9,552 research outputs found
Sterile neutrinos, dark matter, and resonant effects in ultra high energy regimes
Interest in light dark matter candidates has recently increased in the
literature; some of these works consider the role of additional neutrinos,
either active or sterile. Furthermore, extragalactic neutrinos have been
detected with energies higher than have ever been reported before. This opens a
new window of opportunities to the study of neutrino properties that were
unreachable up to now. We investigate how an interaction potential between
neutrinos and dark matter might induce a resonant enhancement in the
oscillation probability, an effect that may be tested with future neutrino
data.Comment: 11 pages, 2 figures, to be published in PL
The reactor antineutrino anomaly and low energy threshold neutrino experiments
Short distance reactor antineutrino experiments measure an antineutrino
spectrum a few percent lower than expected from theoretical predictions. In
this work we study the potential of low energy threshold reactor experiments in
the context of a light sterile neutrino signal. We discuss the perspectives of
the recently detected coherent elastic neutrino-nucleus scattering in future
reactor antineutrino experiments. We find that the expectations to improve the
current constraints on the mixing with sterile neutrinos are promising. We also
analyse the measurements of antineutrino scattering off electrons from short
distance reactor experiments. In this case, the statistics is not competitive
with inverse beta decay experiments, although future experiments might play a
role when compare it with the Gallium anomaly.Comment: 9 pages, 6 figures, 1 table, matches published versio
Collapse of Primordial Clouds
We present here studies of collapse of purely baryonic Population III objects
with masses ranging from to . A spherical Lagrangian
hydrodynamic code has been written to study the formation and evolution of the
primordial clouds, from the beginning of the recombination era () until the redshift when the collapse occurs. All the relevant processes
are included in the calculations, as well as, the expansion of the Universe. As
initial condition we take different values for the Hubble constant and for the
baryonic density parameter (considering however a purely baryonic Universe), as
well as different density perturbation spectra, in order to see their influence
on the behavior of the Population III objects evolution. We find, for example,
that the first mass that collapses is for ,
and with the mass scale . For
we obtain for the first
mass that collapses. The cooling-heating and photon drag processes have a key
role in the collapse of the clouds and in their thermal history. Our results
show, for example, that when we disregard the Compton cooling-heating, the
collapse of the objects with masses occurs earlier. On
the other hand, disregarding the photon drag process, the collapse occurs at a
higher redshift.Comment: 10 pages, MN plain TeX macros v1.6 file, 9 PS figures. Also available
at http://www.iagusp.usp.br/~oswaldo (click "OPTIONS" and then "ARTICLES").
MNRAS in pres
Collapse of Primordial Clouds II. The Role of Dark Matter
In this article we extend the study performed in our previous article on the
collapse of primordial objects. We here analyze the behavior of the physical
parameters for clouds ranging from to . We
studied the dynamical evolution of these clouds in two ways: purely baryonic
clouds and clouds with non-baryonic dark matter included. We start the
calculations at the beginning of the recombination era, following the evolution
of the structure until the collapse (that we defined as the time when the
density contrast of the baryonic matter is greater than ). We analyze the
behavior of the several physical parameters of the clouds (as, e.g., the
density contrast and the velocities of the baryonic matter and the dark matter)
as a function of time and radial position in the cloud. In this study all
physical processes that are relevant to the dynamical evolution of the
primordial clouds, as for example photon-drag (due to the cosmic background
radiation), hydrogen molecular production, besides the expansion of the
Universe, are included in the calculations. In particular we find that the
clouds, with dark matter, collapse at higher redshift when we compare the
results with the purely baryonic models. As a general result we find that the
distribution of the non-baryonic dark matter is more concentrated than the
baryonic one. It is important to stress that we do not take into account the
putative virialization of the non-baryonic dark matter, we just follow the time
and spatial evolution of the cloud solving its hydrodynamical equations. We
studied also the role of the cooling-heating processes in the purely baryonic
clouds.Comment: 8 pages, MN plain TeX macros v1.6 file, 13 PS figures. Also available
at http://www.iagusp.usp.br/~oswaldo (click "OPTIONS" and then "ARTICLES").
MNRAS in pres
A non-resonant dark-side solution to the solar neutrino problem
We re-analyse spin-flavour precession solutions to the solar neutrino problem
in the light of the recent SNO CC result as well as the 1258--day
Super-Kamiokande data and the upper limit on solar anti-neutrinos. In a
self-consistent magneto-hydrodynamics approach the resulting scheme has only 3
effective parameters: , and the neutrino mixing angle
. We show how a rates-only analysis for fixed slightly
favours spin-flavour precession (SFP) solutions over oscillations (OSC). In
addition to the resonant solution (RSFP for short), there is a new non-resonant
solution (NRSFP) in the ``dark-side''. Both RSFP and NRSFP lead to flat recoil
energy spectra in excellent agreement with the latest SuperKamiokande data. We
also show that in the presence of a neutrino transition magnetic moment of
Bohr magneton, a magnetic field of 80 KGauss eliminates all large
mixing solutions other than the so-called LMA solution.Comment: 12 pages, 3 postscript figures, using elsart.cls. Published versio
A COMPARATIVE STUDY FOR PROPELLER BLADE DESIGN
This work presents a comparative study between two propeller design methods for aeronautical application, with emphasis on its main element, the blade. The first method is an empirical approach based on graphical distribution of design parameters of a propeller and consists on a sequence of steps which starts from defined value for parameters like flight speed, propeller RPM, etc; with a view to obtain others dimensional parameters (diameter, twisting angle, etc) for a propeller to be used on a general aviation aircraft, with the goal to achieve certain performance target. According to the author of this method, the design of a propeller should be seen more as an art rather than exact science. The second method is well known by the aeronautical industry and called “method or theory of blade element”. This theory consider a propeller blade as a twisted wing, for which the quantities of interest to be obtained are the aerodynamics reactions, lift and drag, which are a function of the airfoil characteristics (treated as aerodynamic coefficients, cl for lift and cd for drag) for each section along blades length, twist angle, Mach, etc. For obtaining the propeller value of interest, the number of blades must also be considered. As an application for the study it was used a tri-blade propeller which equips an airplane for general aviation, that can carry 4 occupants flying at 170 Knots. The first aim of this study was to compare the results provided by the empirical method against the BET (Blade Element Theory). A secondary objective was to extend the empirical method in the design of a propeller for use on a closed circuit wind tunnel, once verified the consistency of obtained results as aimed on the first part of this study. Although the results were favorable, showing that both methods provide similar results, the study showed that the empirical method is not valid for operating and constructive conditions set for conditions like the defined for this wind tunnel, once for this type of application, the design parameters extrapolates the minimum and maximum limits established in the empirical method, providing extremely inconsistent results
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