953 research outputs found
Scalar Field Cosmologies with Viscous Fluid
We investigate cosmological models with a free scalar field and a viscous
fluid. We find exact solutions for a linear and nonlinear viscosity pressure.
Both yield singular and bouncing solutions. In the first regime, a de Sitter
stage is asymptotically stable, while in the second case we find power-law
evolutions for vanishing cosmological constant.Comment: 8 pages, LaTeX. To be published in International Journal of Modern
Physics
Observation of the beam-size effect at HERA
A precise measurement of the spectrum of the photons from bremsstrahlung
with the ZEUS luminosity monitor at HERA is reported. The measurement shows a
reduced rate compared to the Bethe-Heitler spectrum for photon energies below
5~GeV. This suppression, called the beam-size effect, is explained by the
finite transverse size of the beam overlap relative to the typical impact
parameter in the process of bremsstrahlung at HERA energies.Comment: 12 pages, late
Relaxation dominated cosmological expansion
The behavior near the singularity of an isotropic, homogeneous cosmological
model with a viscous fluid source is investigated. This turns out to be a
relaxation dominated regime. Full extended irreversible thermodynamics is used,
and comparison with results of the truncated theory is made. New singular
behaviors are found and it is shown that a relaxation dominated inflationary
epoch may exist for fluids with small heat capacity.Comment: 7 pages, LaTeX. To be published in Physics Letters
Time-Symmetrization and Isotropization of Stiff-Fluid Kantowski-Sachs Universes
It is shown that growing-entropy stiff-fluid Kantowski-Sachs universes become
time-symmetric (if they start with time-asymmetric phase) and isotropize.
Isotropization happens without any inflationary era during the evolution since
there is no cosmological term here. It seems that this approach is an
alternative to inflation since the universe gets bigger and bigger approaching
'flatness'.Comment: 9 pages, no figure
Asymptonic states of Friedman universe and the energy conditions using the phase variable method
The evolution of Friedman models with arbitrary pressure p = p(, H) in the phase plane: Hubble function-energy density a is presented. The conclusions are: critical points of the phase plane and their stability depend on energy conditions but not on the actual form of pressure; models with constant viscosity violate the condition e + p 0; the weak and the strong energy conditions are preserved if the viscosity coefficient is proportional to
Can a matter-dominated model with constant bulk viscosity drive the accelerated expansion of the universe?
We test a cosmological model which the only component is a pressureless fluid
with a constant bulk viscosity as an explanation for the present accelerated
expansion of the universe. We classify all the possible scenarios for the
universe predicted by the model according to their past, present and future
evolution and we test its viability performing a Bayesian statistical analysis
using the SCP ``Union'' data set (307 SNe Ia), imposing the second law of
thermodynamics on the dimensionless constant bulk viscous coefficient \zeta and
comparing the predicted age of the universe by the model with the constraints
coming from the oldest globular clusters.
The best estimated values found for \zeta and the Hubble constant Ho are:
\zeta=1.922 \pm 0.089 and Ho=69.62 \pm 0.59 km/s/Mpc with a \chi^2=314. The age
of the universe is found to be 14.95 \pm 0.42 Gyr. We see that the estimated
value of Ho as well as of \chi^2 are very similar to those obtained from LCDM
model using the same SNe Ia data set. The estimated age of the universe is in
agreement with the constraints coming from the oldest globular clusters.
Moreover, the estimated value of \zeta is positive in agreement with the second
law of thermodynamics (SLT).
On the other hand, we perform different forms of marginalization over the
parameter Ho in order to study the sensibility of the results to the way how Ho
is marginalized. We found that it is almost negligible the dependence between
the best estimated values of the free parameters of this model and the way how
Ho is marginalized in the present work. Therefore, this simple model might be a
viable candidate to explain the present acceleration in the expansion of the
universe.Comment: 31 pages, 12 figures and 2 tables. Accepted to be published in the
Journal of Cosmology and Astroparticle Physics. Analysis using the new SCP
"Union" SNe Ia dataset instead of the Gold 2006 and ESSENCE datasets and
without changes in the conclusions. Added references. Related works:
arXiv:0801.1686 and arXiv:0810.030
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