11 research outputs found
On the scaling rules for the anomaly-induced effective action of metric and electromagnetic field
The anomaly-induced effective action is a useful tool for deriving the
contributions coming from quantum effects of massless conformal fields. It is
well-known that such corrections in the higher derivative vacuum sector of the
gravitational action provide the same exponential inflation (Starobinsky model)
as the cosmological constant term. At the same time, the presence of a
classical electromagnetic field breaks down the exponential solution. In this
paper we explore the role of the anomaly-induced term in the radiation sector
and, furthermore, derive the ``equation of state'' and the scaling laws for all
terms in the Einstein equations. As one could expect, the scaling law for the
vacuum anomaly-induced effective action is the same as for the cosmological
constant.Comment: 12 pages, LaTeX, 4 figure
Anomaly-Induced Effective Action and Inflation
In the early Universe matter can be described as a conformal invariant
ultra-relativistic perfect fluid, which does not contribute, on classical
level, to the evolution of the isotropic and homogeneous metric. If we suppose
that there is some desert in the particle spectrum just below the Planck mass,
then the effect of conformal trace anomaly is dominating at the corresponding
energies. With some additional constraints on the particle content of the
underlying gauge model (which favor extended or supersymmetric versions of the
Standard Model rather than the minimal one), one arrives at the stable
inflation. We review the model and report about the calculation of the
gravitational waves on the background of the anomaly-induced inflation. The
result for the perturbation spectrum is close to the one for the conventional
inflaton model, and is in agreement with the existing Cobe data (see also
[hep-th/0009197]).Comment: 4 pages, LaTeX. Contribution to the Proceedings of the EuroConference
on Frontiers in Particle Astrophysics and Cosmology, 30 September - 5 October
2000. San Feliu, Spai
Dark energy perturbations and cosmic coincidence
While there is plentiful evidence in all fronts of experimental cosmology for
the existence of a non-vanishing dark energy (DE) density \rho_D in the
Universe, we are still far away from having a fundamental understanding of its
ultimate nature and of its current value, not even of the puzzling fact that
\rho_D is so close to the matter energy density \rho_M at the present time
(i.e. the so-called "cosmic coincidence" problem). The resolution of some of
these cosmic conundrums suggests that the DE must have some (mild) dynamical
behavior at the present time. In this paper, we examine some general properties
of the simultaneous set of matter and DE perturbations (\delta\rho_M,
\delta\rho_D) for a multicomponent DE fluid. Next we put these properties to
the test within the context of a non-trivial model of dynamical DE (the LXCDM
model) which has been previously studied in the literature. By requiring that
the coupled system of perturbation equations for \delta\rho_M and \delta\rho_D
has a smooth solution throughout the entire cosmological evolution, that the
matter power spectrum is consistent with the data on structure formation and
that the "coincidence ratio" r=\rho_D/\rho_M stays bounded and not unnaturally
high, we are able to determine a well-defined region of the parameter space
where the model can solve the cosmic coincidence problem in full compatibility
with all known cosmological data.Comment: Typos correcte
Effective growth of matter density fluctuations in the running LCDM and LXCDM models
We investigate the matter density fluctuations \delta\rho/\rho for two dark
energy (DE) models in the literature in which the cosmological term \Lambda is
a running parameter. In the first model, the running LCDM model, matter and DE
exchange energy, whereas in the second model, the LXCDM model, the total DE and
matter components are conserved separately. The LXCDM model was proposed as an
interesting solution to the cosmic coincidence problem. It includes an extra
dynamical component, the "cosmon" X, which interacts with the running \Lambda,
but not with matter. In our analysis we make use of the current value of the
linear bias parameter, b^2(0)= P_{GG}/P_{MM}, where P_{MM} ~
(\delta\rho/\rho)^2 is the present matter power spectrum and P_{GG} is the
galaxy fluctuation power spectrum. The former can be computed within a given
model, and the latter is found from the observed LSS data (at small z) obtained
by the 2dF galaxy redshift survey. It is found that b^2(0)=1 within a 10%
accuracy for the standard LCDM model. Adopting this limit for any DE model and
using a method based on the effective equation of state for the DE, we can set
a limit on the growth of matter density perturbations for the running LCDM
model, the solution of which is known. This provides a good test of the
procedure, which we then apply to the LXCDM model in order to determine the
physical region of parameter space, compatible with the LSS data. In this
region, the LXCDM model is consistent with known observations and provides at
the same time a viable solution to the cosmic coincidence problem.Comment: LaTeX, 38 pages, 8 figures. Version accepted in JCA
Novellierung des Energiewirtschaftsgesetzes
SIGLEAvailable from FIZ Karlsruhe / FIZ - Fachinformationszzentrum Karlsruhe / TIB - Technische InformationsbibliothekDEGerman