188 research outputs found
Bounding the Hubble flow in terms of the w parameter
The last decade has seen increasing efforts to circumscribe and bound the
cosmological Hubble flow in terms of model-independent constraints on the
cosmological fluid - such as, for instance, the classical energy conditions of
general relativity. Quite a bit can certainly be said in this regard, but much
more refined bounds can be obtained by placing more precise constraints (either
theoretical or observational) on the cosmological fluid. In particular, the use
of the w-parameter (w=p/rho) has become increasingly common as a surrogate for
trying to say something about the cosmological equation of state. Herein we
explore the extent to which a constraint on the w-parameter leads to useful and
nontrivial constraints on the Hubble flow, in terms of constraints on density
rho(z), Hubble parameter H(z), density parameter Omega(z), cosmological
distances d(z), and lookback time T(z). In contrast to other partial results in
the literature, we carry out the computations for arbitrary values of the space
curvature k in [-1,0,+1], equivalently for arbitrary Omega_0 <= 1.Comment: 15 page
Accelerating expansion and change of signature
We show that some types of sudden singularities admit a natural explanation
in terms of regular changes of signature on brane-worlds in AdS. The
present accelerated expansion of the Universe and its possible ending at a
sudden singularity may therefore simply be an indication that our braneworld is
about to change its Lorentzian signature to an Euclidean one, while remaining
fully regular. An explicit example of this behaviour satisfying the weak and
strong energy conditions is presented.Comment: LaTeX, 4 pages. Uses the eas.cls class. To appear in the proceedings
of the Spanish Relativity Meeting ERE'0
Cosmological milestones and energy conditions
Until recently, the physically relevant singularities occurring in FRW
cosmologies had traditionally been thought to be limited to the "big bang", and
possibly a "big crunch". However, over the last few years, the zoo of
cosmological singularities considered in the literature has become considerably
more extensive, with "big rips" and "sudden singularities" added to the mix, as
well as renewed interest in non-singular cosmological events such as "bounces"
and "turnarounds". In this talk, we present an extensive catalogue of such
cosmological milestones, both at the kinematical and dynamical level. First,
using generalized power series, purely kinematical definitions of these
cosmological events are provided in terms of the behaviour of the scale factor
a(t). The notion of a "scale-factor singularity" is defined, and its relation
to curvature singularities (polynomial and differential) is explored. Second,
dynamical information is extracted by using the Friedmann equations (without
assuming even the existence of any equation of state) to place constraints on
whether or not the classical energy conditions are satisfied at the
cosmological milestones. Since the classification is extremely general, and
modulo certain technical assumptions complete, the corresponding results are to
a high degree model-independent.Comment: 8 pages, 1 table, conference proceedings for NEB XII conference in
Nafplio, Greec
-singularities in cosmological models
Recently a new type of cosmological singularity has been postulated for
infinite barotropic index in the equation of state of the
cosmological fluid, but vanishing pressure and density at the singular event.
Apparently the barotropic index would be the only physical quantity to blow
up at the singularity. In this talk we would like to discuss the strength of
such singularities and compare them with other types. We show that they are
weak singularities.Comment: 4 pp, jpconf.cls, to appear in Proceedings of Spanish Relativity
Meeting 2010 (ERE 2010) held in Granada, Spai
The Hubble series: Convergence properties and redshift variables
In cosmography, cosmokinetics, and cosmology it is quite common to encounter
physical quantities expanded as a Taylor series in the cosmological redshift z.
Perhaps the most well-known exemplar of this phenomenon is the Hubble relation
between distance and redshift. However, we now have considerable high-z data
available, for instance we have supernova data at least back to redshift
z=1.75. This opens up the theoretical question as to whether or not the Hubble
series (or more generally any series expansion based on the z-redshift)
actually converges for large redshift? Based on a combination of mathematical
and physical reasoning, we argue that the radius of convergence of any series
expansion in z is less than or equal to 1, and that z-based expansions must
break down for z>1, corresponding to a universe less than half its current
size.
Furthermore, we shall argue on theoretical grounds for the utility of an
improved parameterization y=z/(1+z). In terms of the y-redshift we again argue
that the radius of convergence of any series expansion in y is less than or
equal to 1, so that y-based expansions are likely to be good all the way back
to the big bang y=1, but that y-based expansions must break down for y<-1, now
corresponding to a universe more than twice its current size.Comment: 15 pages, 2 figures, accepted for publication in Classical and
Quantum Gravit
Classical and semi-classical energy conditions
The standard energy conditions of classical general relativity are (mostly)
linear in the stress-energy tensor, and have clear physical interpretations in
terms of geodesic focussing, but suffer the significant drawback that they are
often violated by semi-classical quantum effects. In contrast, it is possible
to develop non-standard energy conditions that are intrinsically non-linear in
the stress-energy tensor, and which exhibit much better well-controlled
behaviour when semi-classical quantum effects are introduced, at the cost of a
less direct applicability to geodesic focussing. In this article we will first
review the standard energy conditions and their various limitations. (Including
the connection to the Hawking--Ellis type I, II, III, and IV classification of
stress-energy tensors). We shall then turn to the averaged, nonlinear, and
semi-classical energy conditions, and see how much can be done once
semi-classical quantum effects are included.Comment: V1: 25 pages. Draft chapter, on which the related chapter of the book
"Wormholes, Warp Drives and Energy Conditions" (to be published by Springer),
will be based. V2: typos fixed. V3: small typo fixe
Detecting the cosmic acceleration with current data
The deceleration parameter q as the diagnostic of the cosmological
accelerating expansion is investigated. By expanding the luminosity distance to
the fourth order of redshift and the so-called y-redshift in two redshift bins
and fitting the SNIa data (Union2), the marginalized likelihood distribution of
the current deceleration parameter shows that the cosmic acceleration is still
increasing, but there might be a tendency that the cosmic acceleration will
slow down in the near future. We also fit the Hubble evolution data together
with SNIa data by expanding the Hubble parameter to the third order, showing
that the present decelerating expansion is excluded within error.
Further exploration on this problem is also approached in a non-parametrization
method by directly reconstructing the deceleration parameter from the distance
modulus of SNIa, which depends neither on the validity of general relativity
nor on the content of the universe or any assumption regarding cosmological
parameters. More accurate observation datasets and more effective methods are
still in need to make a clear answer on whether the cosmic acceleration will
keep increasing or not.Comment: 20 pages, 5 figures, 3 table
How strong is the evidence for accelerated expansion?
We test the present expansion of the universe using supernova type Ia data
without making any assumptions about the matter and energy content of the
universe or about the parameterization of the deceleration parameter. We assume
the cosmological principle to apply in a strict sense. The result strongly
depends on the data set, the light-curve fitting method and the calibration of
the absolute magnitude used for the test, indicating strong systematic errors.
Nevertheless, in a spatially flat universe there is at least a 5 sigma evidence
for acceleration which drops to 1.8 sigma in an open universe.Comment: 16 pages, 3 figure
Anisotropic dark energy stars
A model of compact object coupled to inhomogeneous anisotropic dark energy is
studied. It is assumed a variable dark energy that suffers a phase transition
at a critical density. The anisotropic Lambda-Tolman-Oppenheimer-Volkoff
equations are integrated to know the structure of these objects. The anisotropy
is concentrated on a thin shell where the phase transition takes place, while
the rest of the star remains isotropic. The family of solutions obtained
depends on the coupling parameter between the dark energy and the fermion
matter. The solutions share several features in common with the gravastar
model. There is a critical coupling parameter that gives non-singular black
hole solutions. The mass-radius relations are studied as well as the internal
structure of the compact objects. The hydrodynamic stability of the models is
analyzed using a standard test from the mass-radius relation. For each
permissible value of the coupling parameter there is a maximum mass, so the
existence of black holes is unavoidable within this model.Comment: 12 pages, 6 figures, final manuscript, Accepted for publication in
Astrophysics & Space Scienc
Could the cosmic acceleration be transient? A cosmographic evaluation
A possible slowing down of the cosmic expansion is investigated through a
cosmographic approach. By expanding the luminosity distance to fourth order and
fitting the SN Ia data from the most recent compilations (Union, Constitution
and Union 2), the marginal likelihood distributions for the deceleration
parameter today suggest a recent reduction of the cosmic acceleration and
indicate that there is a considerable probability for . Also in contrast
to the prediction of the CDM model, the cosmographic
reconstruction permits a cosmic expansion history where the cosmic acceleration
could already have peaked and be presently slowing down, which would imply that
the recent accelerated expansion of the Universe is a transient phenomenon. It
is also shown that to describe a transient acceleration the luminosity distance
needs to be expanded at least to fourth order. The present cosmographic results
depend neither on the validity of general relativity nor on the matter-energy
contents of the Universe.Comment: 11 pages, 4 figures. Accepted for publication in Classical and
Quantum Gravit
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