1,053 research outputs found
Failure mode and effect analysis in interhospital transport of critically ill patients: a tool to design checklists for handovers in the mobile intensive care unit
Measurement properties of Patient-Reported Outcome Measures in patients with a tibial shaft fracture; validation study alongside the multicenter TRAVEL study
A systematic review on intra-abdominal pressure in severely burned patients
Objective Intra-abdominal hypertension (IAH) and abdominal compartment syndrome (ACS) are complications that may occur in severely burned patients. Evidenced based medicine for these patients is in its early development. The aim of this study was to provide an overview of literature regarding IAH and ACS in severely burned patients. Methods A systematic search was performed in Cochrane Central Register of Controlled Trials, PubMed, Embase, Web of Science and CINAHL on October 1, 2012. These databases were searched on 'burn', 'intra-abdominal hypertension', 'abdominal compartment syndrome', synonyms and abbreviations. Studies reporting original data on mortality, abdominal decompression or abdominal pressure related complications were included. Results Fifty publications met the criteria, reporting 1616 patients. The prevalence of ACS and IAH in severely burned patients is 4.1-16.6% and 64.7-74.5%, respectively. The mean mortality rate for ACS in burn patients is 74.8%. The use of plasma and hypertonic lactated resuscitation may prevent IAH or ACS. Despite colloids decrease resuscitation volume needs, no benefit in preventing IAH was proven. Escharotomy, peritoneal catheter drainage, and decompression laparotomy are effective intra-abdominal pressure (IAP) diminishing treatments in burn patients. Markers for IAP-related organ damage might be superior to IAP measurement itself. Conclusion ACS and IAH are frequently seen devastating complications in already severely injured burn patients. Prevention is challenging but can be achieved by improving fluid resuscitation strategies. Surgical decompression measures are effective and often unavoidable. Timing is essential since decompression should prevent progression to ACS rather than limit its effects. Prognosis of ACS remains poor, but options for care improvement are available in literature
Dusty tails of evaporating exoplanets. II. Physical modelling of the KIC 12557548b light curve
Evaporating rocky exoplanets, such as KIC 12557548b, eject large amounts of
dust grains, which can trail the planet in a comet-like tail. When such objects
occult their host star, the resulting transit signal contains information about
the dust in the tail. We aim to use the detailed shape of the Kepler light
curve of KIC 12557548b to constrain the size and composition of the dust grains
that make up the tail, as well as the mass loss rate of the planet. Using a
self-consistent numerical model of the dust dynamics and sublimation, we
calculate the shape of the tail by following dust grains from their ejection
from the planet to their destruction due to sublimation. From this dust cloud
shape, we generate synthetic light curves (incorporating the effects of
extinction and angle-dependent scattering), which are then compared with the
phase-folded Kepler light curve. We explore the free-parameter space thoroughly
using a Markov chain Monte Carlo method. Our physics-based model is capable of
reproducing the observed light curve in detail. Good fits are found for initial
grain sizes between 0.2 and 5.6 micron and dust mass loss rates of 0.6 to 15.6
M_earth/Gyr (2-sigma ranges). We find that only certain combinations of
material parameters yield the correct tail length. These constraints are
consistent with dust made of corundum (Al2O3), but do not agree with a range of
carbonaceous, silicate, or iron compositions. Using a detailed, physically
motivated model, it is possible to constrain the composition of the dust in the
tails of evaporating rocky exoplanets. This provides a unique opportunity to
probe to interior composition of the smallest known exoplanets.Comment: 18 pages, 11 figures, A&A accepte
A Health Technology Assessment of Hyperthermic Intraperitoneal Chemotherapy Added to Interval Cytoreductive Surgery in Stage III Ovarian Cancer
Filaments in observed and mock galaxy catalogues
Context. The main feature of the spatial large-scale galaxy distribution is
an intricate network of galaxy filaments. Although many attempts have been made
to quantify this network, there is no unique and satisfactory recipe for that
yet. Aims. The present paper compares the filaments in the real data and in the
numerical models, to see if our best models reproduce statistically the
filamentary network of galaxies. Methods. We apply an object point process with
interactions (the Bisous process) to trace and describe the filamentary network
both in the observed samples (the 2dFGRS catalogue) and in the numerical models
that have been prepared to mimic the data.We compare the networks. Results. We
find that the properties of filaments in numerical models (mock samples) have a
large variance. A few mock samples display filaments that resemble the observed
filaments, but usually the model filaments are much shorter and do not form an
extended network. Conclusions. We conclude that although we can build numerical
models that are similar to observations in many respects, they may fail yet to
explain the filamentary structure seen in the data. The Bisous-built filaments
are a good test for such a structure.Comment: 13 pages, accepted for publication in Astronomy and Astrophysic
Luminosity- and morphology-dependent clustering of galaxies
How does the clustering of galaxies depend on their inner properties like
morphological type and luminosity? We address this question in the mathematical
framework of marked point processes and clarify the notion of luminosity and
morphological segregation. A number of test quantities such as conditional
mark-weighted two-point correlation functions are introduced. These descriptors
allow for a scale-dependent analysis of luminosity and morphology segregation.
Moreover, they break the degeneracy between an inhomogeneous fractal point set
and actual present luminosity segregation. Using the Southern Sky Redshift
Survey~2 (da Costa et al. 1998, SSRS2) we find both luminosity and
morphological segregation at a high level of significance, confirming claims by
previous works using these data (Benoist et al. 1996, Willmer et al. 1998).
Specifically, the average luminosity and the fluctuations in the luminosity of
pairs of galaxies are enhanced out to separations of 15Mpc/h. On scales smaller
than 3Mpc/h the luminosities on galaxy pairs show a tight correlation. A
comparison with the random-field model indicates that galaxy luminosities
depend on the spatial distribution and galaxy-galaxy interactions. Early-type
galaxies are also more strongly correlated, indicating morphological
segregation. The galaxies in the PSCz catalog (Saunders et al. 2000) do not
show significant luminosity segregation. This again illustrates that mainly
early-type galaxies contribute to luminosity segregation. However, based on
several independent investigations we show that the observed luminosity
segregation can not be explained by the morphology-density relation alone.Comment: aastex, emulateapj5, 20 pages, 13 figures, several clarifying
comments added, ApJ accepte
Effects of disclosing sponsored content in blogs:how the use of resistance strategies mediates effects on persuasion
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