511 research outputs found
Inflationary spacetimes are not past-complete
Many inflating spacetimes are likely to violate the weak energy condition, a
key assumption of singularity theorems. Here we offer a simple kinematical
argument, requiring no energy condition, that a cosmological model which is
inflating -- or just expanding sufficiently fast -- must be incomplete in null
and timelike past directions. Specifically, we obtain a bound on the integral
of the Hubble parameter over a past-directed timelike or null geodesic. Thus
inflationary models require physics other than inflation to describe the past
boundary of the inflating region of spacetime.Comment: We improve the basic argument to apply to a wider class of
spacetimes, use a better title and add a discussion of cyclic models. 4
pages, 1 figure, RevTe
Non-Singular Charged Black Hole Solution for Non-Linear Source
A non-singular exact black hole solution in General Relativity is presented.
The source is a non-linear electromagnetic field, which reduces to the Maxwell
theory for weak field. The solution corresponds to a charged black hole with
|q| \leq 2s_c m \approx 0.6 m, having metric, curvature invariants, and
electric field bounded everywhere.Comment: 3 pages, RevTe
Regular Black Hole in General Relativity Coupled to Nonlinear Electrodynamics
The first regular exact black hole solution in General Relativity is
presented. The source is a nonlinear electrodynamic field satisfying the weak
energy condition, which in the limit of weak field becomes the Maxwell field.
The solution corresponds to a charged black hole with |q| \leq 2 s_c m \approx
0.6 m, having the metric, the curvature invariants, and the electric field
regular everywhere.Comment: 5 pages, RevTex, 6 figure
Open and Closed Universes, Initial Singularities and Inflation
The existence of initial singularities in expanding universes is proved
without assuming the timelike convergence condition. The assumptions made in
the proof are ones likely to hold both in open universes and in many closed
ones. (It is further argued that at least some of the expanding closed
universes that do not obey a key assumption of the theorem will have initial
singularities on other grounds.) The result is significant for two reasons:
(a)~previous closed-universe singularity theorems have assumed the timelike
convergence condition, and (b)~the timelike convergence condition is known to
be violated in inflationary spacetimes. An immediate consequence of this
theorem is that a recent result on initial singularities in open,
future-eternal, inflating spacetimes may now be extended to include many closed
universes. Also, as a fringe benefit, the time-reverse of the theorem may be
applied to gravitational collapse.Comment: 27 pages, Plain TeX (figures are embedded in the file itself and they
will emerge if it is processed according to the instructions at the top of
the file
Eternal inflation and the initial singularity
It is shown that a physically reasonable spacetime that is eternally
inflating to the future must possess an initial singularity.Comment: 11 pages, Tufts University cosmology preprin
Atom interferometer as a selective sensor of rotation or gravity
In the presence of Earth gravity and gravity-gradient forces, centrifugal and
Coriolis forces caused by the Earth rotation, the phase of the time-domain atom
interferometers is calculated with accuracy up to the terms proportional to the
fourth degree of the time separation between pulses. We considered double-loop
atom interferometers and found appropriate condition to eliminate their
sensitivity to acceleration to get atomic gyroscope, or to eliminate the
sensitivity to rotation to increase accuracy of the atomic gravimeter.
Consequent use of these interferometers allows one to measure all components of
the acceleration and rotation frequency projection on the plane perpendicular
to gravity acceleration. Atom interference on the Raman transition driving by
noncounterpropagating optical fields is proposed to exclude stimulated echo
processes which can affect the accuracy of the atomic gyroscopes. Using
noncounterpropagating optical fields allows one to get a new type of the Ramsey
fringes arising in the unidirectional Raman pulses and therefore centered at
the two-quantum line center. Density matrix in the Wigner representation is
used to perform calculations. It is shown that in the time between pulses, in
the noninertial frame, for atoms with fully quantized spatial degrees of
freedom, this density matrix obeys classical Liouville equations.Comment: 21 pages, 4 figures, extended references, discussion, and motivatio
as parameter of Minkowski metric in effective theory
With the proper choice of the dimensionality of the metric components, the
action for all fields becomes dimensionless. Such quantities as the vacuum
speed of light c, the Planck constant \hbar, the electric charge e, the
particle mass m, the Newton constant G never enter equations written in the
covariant form, i.e., via the metric g^{\mu\nu}. The speed of light c and the
Planck constant are parameters of a particular two-parametric family of
solutions of general relativity equations describing the flat isotropic
Minkowski vacuum in effective theory emerging at low energy:
g^{\mu\nu}=diag(-\hbar^2, (\hbar c)^2, (\hbar c)^2, (\hbar c)^2). They
parametrize the equilibrium quantum vacuum state. The physical quantities which
enter the covariant equations are dimensionless quantities and dimensionful
quantities of dimension of rest energy M or its power. Dimensionless quantities
include the running coupling `constants' \alpha_i; topological and geometric
quantum numbers (angular momentum quantum number j, weak charge, electric
charge q, hypercharge, baryonic and leptonic charges, number of atoms N, etc).
Dimensionful parameters include the rest energies of particles M_n (or/and mass
matrices); the gravitational coupling K with dimension of M^2; cosmological
constant with dimension M^4; etc. In effective theory, the interval s has the
dimension of 1/M; it characterizes the dynamics of particles in the quantum
vacuum rather than geometry of space-time. We discuss the effective action, and
the measured physical quantities resulting from the action, including
parameters which enter the Josepson effect, quantum Hall effect, etc.Comment: 18 pages, no figures, extended version of the paper accepted in JETP
Letter
Methods of approaching decoherence in the flavour sector due to space-time foam
In the first part of this work we discuss possible effects of stochastic
space-time foam configurations of quantum gravity on the propagation of
``flavoured'' (Klein-Gordon and Dirac) neutral particles, such as neutral
mesons and neutrinos. The formalism is not the usually assumed Lindblad one,
but it is based on random averages of quantum fluctuations of space time
metrics over which the propagation of the matter particles is considered. We
arrive at expressions for the respective oscillation probabilities between
flavours which are quite distinct from the ones pertaining to Lindblad-type
decoherence, including in addition to the (expected) Gaussian decay with time,
a modification to oscillation behaviour, as well as a power-law cutoff of the
time-profile of the respective probability. In the second part we consider
space-time foam configurations of quantum-fluctuating charged black holes as a
way of generating (parts of) neutrino mass differences, mimicking appropriately
the celebrated MSW effects of neutrinos in stochastically fluctuating random
media. We pay particular attention to disentangling genuine quantum-gravity
effects from ordinary effects due to the propagation of a neutrino through
ordinary matter. Our results are of interest to precision tests of quantum
gravity models using neutrinos as probes.Comment: 35 pages revtex, no figures, typos corrected in section II
Recycling universe
If the effective cosmological constant is non-zero, our observable universe
may enter a stage of exponential expansion. In such case, regions of it may
tunnel back to the false vacuum of an inflaton scalar field, and inflation with
a high expansion rate may resume in those regions. An ``ideal'' eternal
observer would then witness an infinite succession of cycles from false vacuum
to true, and back. Within each cycle, the entire history of a hot universe
would be replayed. If there were several minima of the inflaton potential, our
ideal observer would visit each one of these minima with a frequency which
depends on the shape of the potential. We generalize the formalism of
stochastic inflation to analyze the global structure of the universe when this
`recycling' process is taken into account.Comment: 43 pages, 10 figure
Theorems on gravitational time delay and related issues
Two theorems related to gravitational time delay are proven. Both theorems
apply to spacetimes satisfying the null energy condition and the null generic
condition. The first theorem states that if the spacetime is null geodesically
complete, then given any compact set , there exists another compact set
such that for any , if there exists a ``fastest null
geodesic'', , between and , then cannot enter . As
an application of this theorem, we show that if, in addition, the spacetime is
globally hyperbolic with a compact Cauchy surface, then any observer at
sufficiently late times cannot have a particle horizon. The second theorem
states that if a timelike conformal boundary can be attached to the spacetime
such that the spacetime with boundary satisfies strong causality as well as a
compactness condition, then any ``fastest null geodesic'' connecting two points
on the boundary must lie entirely within the boundary. It follows from this
theorem that generic perturbations of anti-de Sitter spacetime always produce a
time delay relative to anti-de Sitter spacetime itself.Comment: 15 pages, 1 figure. Example of gauge perturbation changed/corrected.
Two footnotes added and one footnote remove
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