decelerated to the
accelerated phase of expansion takes place smoothly without having to resort to
a study of asymptotic behaviour. This result emphasizes the need for thorough
and critical examination of models with nonlinear contribution from the
curvature.Comment: 8 pages, 4 figure
Gravitational instability on the brane: the role of boundary conditions
An outstanding issue in braneworld theory concerns the setting up of proper
boundary conditions for the brane-bulk system. Boundary conditions (BC's)
employing regulatory branes or demanding that the bulk metric be nonsingular
have yet to be implemented in full generality. In this paper, we take a
different route and specify boundary conditions directly on the brane thereby
arriving at a local and closed system of equations (on the brane). We consider
a one-parameter family of boundary conditions involving the anisotropic stress
of the projection of the bulk Weyl tensor on the brane and derive an exact
system of equations describing scalar cosmological perturbations on a generic
braneworld with induced gravity. Depending upon our choice of boundary
conditions, perturbations on the brane either grow moderately (region of
stability) or rapidly (instability). In the instability region, the evolution
of perturbations usually depends upon the scale: small scale perturbations grow
much more rapidly than those on larger scales. This instability is caused by a
peculiar gravitational interaction between dark radiation and matter on the
brane. Generalizing the boundary conditions obtained by Koyama and Maartens, we
find for the Dvali-Gabadadze-Porrati model an instability, which leads to a
dramatic scale-dependence of the evolution of density perturbations in matter
and dark radiation. A different set of BC's, however, leads to a more moderate
and scale-independent growth of perturbations. For the mimicry braneworld,
which expands like LCDM, this class of BC's can lead to an earlier epoch of
structure formation.Comment: 35 pages, 9 figures, an appendix and references added, version to be
published in Classical and Quantum Gravit
Complementary Constraints on Brane Cosmology
The acceleration of the expansion of the universe represents one of the major
challenges to our current understanding of fundamental physics. In principle,
to explain this phenomenon, at least two different routes may be followed:
either adjusting the energy content of the Universe -- by introducing a
negative-pressure dark energy -- or modifying gravity at very large scales --
by introducing new spatial dimensions, an idea also required by unification
theories. In the cosmological context, the role of such extra dimensions as the
source of the dark pressure responsable for the acceleration of our Universe is
translated into the so-called brane world (BW) cosmologies. Here we study
complementary constraints on a particular class of BW scenarios in which the
modification of gravity arises due to a gravitational \emph{leakage} into extra
dimensions. To this end, we use the most recent Chandra measurements of the
X-ray gas mass fraction in galaxy clusters, the WMAP determinations of the
baryon density parameter, measurements of the Hubble parameter from the
\emph{HST}, and the current supernova data. In agreement with other recent
results, it is shown that these models provide a good description for these
complementary data, although a closed scenario is always favored in the joint
analysis. We emphasize that observational tests of BW scenarios constitute a
natural verification of the role of possible extra dimensions in both
fundamental physics and cosmology.Comment: 6 Pages, 4 Figures, LaTe
Positron and positronium affinities in the work-formalism Hartree-Fock approximation
Positron binding to anions is investigated within the work formalism proposed
by Harbola and Sahni for the halide anions and the systems Li^- through O^-
excluding Be^- and N^-. The toal ground-state energies of the anion-positron
bound systems are empirically found to be an upper bound to the Hartree-Fock
energies. The computed expectation values as well as positron and positronium
affinities are in good agreement with their restricted Hartree-Fock
counterparts. Binding of a positron to neutral species is also investigated
using an iterative method.Comment: 12 pages, to appear in Physical Review
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