7,009 research outputs found
Measure Problem for Eternal and Non-Eternal Inflation
We study various probability measures for eternal inflation by applying their
regularization prescriptions to models where inflation is not eternal. For
simplicity we work with a toy model describing inflation that can interpolate
between eternal and non-eternal inflation by continuous variation of a
parameter. We investigate whether the predictions of four different measures
(proper time, scale factor cutoff, stationary and causal {diamond}) change
continuously with the change of this parameter. We will show that {only} for
the stationary measure the predictions change continuously. For the proper-time
and the scale factor cutoff, the predictions are strongly discontinuous. For
the causal diamond measure, the predictions are continuous only if the stage of
the slow-roll inflation is sufficiently long.Comment: 9 pages, 4 figure
Towards a gauge invariant volume-weighted probability measure for eternal inflation
An improved volume-weighted probability measure for eternal inflation is
proposed. For the models studied in this paper it leads to simple and
intuitively expected gauge-invariant results.Comment: 16 pages, 3 figs, few misprints corrected, comments adde
Towards the Theory of Cosmological Phase Transitions
We discuss recent progress (and controversies) in the theory of finite
temperature phase transitions. This includes the structure of the effective
potential at a finite temperature, the infrared problem in quantum statistics
of gauge fields, the theory of formation of critical and subcritical bubbles
and the theory of bubble wall propagation.Comment: 50 p
Relaxing the Cosmological Moduli Problem
Typically the moduli fields acquire mass m =C H in the early universe, which
shifts the position of the minimum of their effective potential and leads to an
excessively large energy density of the oscillating moduli fields at the later
stages of the evolution of the universe. This constitutes the cosmological
moduli problem, or Polonyi field problem. We show that the cosmological moduli
problem can be solved or at least significantly relaxed in the theories in
which C >> 1, as well as in some models with C << 1.Comment: 9 pages, 3 Postscript figure
Inflation with
We discuss various models of inflationary universe with . A
homogeneous universe with may appear due to creation of the
universe "from nothing" in the theories where the effective potential becomes
very steep at large , or in the theories where the inflaton field
nonminimally couples to gravity. Inflation with generally requires
intermediate first order phase transition with the bubble formation, and with a
second stage of inflation inside the bubble. It is possible to realize this
scenario in the context of a theory of one scalar field, but typically it
requires artificially bent effective potentials and/or nonminimal kinetic
terms. It is much easier to obtain an open universe in the models involving two
scalar fields. However, these models have their own specific problems. We
propose three different models of this type which can describe an open
homogeneous inflationary universe.Comment: 29 pages, LaTeX, parameters of one of the models are slightly
modifie
Creation of the universe with a stealth scalar field
The stealth scalar field is a non-trivial configuration without any
back-reaction to geometry, which is characteristic for non-minimally coupled
scalar fields. Studying the creation probability of the de Sitter universe with
a stealth scalar field by the Hartle and Hawking's semi-classical method, we
show that the effect of the stealth field can be significant. For the class of
scalar fields we consider, creation with a stealth field is possible for a
discrete value of the coupling constant and its creation probability is always
less than that with a trivial scalar field. However, those creation rates can
be almost the same depending on the parameters of the theory.Comment: 7 pages; v2, references added; v3, creation of the open universe
adde
Relic Gravitons, Dominant Energy Condition and Bulk Viscous Stresses
If the energy momentum tensor contains bulk viscous stresses violating the
dominant energy condition (DOC) the energy spectra of the relic gravitons
(produced at the time of the DOC's violation) increase in frequency in a
calculable way. In a general relativistic context we give examples where the
DOC is only violated for a limited amount of time after which the ordinary
(radiation dominated) evolution takes place. We connect our discussion to some
recent remarks of Grishchuk concerning the detectability of the stochastic
gravitational wave background by the forthcoming interferometric detectors.Comment: 7 pages in LaTex style. Accepted for publication in Phys. Rev. D
(Rapid Comm.
Warm inflation and scalar perturbations of the metric
A second-order expansion for the quantum fluctuations of the matter field was
considered in the framework of the warm inflation scenario. The friction and
Hubble parameters were expended by means of a semiclassical approach. The
fluctuations of the Hubble parameter generates fluctuations of the metric.
These metric fluctuations produce an effective term of curvature. The power
spectrum for the metric fluctuations can be calculated on the infrared sector.Comment: 10 pages, no figures, to be published in General Rel. and Gravitatio
The non-unique Universe
The purpose of this paper is to elucidate, by means of concepts and theorems
drawn from mathematical logic, the conditions under which the existence of a
multiverse is a logical necessity in mathematical physics, and the implications
of Godel's incompleteness theorem for theories of everything.
Three conclusions are obtained in the final section: (i) the theory of the
structure of our universe might be an undecidable theory, and this constitutes
a potential epistemological limit for mathematical physics, but because such a
theory must be complete, there is no ontological barrier to the existence of a
final theory of everything; (ii) in terms of mathematical logic, there are two
different types of multiverse: classes of non-isomorphic but elementarily
equivalent models, and classes of model which are both non-isomorphic and
elementarily inequivalent; (iii) for a hypothetical theory of everything to
have only one possible model, and to thereby negate the possible existence of a
multiverse, that theory must be such that it admits only a finite model
Islands in the landscape
The string theory landscape consists of many metastable de Sitter vacua,
populated by eternal inflation. Tunneling between these vacua gives rise to a
dynamical system, which asymptotically settles down to an equilibrium state. We
investigate the effects of sinks to anti-de Sitter space, and show how their
existence can change probabilities in the landscape. Sinks can disturb the
thermal occupation numbers that would otherwise exist in the landscape and may
cause regions that were previously in thermal contact to be divided into
separate, thermally isolated islands.Comment: 31 pages, 8 figure
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