35 research outputs found
Dynamical effects of the neutrino gravitational clustering at Planck angular scales
We study the CMB anisotropy induced by the non-linear perturbations in the
massive neutrino density associated to the non-linear gravitational clustering
proceses. Our results show that for the neutrino fraction in agreement with
that indicated by the astroparticle and nuclear physics experiments and a
cosmological accreting mass comparable with the mass of known clusters, the
angular resolution and the sensitivity of the CMB anisotropy measurements from
the Planck surveyor will allow the detection of the dynamical effects of the
neutrino gravitational clustering.Comment: 40 pages and 12 figures, submitted to ApJ (14 March 2002
On the origin of the large scale structures of the universe
We revise the statistical properties of the primordial cosmological density
anisotropies that, at the time of matter radiation equality, seeded the
gravitational development of large scale structures in the, otherwise,
homogeneous and isotropic Friedmann-Robertson-Walker flat universe. Our
analysis shows that random fluctuations of the density field at the same
instant of equality and with comoving wavelength shorter than the causal
horizon at that time can naturally account, when globally constrained to
conserve the total mass (energy) of the system, for the observed scale
invariance of the anisotropies over cosmologically large comoving volumes.
Statistical systems with similar features are generically known as glass-like
or lattice-like. Obviously, these conclusions conflict with the widely accepted
understanding of the primordial structures reported in the literature, which
requires an epoch of inflationary cosmology to precede the standard expansion
of the universe. The origin of the conflict must be found in the widespread,
but unjustified, claim that scale invariant mass (energy) anisotropies at the
instant of equality over comoving volumes of cosmological size, larger than the
causal horizon at the time, must be generated by fluctuations in the density
field with comparably large comoving wavelength.Comment: New section added; final version to appear in Physical Review D;
discussion extended and detailed with new calculations to support the claims
of the paper; statistical properties of vacuum fluctuations now discussed in
the context of FRW flat universe; new important conclussions adde
Cosmological thermodynamics and deflationary gas universe
We establish a general thermodynamic scheme for cosmic fluids with internal
self-interactions and discuss equilibrium and non-equilibrium aspects of such
systems in connection with (generalized) symmetry properties of the
cosmological dynamics. As an example we construct an exactly solvable gas
dynamical model of a ``deflationary'' transition from an initial de Sitter
phase to a subsequent Friedmann-Lema\^{\i}tre-Robertson-Walker (FLRW) period.
We demonstrate that this dynamics represents a manifestation of a conformal
symmetry of an ``optical'' metric, characterized by a specific effective
refraction index of the cosmic medium.Comment: 12 pages, to appear in PR
Growth rate of matter perturbations as a probe of large-scale magnetism
The growth rate of matter perturbations is computed in a magnetized
environment for the LambdaCDM and wCDM paradigms. It is argued that the baryons
do not necessarily follow into the dark matter potential wells after they are
released from the drag of the photons. The baryonic evolution equations inherit
a forcing term whose explicit form depends on the plasma description and can be
deduced, for instance, in the resistive magnetohydrodynamical approximation.
After deriving an analytical expression for the growth rate applicable when
dark energy does not cluster, the effects of relativistic corrections and of
the inhomogeneities associated with the other species of the plasma are taken
into account numerically. The spectral amplitudes and slopes of the stochastic
magnetic background are selected to avoid appreciable distortions in the
measured temperature and polarization anisotropies of the Cosmic Microwave
Background. The growth of structures in the current paradigms of structure
formation represents a complementary probe of large-scale magnetism in the same
way as the shape of the growth factor and the associated indices can be used,
in the conventional lore, to discriminate between competing scenarios of dark
energy or even to distinguish different models of gravity.Comment: 32 pages, 7 figures, 14 plot
Cosmological nonlinear hydrodynamics with post-Newtonian corrections
The post-Newtonian (PN) approximation, based on the assumptions of weak
gravitational fields and slow motions, provides a way to estimate general
relativistic effects in the fully nonlinear evolution stage of the large-scale
cosmic structures. We extend Chandrasekhar's first order PN (1PN) hydrodynamics
based on the Minkowski background to the Robertson-Walker background. We assume
the presence of Friedmann's cosmological spacetime as a background. In the
background we include the three-space curvature, the cosmological constant and
general pressure. In the Newtonian order and 1PN order we include general
pressure, stress, and flux. The Newtonian hydrodynamic equations appear
naturally in the 0PN order. The spatial gauge degree of freedom is fixed in a
unique manner and the basic equations are arranged without taking the temporal
gauge condition. In this way we can conveniently try alternative temporal gauge
conditions. We investigate a number of temporal gauge conditions under which
all the remaining variables are equivalently gauge-invariant. Our aim is to
present the fully nonlinear 1PN equations in a form suitable for implementation
in conventional Newtonian hydrodynamic simulations with minimal extensions. The
1PN terms can be considered as relativistic corrections added to the well known
Newtonian equations. The proper arrangement of the variables and equations in
combination with suitable gauge conditions would allow the possible future 1PN
cosmological simulations to become more tractable. Our equations and gauges are
arranged for that purpose. We suggest ways of controlling the numerical
accuracy. The typical 1PN order terms are about times
smaller than the Newtonian terms.Comment: 26 pages, no figur
Statistical characteristics of formation and evolution of structure in the universe
An approximate statistical description of the formation and evolution of
structure of the universe based on the Zel'dovich theory of gravitational
instability is proposed. It is found that the evolution of DM structure shows
features of self-similarity and the main structure characteristics can be
expressed through the parameters of initial power spectrum and cosmological
model. For the CDM-like power spectrum and suitable parameters of the
cosmological model the effective matter compression reaches the observed scales
20 -- 25Mpc with the typical mean separation of
wall-like elements 50 -- 70Mpc. This description can be
directly applied to the deep pencil beam galactic surveys and absorption
spectra of quasars. For larger 3D catalogs and simulations it can be applied to
results obtained with the core-sampling analysis.
It is shown that the interaction of large and small scale perturbations
modulates the creation rate of early Zel'dovich pancakes and generates bias on
the SLSS scale. For suitable parameters of the cosmological model and reheating
process this bias can essentially improve the characteristics of simulated
structure of the universe.
The models with give the best description of the
observed structure parameters. The influence of low mass "warm" dark matter
particles, such as a massive neutrino, will extend the acceptable range of
and .Comment: 20pages, 7 figures, MNRAS in pres
Quantum Creation of an Open Inflationary Universe
We discuss a dramatic difference between the description of the quantum
creation of an open universe using the Hartle-Hawking wave function and the
tunneling wave function. Recently Hawking and Turok have found that the
Hartle-Hawking wave function leads to a universe with Omega = 0.01, which is
much smaller that the observed value of Omega > 0.3. Galaxies in such a
universe would be about light years away from each other, so the
universe would be practically structureless. We will argue that the
Hartle-Hawking wave function does not describe the probability of the universe
creation. If one uses the tunneling wave function for the description of
creation of the universe, then in most inflationary models the universe should
have Omega = 1, which agrees with the standard expectation that inflation makes
the universe flat. The same result can be obtained in the theory of a
self-reproducing inflationary universe, independently of the issue of initial
conditions. However, there exist two classes of models where Omega may take any
value, from Omega > 1 to Omega << 1.Comment: 23 pages, 4 figures. New materials are added. In particular, we show
that boundary terms do not help to solve the problem of unacceptably small
Omega in the new model proposed by Hawking and Turok in hep-th/9803156. A
possibility to solve the cosmological constant problem in this model using
the tunneling wave function is discusse
From the Big Bang Theory to the Theory of a Stationary Universe
We consider chaotic inflation in the theories with the effective potentials
phi^n and e^{\alpha\phi}. In such theories inflationary domains containing
sufficiently large and homogeneous scalar field \phi permanently produce new
inflationary domains of a similar type. We show that under certain conditions
this process of the self-reproduction of the Universe can be described by a
stationary distribution of probability, which means that the fraction of the
physical volume of the Universe in a state with given properties (with given
values of fields, with a given density of matter, etc.) does not depend on
time, both at the stage of inflation and after it. This represents a strong
deviation of inflationary cosmology from the standard Big Bang paradigm. We
compare our approach with other approaches to quantum cosmology, and illustrate
some of the general conclusions mentioned above with the results of a computer
simulation of stochastic processes in the inflationary Universe.Comment: No changes to the file, but original figures are included. They
substantially help to understand this paper, as well as eternal inflation in
general, and what is now called the "multiverse" and the "string theory
landscape." High quality figures can be found at
http://www.stanford.edu/~alinde/LLMbigfigs
Stochastic Behavior of Effective Field Theories Across Threshold
We explore how the existence of a field with a heavy mass influences the low
energy dynamics of a quantum field with a light mass by expounding the
stochastic characters of their interactions which take on the form of
fluctuations in the number of (heavy field) particles created at the threshold,
and dissipation in the dynamics of the light fields, arising from the
backreaction of produced heavy particles. We claim that the stochastic nature
of effective field theories is intrinsic, in that dissipation and fluctuations
are present both above and below the threshold. Stochasticity builds up
exponentially quickly as the heavy threshold is approached from below, becoming
dominant once the threshold is crossed. But it also exists below the threshold
and is in principle detectable, albeit strongly suppressed at low energies. The
results derived here can be used to give a quantitative definition of the
`effectiveness' of a theory in terms of the relative weight of the
deterministic versus the stochastic behavior at different energy scales.Comment: 32 pages, Latex, no figure
A Quintessentially Geometric Model
We consider string inspired cosmology on a solitary -brane moving in the
background of a ring of branes located on a circle of radius . The motion of
the -brane transverse to the plane of the ring gives rise to a radion field
which can be mapped to a massive non-BPS Born-Infeld type field with a cosh
potential. For certain bounds of the brane tension we find an inflationary
phase is possible, with the string scale relatively close to the Planck scale.
The relevant perturbations and spectral indices are all well within the
expected observational bounds. The evolution of the universe eventually comes
to be dominated by dark energy, which we show is a late time attractor of the
model. However we also find that the equation of state is time dependent, and
will lead to late time Quintessence.Comment: 11 pages, 3 figures. References and comments adde