3,648 research outputs found
Influence d'une hospitalisation prénatale sur les facteurs de stress
But.
- Investiguer l'influence d'une hospitalisation prénatale précédant une naissance préma¬turée sur les facteurs de stress parentaux et la relation parent-enfant lors de l'hospitalisation en néonatologie ainsi que sur les symptômes de stress post-traumatique parentaux.
Population et méthodes.
- Population : 51 enfants prématurés et 25 enfants nés à terme (groupe témoin). Quatre groupes : groupe témoin, prématurés sans hospitalisation prénatale, prématu¬rés avec hospitalisation courte (< 8 jours) et prématurés avec hospitalisation longue (> 8 jours). Instruments: le Parental Stressor Scale: Neonatal Intensive Care Unit (PSS: NICU, Miles et al., 1993 [14]) et le Perinatal PTSD Questionnaire (PPQ, Quinnell et Hynan, 1999 [16]).
Résultats.
-En cas d'hospitalisation prénatale, les parents se disent plus stressés par l'environnement du bébé en néonatologie. Les mères avec une hospitalisation prénatale courte (< 8 jours) se différencient significativement du groupe témoin par plus de symptômes de stress post-traumatique. Les parents présentant plus de symptômes post-traumatiques décrivent la relation avec leur bébé en néonatologie comme significativement plus difficile.
Conclusion.
- Cette étude indique l'attention à apporter aux patientes hospitalisées brièvement en prénatal (< 8 jours). Il s'agit d'un groupe plus à risque de présenter des symptômes de stress post-traumatique qui peuvent engendrer des troubles dans la relation à l'enfant
Lensing of ultra-high energy cosmic rays in turbulent magnetic fields
We consider the propagation of ultra high energy cosmic rays through
turbulent magnetic fields and study the transition between the regimes of
single and multiple images of point-like sources. The transition occurs at
energies around , where is the distance traversed by the
CR's with electric charge in the turbulent magnetic field of root mean
square strength and coherence length . We find that above only sources located in a fraction of a few % of the sky can reach large
amplifications of its principal image or start developing multiple images. New
images appear in pairs with huge magnifications, and they remain amplified over
a significant range of energies. At decreasing energies the fraction of the sky
in which sources can develop multiple images increases, reaching about 50% for
. The magnification peaks become however increasingly narrower and for
their integrated effect becomes less noticeable. If a uniform
magnetic field component is also present it would further narrow down the
peaks, shrinking the energy range in which they can be relevant. Below some kind of scintillation regime is reached, where many demagnified
images of a source are present but with overall total magnification of order
unity. We also search for lensing signatures in the AGASA data studying
two-dimensional correlations in angle and energy and find some interesting
hints.Comment: 30 pages, 16 figures, final version with minor change
Ultrahigh Energy Nuclei in the Galactic Magnetic Field
Observations are consistent with a significant fraction of heavy nuclei in
the cosmic ray flux above a few times 10^19 eV. Such nuclei can be deflected
considerably in the Galactic magnetic field, with important implications for
the search of their sources. We perform detailed simulations of heavy nuclei
propagation within recent Galactic magnetic field models. While such models are
not yet sufficiently constrained to predict deflection maps in detail, we find
general features of the distribution of (de-) magnified flux from sources.
Since in most theoretical models sources of heavy nuclei are located in the
local large scale structure of galaxies, we show examples of images of several
nearby galaxy clusters and of the supergalactic plane. Such general features
may be useful to develop efficient methods for source reconstruction from
observed ultrahigh energy cosmic ray arrival directions.Comment: 17 pages, 11 figures. Published in JCA
Ultrahigh Energy Nuclei in the Turbulent Galactic Magnetic Field
In this work we study how the turbulent component of the Galactic magnetic
field (GMF) affects the propagation of ultrahigh energy heavy nuclei. We
investigate first how the images of individual sources and of the supergalactic
plane depend on the properties of the turbulent GMF. Then we present a
quantitative study of the impact of the turbulent field on (de-) magnification
of source fluxes, due to magnetic lensing effects. We also show that it is
impossible to explain the Pierre Auger data assuming that all ultrahigh energy
nuclei are coming from Cen A, even in the most favorable case of a strong,
extended turbulent field in the Galactic halo.Comment: 10 pages (2 columns), 8 figures. Published in Astroparticle Physic
Decaying neutron propagation in the Galaxy and the Cosmic Ray anisotropy at 1 EeV
We study the cosmic ray arrival distribution expected from a source of
neutrons in the galactic center at energies around 1 EeV and compare it with
the anisotropy detected by AGASA and SUGAR. Besides the point-like signal in
the source direction produced by the direct neutrons, an extended signal due to
the protons produced in neutron decays is expected. This associated proton
signal also leads to an excess in the direction of the spiral arm. For
realistic models of the regular and random galactic magnetic fields, the
resulting anisotropy as a function of the energy is obtained. We find that for
the anisotropy to become sufficiently suppressed below E\sim 10^{17.9}eV, a
significant random magnetic field component is required, while on the other
hand, this also tends to increase the angular spread of the associated proton
signal and to reduce the excess in the spiral arm direction. The source
luminosity required in order that the right ascension anisotropy be 4% for the
AGASA angular exposure corresponds to a prediction for the point-like flux from
direct neutrons compatible with the flux detected by SUGAR. We also analyse the
distinguishing features predicted for a large statistics southern observatory.Comment: 14 pages, 6 figures, minor changes to match published versio
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