271 research outputs found
Exit from Inflation with a First-Order Phase Transition and a Gravitational Wave Blast
In double-field inflation, which exploits two scalar fields, one of the
fields rolls slowly during inflation whereas the other field is trapped in a
meta-stable vacuum. The nucleation rate from the false vacuum to the true one
becomes substantial enough that triggers a first order phase transition and
ends inflation. We revisit the question of first order phase transition in an
"extended" model of hybrid inflation, realizing the double-field inflationary
scenario, and correctly identify the parameter space that leads to a first
order phase transition at the end of inflation. We compute the gravitational
wave profile which is generated during this first order phase transition.
Assuming instant reheating, the peak frequency falls in the GHz to GHz
frequency band and the amplitude varies in the range , depending on the value of the
cosmological constant in the false vacuum. The signature could be observed by
the planned Chongqing high frequency gravitational probe. For a narrow band of
vacuum energies, the first order phase transition can happen after the end of
inflation via the violation of slow-roll, with a peak frequency that varies
from THz to THz. For smaller values of cosmological constant, even
though inflation can end via slow-roll violation, the universe gets trapped in
a false vacuum whose energy drives a second phase of eternal inflation. This
range of vacuum energies do not lead to viable inflationary models, unless the
value of the cosmological constant is compatible with the observed value,
eV.Comment: v1: 15 pages, 8 Figures; v2: typos corrected;v3: matched the PLB
versio
Rescuing Single Field Inflation from the Swampland
The difficulty of building metastable vacua in string theory has led some to
conjecture that, in the string theory landscape, potentials satisfy
. This condition, which is
supported by different explicit constructions, suggests that the EFTs which
lead to metastable de-Sitter vacua belong to what is dubbed as swampland. This
condition endangers the paradigm of single field inflation. In this paper, we
show how scalar excited initial states cannot rescue single field inflation
from the swampland, as they produce large local scalar non-gaussianity, which
is in conflict with the Planck upper bound. Instead, we demonstrate that one
can salvage single field inflation using excited initial states for tensor
perturbations, which in this case produce only large flattened non-gaussianity
in the tensor bispectrum. We comment on the possible methods one can prepare
such excited initial conditions for the tensor perturbations.Comment: v1: 8 pages double columns, no figures; v2: references added, matched
the PLB versio
A Note on Calm Excited States of Inflation
We identify a two-parameter family of excited states within slow-roll
inflation for which either the corrections to the two-point function or the
characteristic signatures of excited states in the three-point function -- i.e.
the enhancement for the flattened momenta configurations-- are absent. These
excited states may nonetheless violate the adiabaticity condition maximally. We
dub these initial states of inflation calm excited states. We show that these
two sets do not intersect, i.e., those that leave the power-spectrum invariant
can be distinguished from their bispectra, and vice versa. The same set of calm
excited states that leave the two-point function invariant for slow-roll
inflation, do the same task for DBI inflation. However, at the level of
three-point function, the calm excited states whose flattened configuration
signature is absent for slow-roll inflation, will lead to an enhancement for
DBI inflation generally, although the signature is smaller than what suggested
by earlier analysis. This example also illustrates that imposing the Wronskian
condition is important for obtaining a correct estimate of the non-Gaussian
signatures.Comment: v1: 13 pages; v2: matched the JCAP versio
Observing the Structure of the Landscape with the CMB Experiments
Assuming that inflation happened through a series of tunneling in the string
theory landscape, it is argued that one can determine the structure of vacua
using precise measurements of the scalar spectral index and tensor
perturbations at large scales. It is shown that for a vacuum structure where
the energy gap between the minima is constant, i.e. , one
obtains the scalar spectral index, , to be , for the modes
that exit the horizon 60 e-folds before the end of inflation. Alternatively,
for a vacuum structure in which the energy gap increases linearly with the
vacuum index, i.e. , turns out to be
. Both these two models are motivated within the string theory
landscape using flux-compactification and their predictions for scalar spectral
index are compatible with WMAP results. For both these two models, the results
for the scalar spectral index turn out to be independent of . Nonetheless,
assuming that inflation started at Planckian energies and that there had been
successful thermalization at each step, one can constrain and in these two models,
respectively. Violation of the single-field consistency relation between the
tensor and scalar spectra is another prediction of chain inflation models. This
corresponds to having a smaller tensor/scalar ratio at large scales in
comparison with the slow-roll counterparts. Similar to slow-roll inflation, it
is argued that one can reconstruct the vacuum structure using the CMB
experiments.Comment: v1: 8 pages, 2 figures; v2: grammatical typos corrected, results
unchanged v3: To be published in JCA
Black Holes as Beads on Cosmic Strings
We consider the possibility of formation of cosmic strings with black holes
as beads. We focus on the simplest setup where two black holes are formed on a
long cosmic string. It turns out the in absence of a background magnetic field
and for observationally viable values for cosmic string tensions, , the tension of the strut in between the black holes has to be less
than the ones that run into infinity. This result does not change if a
cosmological constant is present. However if the background magnetic field is
turned on, we can have stable setups where the tensions of all cosmic strings
are equal. We derive the equilibrium conditions in each of these setups
depending on whether the black holes are extremal or non-extremal. We obtain
cosmologically acceptable solutions with solar mass black holes and
intragalactic strength cosmic magnatic field.Comment: v1: 1+13 pages, 1 figure; v2: References added, typos corrected; v3:
Matched the published versio
Gauged M-flation After BICEP2
In view of the recent BICEP2 results [arXiv:1403.3985] which may be
attributed to the observation of B-modes polarization of the CMB with
tensor-to-scalar ratio , we revisit M-flation model.
Gauged M-flation is a string theory motivated inflation model with Matrix
valued scalar inflaton fields in the adjoint representation of a
Yang-Mills theory. In continuation of our previous works, we show that in the
M-flation model induced from a supersymmetric 10d background probed by a stack
of D3-branes, the "effective inflaton" has a double-well Higgs-like
potential, with minima at . We focus on the ,
symmetry-breaking region. We thoroughly examine predictions of the model for
in the region allowed for by the Planck experiment. As
computed in [arXiv:0903.1481], for and we find , which sits in the sweet spot of BICEP2 region for . We find that with
increasing arbitrarily, cannot go beyond . As
varies in the range which is allowed by Planck and could be reached
by the model, varies in the range . Future cosmological
experiments, like the CMBPOL, that confines with can
constrain the model further. Also, in this region of potential, for
, we find that the largest isocurvature mode, which is uncorrelated
with curvature perturbations, has a power spectrum with the amplitude of order
at the end of inflation. We also discuss the range of predictions of
in the hilltop region, .Comment: v1:16 pages, 9 figures; v2: matched the published versio
Matrix Inflation and the Landscape of its Potential
Recently we introduced an inflationary setup in which the inflaton fields are
matrix valued scalar fields with a generic quartic potential, M-flation. In
this work we study the landscape of various inflationary models arising from
M-flation. The landscape of the inflationary potential arises from the dynamics
of concentric multiple branes in appropriate flux compactifications of string
theory. After discussing the classical landscape of the theory we study the
possibility of transition among various inflationary models appearing at
different points on the landscape, mapping the quantum landscape of M-flation.
As specific examples, we study some two-field inflationary models arising from
this theory in the landscape.Comment: v1: 34 pages, 5 figures; v2: To be published in JCAP; v3: JCAP
versio
On the Tensor/Scalar Ratio in Inflation with UV Cutoff
Anisotropy of the cosmic microwave background radiation (CMB) originates from
both tensor and scalar perturbations. To study the characteristics of each of
these two kinds of perturbations, one has to determine the contribution of each
to the anisotropy of CMB. For example, the ratio of the power spectra of
tensor/scalar perturbations can be used to tighten bounds on the scalar
spectral index. We investigate here the implications for the tensor/scalar
ratio of the recent discovery (noted in astro-ph/0410139) that the introduction
of a minimal length cutoff in the structure of spacetime does not leave
boundary terms invariant. Such a cutoff introduces an ambiguity in the choice
of action for tensor and scalar perturbations, which in turn can affect this
ratio. We numerically solve for both tensor and scalar mode equations in a
near-de-sitter background and explicitly find the cutoff dependence of the
tensor/scalar ratio during inflation.Comment: 19 pages, 14 figures, to appear in Nucl. Phys. B; v4: typos
corrected, matched with the published versio
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