50,322 research outputs found
Effective interactions from q-deformed inspired transformations
From the mass term for the transformed quark fields, we obtain effective
contact interactions of the NJL type. The parameters of the model that maps a
system of non-interacting transformed fields into quarks interacting via NJL
contact terms are discussed
Gravitational Wave Emission and Mass Extraction from a Perturbed Schwarzschild Black Hole (continue)
A relativistic model for the emission of gravitational waves from an
initially unperturbed Schwarzschild black hole, or spherical collapsing
configuration, is completely integrated. The model consists basically of
gravitational perturbations of the Robinson-Trautman type on the Schwarzschild
spacetime. In our scheme of perturbation, gravitational waves may extract mass
from the collapsing configuration. Robinson-Trautmann perturbations also
include another mode of emission of mass, which we denote shell emission mode:
in the equatorial plane of the configuration, a timelike shell of
matter may be present, whose stress-energy tensor is modelled by neutrinos and
strings emitted radially on the shell; no gravitational waves are present in
this mode. The invariant characterization of gravitational wave perturbations
and of the gravitational wave zone is made through the analysis of the
structure of the curvature tensor and the use of the Peeling Theorem.Comment: 26 pages, LaTex, no figure
Studying light propagation in a locally homogeneous universe through an extended Dyer-Roeder approach
Light is affected by local inhomogeneities in its propagation, which may
alter distances and so cosmological parameter estimation. In the era of
precision cosmology, the presence of inhomogeneities may induce systematic
errors if not properly accounted. In this vein, a new interpretation of the
conventional Dyer-Roeder (DR) approach by allowing light received from distant
sources to travel in regions denser than average is proposed. It is argued that
the existence of a distribution of small and moderate cosmic voids (or "black
regions") implies that its matter content was redistributed to the homogeneous
and clustered matter components with the former becoming denser than the cosmic
average in the absence of voids. Phenomenologically, this means that the DR
smoothness parameter (denoted here by ) can be greater than unity,
and, therefore, all previous analyses constraining it should be rediscussed
with a free upper limit. Accordingly, by performing a statistical analysis
involving 557 type Ia supernovae (SNe Ia) from Union2 compilation data in a
flat CDM model we obtain for the extended parameter,
(). The effects of are also
analyzed for generic CDM models and flat XCDM cosmologies. For both
models, we find that a value of greater than unity is able to
harmonize SNe Ia and cosmic microwave background observations thereby
alleviating the well-known tension between low and high redshift data. Finally,
a simple toy model based on the existence of cosmic voids is proposed in order
to justify why can be greater than unity as required by supernovae
data.Comment: 5 pages, 2 figures. Title modified, results unchanged. It matches
version published as a Brief Report in Phys. Rev.
Comment on "Constraining the smoothness parameter and dark energy using observational H(z) data"
In this Comment we discuss a recent analysis by Yu et al. [RAA 11, 125
(2011)] about constraints on the smoothness parameter and dark energy
models using observational data. It is argued here that their procedure
is conceptually inconsistent with the basic assumptions underlying the adopted
Dyer-Roeder approach. In order to properly quantify the influence of the
data on the smoothness parameter, a -test involving a sample
of SNe Ia and data in the context of a flat CDM model is
reanalyzed. This result is confronted with an earlier approach discussed by
Santos et al. (2008) without data. In the () plane, it
is found that such parameters are now restricted on the intervals and within 95.4% confidence
level (2), and, therefore, fully compatible with the homogeneous case.
The basic conclusion is that a joint analysis involving data can
indirectly improve our knowledge about the influence of the inhomogeneities.
However, this happens only because the data provide tighter constraints
on the matter density parameter .Comment: 3 pages, 1 figure, submitted to Research in Astronomy and
Astrophysic
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