33,312 research outputs found
Weak gravity conjecture constraints on inflation
We consider the gravitational correction to the coupling of the scalar
fields. Weak gravity conjecture says that the gravitational correction to the
running of scalar coupling should be less than the contribution from scalar
fields. For instance, a new scale sets a UV cutoff
on the validity of the effective theory. Furthermore, this
conjecture implies a possible constraint on the inflation model, e.g. the
chaotic inflation model might be in the swampland.Comment: 11 pages, 3 figs; monor corrections; some clarifying remarks added
and the final version for publication in JHE
Interacting non-minimally coupled canonical, phantom and quintom models of holographic dark energy in non-flat universe
Motivated by our recent work \cite{set1}, we generalize this work to the
interacting non-flat case. Therefore in this paper we deal with canonical,
phantom and quintom models, with the various fields being non-minimally coupled
to gravity, within the framework of interacting holographic dark energy. We
employ the holographic model of interacting dark energy to obtain the equation
of state for the holographic energy density in non-flat (closed) universe
enclosed by the event horizon measured from the sphere of horizon named .Comment: 18 pages, 3 figures. Accepted for publication in IJMPD (2010
An Implication of "Gravity as the Weakest Force"
The negative specific heat of a radiating black hole is indicative of a
cataclysmic endpoint to the evaporation process. In this letter, we suggest a
simple mechanism for circumventing such a dramatic outcome. The basis for our
argument is a conjecture that was recently proposed by Arkani-Hamed and
collaborators. To put it another way, we use their notion of ``Gravity as the
Weakest Force'' as a means of inhibiting the process of black hole evaporation.Comment: 7 pages; v2 some discussion clarifie
The Measure for the Multiverse and the Probability for Inflation
We investigate the measure problem in the framework of inflationary
cosmology. The measure of the history space is constructed and applied to
inflation models. Using this measure, it is shown that the probability for the
generalized single field slow roll inflation to last for e-folds is
suppressed by a factor , and the probability for the generalized
-field slow roll inflation is suppressed by a much larger factor
. Some non-inflationary models such as the cyclic model do not
suffer from this difficulty.Comment: 16 page
Holographic dark energy model with non-minimal coupling
We find that holographic dark energy model with non-minimally coupled scalar
field gives rise to an accelerating universe by choosing Hubble scale as IR
cutoff. We show viable range of a non-minimal coupling parameter in the
framework of this model.Comment: 7 pages, no figure, corrected some typos, to be published in
Europhys. Let
Gravitational Correction and Weak Gravity Conjecture
We consider the gravitational correction to the running of gauge coupling.
Weak gravity conjecture implies that the gauge theories break down when the
gravitational correction becomes greater than the contribution from gauge
theories. This observation can be generalized to non-Abelian gauge theories in
diverse dimensions and the cases with large extra dimensions.Comment: 8 pages; minor correction and refs adde
A geometric description of the non-Gaussianity generated at the end of multi-field inflation
In this paper we mainly focus on the curvature perturbation generated at the
end of multi-field inflation, such as the multi-brid inflation. Since the
curvature perturbation is produced on the super-horizon scale, the bispectrum
and trispectrum have a local shape. The size of bispectrum is measured by
and the trispectrum is characterized by two parameters and
. For simplicity, the trajectory of inflaton is assumed to be a
straight line in the field space and then the entropic perturbations do not
contribute to the curvature perturbation during inflation. As long as the
background inflaton path is not orthogonal to the hyper-surface for inflation
to end, the entropic perturbation can make a contribution to the curvature
perturbation at the end of inflation and a large local-type non-Gaussiantiy is
expected. An interesting thing is that the non-Gaussianity parameters are
completely determined by the geometric properties of the hyper-surface of the
end of inflation. For example, is proportional to the curvature of the
curve on this hyper-surface along the adiabatic direction and is
related to the change of the curvature radius per unit arc-length of this
curve. Both and can be positive or negative respectively, but
must be positive and not less than .Comment: 19 pages, 4 figures; refs added; a correction to \tau_{NL} for
n-field inflation added, version accepted for publication in JCA
Eternal Chaotic Inflation is Prohibited by Weak Gravity Conjecture
We investigate whether the eternal chaotic inflation can be achieved when the
weak gravity conjecture is taken into account. We show that even the assisted
chaotic inflation with potential or can not be
eternal. The effective field theory description for the inflaton field breaks
down before inflation reaches the eternal regime. We also find that the total
number of e-folds is still bounded by the inflationary entropy for the assisted
inflation.Comment: 10 page
A Weak Gravity Conjecture for Scalar Field Theories
We show that the recently proposed weak gravity conjecture\cite{AMNV0601} can
be extended to a class of scalar field theories. Taking gravity into account,
we find an upper bound on the gravity interaction strength, expressed in terms
of scalar coupling parameters. This conjecture is supported by some
two-dimensional models and noncommutative field theories.Comment: version published in JHE
Revisit of the Interaction between Holographic Dark Energy and Dark Matter
In this paper we investigate the possible direct, non-gravitational
interaction between holographic dark energy (HDE) and dark matter. Firstly, we
start with two simple models with the interaction terms
and , and then we move on to the general form . The cosmological constraints of the models are
obtained from the joint analysis of the present Union2.1+BAO+CMB+ data. We
find that the data slightly favor an energy flow from dark matter to dark
energy, although the original HDE model still lies in the 95.4% confidence
level (CL) region. For all models we find at the 95.4% CL. We show that
compared with the cosmic expansion, the effect of interaction on the evolution
of and is smaller, and the relative increment
(decrement) amount of the energy in the dark matter component is constrained to
be less than 9% (15%) at the 95.4% CL. By introducing the interaction, we find
that even when the big rip still can be avoided due to the existence of a
de Sitter solution at . We show that this solution can not be
accomplished in the two simple models, while for the general model such a
solution can be achieved with a large , and the big rip may be avoided
at the 95.4% CL.Comment: 26 pages, 9 figures, version accepted for publication in JCA
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