51,352 research outputs found
Limits from Weak Gravity Conjecture on Dark Energy Models
The weak gravity conjecture has been proposed as a criterion to distinguish
the landscape from the swampland in string theory. As an application in
cosmology of this conjecture, we use it to impose theoretical constraint on
parameters of two types of dark energy models. Our analysis indicates that the
Chaplygin-gas-type models realized in quintessence field are in the swampland,
whereas the power-low decay model of the variable cosmological constant can
be viable but the parameters are tightly constrained by the conjecture.Comment: Revtex4, 8 pages, 5 figures; References, minor corrections in
content, and acknowledgement adde
Weak Gravity Conjecture for the Effective Field Theories with N Species
We conjecture an intrinsic UV cutoff for the validity of the effective field
theory with a large number of species coupled to gravity. In four dimensions
such a UV cutoff takes the form for scalar
fields with the same potential , . This conjecture
implies that the assisted chaotic inflation or N-flation might be in the
swampland, not in the landscape. Similarly a UV cutoff
is conjectured for the U(1) gauge theory with species.Comment: 12 pages; refs added and some statements clarifie
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
Agegraphic Chaplygin gas model of dark energy
We establish a connection between the agegraphic models of dark energy and
Chaplygin gas energy density in non-flat universe. We reconstruct the potential
of the agegraphic scalar field as well as the dynamics of the scalar field
according to the evolution of the agegraphic dark energy. We also extend our
study to the interacting agegraphic generalized Chaplygin gas dark energy
model.Comment: 8 page
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
Extended Holographic dark energy
The idea of relating the infrared and ultraviolet cutoffs is applied to
Brans-Dicke theory of gravitation. We find that extended holographic dark
energy from the Hubble scale or the particle horizon as the infrared cutoff
will not give accelerating expansion. The dynamical cosmological constant with
the event horizon as the infrared cutoff is a viable dark energy model.Comment: one reference is corrected, 3 pages, no figure,V3: minor correction
Cosmological perturbations and noncommutative tachyon inflation
The motivation for studying the rolling tachyon and non-commutative inflation
comes from string theory. In the tachyon inflation scenario, metric
perturbations are created by tachyon field fluctuations during inflation. We
drive the exact mode equation for scalar perturbation of the metric and
investigate the cosmological perturbations in the commutative and
non-commutative inflationary spacetime driven by the tachyon field which have a
Born-Infeld Lagrangian.Comment: 6 two-column pages, no figur
- âŠ