622 research outputs found
Probing Dark Energy with Supernovae : Bias from the time evolution of the equation of state
Observation of thousands of type Ia supernovae should offer the most direct
approach to probe the dark energy content of the universe. This will be
undertaken by future large ground-based surveys followed by a space mission
(SNAP/JDEM). We address the problem of extracting the cosmological parameters
from the future data in a model independent approach, with minimal assumptions
on the prior knowledge of some parameters. We concentrate on the comparison
between a fiducial model and the fitting function and adress in particular the
effect of neglecting (or not) the time evolution of the equation of state. We
present a quantitative analysis of the bias which can be introduced by the
fitting procedure. Such bias cannot be ignored as soon as the statistical
errors from present data are drastically improved.Comment: 22 pages, 10 figures, submitted to Phys. Rev.
Particle-Like Description in Quintessential Cosmology
Assuming equation of state for quintessential matter: , we
analyse dynamical behaviour of the scale factor in FRW cosmologies. It is shown
that its dynamics is formally equivalent to that of a classical particle under
the action of 1D potential . It is shown that Hamiltonian method can be
easily implemented to obtain a classification of all cosmological solutions in
the phase space as well as in the configurational space. Examples taken from
modern cosmology illustrate the effectiveness of the presented approach.
Advantages of representing dynamics as a 1D Hamiltonian flow, in the analysis
of acceleration and horizon problems, are presented. The inverse problem of
reconstructing the Hamiltonian dynamics (i.e. potential function) from the
luminosity distance function for supernovae is also considered.Comment: 35 pages, 26 figures, RevTeX4, some applications of our treatment to
investigation of quintessence models were adde
Quintessence Restrictions on Negative Power and Condensate Potentials
We study the cosmological evolution of scalar fields that arise from a phase
transition at some energy scale \Lm_c. We focus on negative power potentials
given by V=c\Lm_c^{4+n}\phi^{-n} and restrict the cosmological viable values
of \Lm_c and . We make a complete analysis of and impose
conditions on the different cosmological parameters. The cosmological
observations ruled out models where the scalar field has reached its attractor
solution. For models where this is not the case, the analytic approximated
solutions are not good enough to determine whether a specific model is
phenomenologically viable or not and the full differential equations must be
numerically solved. The results are not fine tuned since a change of 45% on the
initial conditions does not spoil the final results. We also determine the
values of that give a condensation scale \Lm_c consistent with
gauge coupling unification, leaving only four models that satisfy unification
and SN1a constraints.Comment: 15 pages, LaTeX, 8 Figures. Minor changes in text, a discussion on
initial conditions added (accepted in Phys.Rev.D
A 5D non compact and non Ricci flat Kaluza-Klein Cosmology
A model universe is proposed in the framework of 5-dimensional noncompact
Kaluza-Klein cosmology which is not Ricci flat. The 4D part as the
Robertson-Walker metric is coupled to conventional perfect fluid, and its
extra-dimensional part is coupled to a dark pressure through a scalar field. It
is shown that neither early inflation nor current acceleration of the 4D
universe would happen if the non-vacuum states of the scalar field would
contribute to 4D cosmology.Comment: 13 pages, major revision, published online in GR
Parameterization and Reconstruction of Quasi Static Universe
We study a possibility of the fate of universe, in which there is neither the
rip singularity, which results in the disintegration of bound systems, nor the
endless expansion, instead the universe will be quasi static. We discuss the
parameterization of the corresponding evolution and the reconstruction of the
scalar field model. We find, with the parameterization consistent with the
current observation, that the current universe might arrive at a quasi static
phase after less than 20Gyr.Comment: minor changes and Refs. added, publish in EPJ
Cosmology With Non-Minimally Coupled K-Field
We consider non-minimally coupled (with gravity) scalar field with
non-canonical kinetic energy. The form of the kinetic term is of
Dirac-Born-Infeld (DBI) form.We study the early evolution of the universe when
it is sourced only by the k-field, as well as late time evolution when both the
matter and k-field are present. For the k-field, we have considered constant
potential as well as potential inspired from Boundary String Field Theory
(B-SFT). We show that it is possible to have inflationary solution in early
time as well as late time accelerating phase. The solutions also exhibit
attractor property in a sense that it does not depend on the initial conditions
for a certain values of the parameters.Comment: 10 pages, Revtex style, 14 eps figures, to appear in General
Relativity and Gravitatio
On exact solutions for quintessential (inflationary) cosmological models with exponential potentials
We first study dark energy models with a minimally-coupled scalar field and
exponential potentials, admitting exact solutions for the cosmological
equations: actually, it turns out that for this class of potentials the
Einstein field equations exhibit alternative Lagrangians, and are completely
integrable and separable (i.e. it is possible to integrate the system
analytically, at least by quadratures). We analyze such solutions, especially
discussing when they are compatible with a late time quintessential expansion
of the universe. As a further issue, we discuss how such quintessential scalar
fields can be connected to the inflationary phase, building up, for this class
of potentials, a quintessential inflationary scenario: actually, it turns out
that the transition from inflation toward late-time exponential quintessential
tail admits a kination period, which is an indispensable ingredient of this
kind of theoretical models. All such considerations have also been done by
including radiation into the model.Comment: Revtex4, 10 figure
Bounds on the possible evolution of the Gravitational Constant from Cosmological Type-Ia Supernovae
Recent high-redshift Type Ia supernovae results can be used to set new bounds
on a possible variation of the gravitational constant . If the local value
of at the space-time location of distant supernovae is different, it would
change both the kinetic energy release and the amount of Ni synthesized
in the supernova outburst. Both effects are related to a change in the
Chandrasekhar mass . In addition, the integrated
variation of with time would also affect the cosmic evolution and therefore
the luminosity distance relation. We show that the later effect in the
magnitudes of Type Ia supernovae is typically several times smaller than the
change produced by the corresponding variation of the Chandrasekhar mass. We
investigate in a consistent way how a varying could modify the Hubble
diagram of Type Ia supernovae and how these results can be used to set upper
bounds to a hypothetical variation of . We find G/G_0 \la 1.1 and G'/G
\la 10^{-11} yr^{-1} at redshifts . These new bounds extend the
currently available constrains on the evolution of all the way from solar
and stellar distances to typical scales of Gpc/Gyr, i.e. by more than 15 orders
of magnitudes in time and distance.Comment: 9 pages, 4 figures, Phys. Rev. D. in pres
Current constraints on the dark energy equation of state
We combine complementary datasets from Cosmic Microwave Background (CMB)
anisotropy measurements, high redshift supernovae (SN-Ia) observations and data
from local cluster abundances and galaxy clustering (LSS) to constrain the dark
energy equation of state parameterized by a constant pressure-to-density ratio
. Under the assumption of flatness, we find at 68% c.l.,
providing no significant evidence for quintessential behaviour different from
that of a cosmological constant. We then generalise our result to show that the
constraints placed on a constant can be safely extended to dynamical
theories. We consider a variety of quintessential dynamical models based on
inverse power law, exponential and oscillatory scaling potentials. We find that
SN1a observations are `numbed' to dynamical shifts in the equation of state,
making the prospect of reconstructing , a challenging one indeed.Comment: 6 pages, 6 figures. Version accepted for publication in PR
On the Degeneracy Inherent in Observational Determination of the Dark Energy Equation of State
Using a specific model for the expansion rate of the Universe as a function
of scale factor, it is demonstrated that the equation of state of the dark
energy cannot be determined uniquely from observations at redshifts
unless the fraction of the mass density of the Universe
in nonrelativistic particles, , somehow can be found independently. A
phenomenological model is employed to discuss the utility of additional
constraints from the formation of large scale structure and the positions of
CMB peaks in breaking the degeneracy among models for the dark energy.Comment: 12 pages, 3 figures. Several references adde
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