12,081 research outputs found
Exact solutions of Brans-Dicke cosmology with decaying vacuum density
We investigate cosmological solutions of Brans-Dicke theory with both the
vacuum energy density and the gravitational constant decaying linearly with the
Hubble parameter. A particular class of them, with constant deceleration
factor, sheds light on the cosmological constant problems, leading to a
presently small vacuum term, and to a constant ratio between the vacuum and
matter energy densities. By fixing the only free parameter of these solutions,
we obtain cosmological parameters in accordance with observations of both the
relative matter density and the universe age. In addition, we have three other
solutions, with Brans-Dicke parameter w = -1 and negative cosmological term,
two of them with a future singularity of big-rip type. Although interesting
from the theoretical point of view, two of them are not in agreement with the
observed universe. The third one leads, in the limit of large times, to a
constant relative matter density, being also a possible solution to the cosmic
coincidence problem.Comment: Minor changes, references added. Version accepted for publication in
Classical and Quantum Gravit
Exact solutions of Brans-Dicke cosmology and the cosmic coincidence problem
We present some cosmological solutions of Brans-Dicke theory, characterized
by a decaying vacuum energy density and by a constant relative matter density.
With these features, they shed light on the cosmological constant problems,
leading to a presently small vacuum term, and to a constant ratio between the
vacuum and matter energy densities. By fixing the only free parameter of our
solutions, we obtain cosmological parameters in accordance with observations of
the relative matter density, the universe age and redshift-distance relations.Comment: To appear in Brazilian Journal of Physics (proceedings of the
conference 100 Years of Relativity, Sao Paulo, August 2005
Identificação de proteínas que interagem com o fator de elongação EF1 alfa no endosperma do grão do milho.
bitstream/item/68614/1/ct-193.pd
Friedmann cosmology with decaying vacuum density
Among the several proposals to solve the incompatibility between the observed
small value of the cosmological constant and the huge value obtained by quantum
field theories, we can find the idea of a decaying vacuum energy density,
leading from high values at early times of universe evolution to the small
value observed nowadays. In this paper we consider a variation law for the
vacuum density recently proposed by Schutzhold on the basis of quantum field
estimations in the curved, expanding background, characterized by a vacuum
density proportional to the Hubble parameter. We show that, in the context of
an isotropic and homogeneous, spatially flat model, the corresponding solutions
retain the well established features of the standard cosmology, and, in
addition, are in accordance with the observed cosmological parameters. Our
scenario presents an initial phase dominated by radiation, followed by a dust
era long enough to permit structure formation, and by an epoch dominated by the
cosmological term, which tends asymptotically to a de Sitter universe. Taking
the matter density equals to half of the vacuum energy density, as suggested by
observation, we obtain a universe age given by Ht = 1.1, and a decelerating
parameter equals to -1/2.Comment: Accepted for publication in General Relativity and Gravitatio
Cosmological Signatures of Anisotropic Spatial Curvature
If one is willing to give up the cherished hypothesis of spatial isotropy,
many interesting cosmological models can be developed beyond the simple
anisotropically expanding scenarios. One interesting possibility is presented
by shear-free models in which the anisotropy emerges at the level of the
curvature of the homogeneous spatial sections, whereas the expansion is
dictated by a single scale factor. We show that such models represent viable
alternatives to describe the large-scale structure of the inflationary
universe, leading to a kinematically equivalent Sachs-Wolfe effect. Through the
definition of a complete set of spatial eigenfunctions we compute the two-point
correlation function of scalar perturbations in these models. In addition, we
show how such scenarios would modify the spectrum of the CMB assuming that the
observations take place in a small patch of a universe with anisotropic
curvature.Comment: 21 pages, 1 figure. To appear in JCA
Inflationary Perturbations in Anisotropic, Shear-Free Universes
In this work, the linear and gauge-invariant theory of cosmological
perturbations in a class of anisotropic and shear-free spacetimes is developed.
After constructing an explicit set of complete eigenfunctions in terms of which
perturbations can be expanded, we identify the effective degrees of freedom
during a generic slow-roll inflationary phase. These correspond to the
anisotropic equivalent of the standard Mukhanov-Sasaki variables. The
associated equations of motion present a remarkable resemblance to those found
in perturbed Friedmann-Robertson-Walker spacetimes with curvature, apart from
the spectrum of the Laplacian, which exhibits the characteristic frequencies of
the underlying geometry. In particular, it is found that the perturbations
cannot develop arbitrarily large super-Hubble modes.Comment: 24 pages, 2 figure
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