Suchergebnisse

Introduction: Intestinal
obstruction (IO) due to postoperative adhesions is an
important cause of hospital admissions worldwide, with
signifi cant morbidity and mortality that represent great
costs for health systems worldwide. Objective: To estimate
the incidence of intestinal obstruction due to
postoperative adhesions and to identify risk factors in
patients admitted to the General Surgery Service of the
Central Military Hospital (CMH). Material and methods: The
database of admitted patients to the CMH was revised from
January 2009 to December 2013. Of the 14,769 surgeries
performed, 393 patients presented intestinal obstruction.
The demographic characteristics, type and number of
previous surgeries and other risk factors for adhesions
were identifi ed. Each patient was classified as IO by
adhesions (IOA) or as IO associated with another pathology
(IOP). Results: The overall incidence of post-surgical IO
was 2.7%; 236 cases (1.6%) were secondary to surgical
adhesions and the rest (1.1%) were associated with other
pathology. Morbidity occurred in 8.5% of the IOA patients
versus 13.5% of the IOP group (p = 0.118). Mortality was
6.4 versus 12.1%, respectively (p < 0.05). Laparotomy
(34%), cholecystectomy (22%) and appendectomy (19%) were
the surgeries most frequently associated with obstruction.
Surgical treatment was done in 20% of the patients of the
IOA group, versus 43% in the IOP group (p = 0.001). Risk
factors associated to IOA were: female patients, number of
previous abdominal surgeries and past admissions for
intestinal obstruction. Conclusions: Intestinal obstruction
syndrome due to post-surgical adhesions was the most common
cause of IO from 2009 to 2013 in the Central Military
Hospital. The incidence of this post-surgical adhesion
syndrome is similar to that reported in world literature.
Therapeutic decision oriented toward an initial
conservative treatment should be correct. There were fewer
hospitalization days and less mortality in the adhesion
group treated without surgery.

A publisher correction to this article was published on 17 April 2019 ; Global dust storms on Mars are rare1,2 but can affect the Martian atmosphere for several months. They can cause changes in atmospheric dynamics and inflation of the atmosphere3, primarily owing to solar heating of the dust3. In turn, changes in atmospheric dynamics can affect the distribution of atmospheric water vapour, with potential implications for the atmospheric photochemistry and climate on Mars4. Recent observations of the water vapour abundance in the Martian atmosphere during dust storm conditions revealed a high-altitude increase in atmospheric water vapour that was more pronounced at high northern latitudes5,6, as well as a decrease in the water column at low latitudes7,8. Here we present concurrent, high-resolution measurements of dust, water and semiheavy water (HDO) at the onset of a global dust storm, obtained by the NOMAD and ACS instruments onboard the ExoMars Trace Gas Orbiter. We report the vertical distribution of the HDO/H2O ratio (D/H) from the planetary boundary layer up to an altitude of 80 kilometres. Our findings suggest that before the onset of the dust storm, HDO abundances were reduced to levels below detectability at altitudes above 40 kilometres. This decrease in HDO coincided with the presence of water-ice clouds. During the storm, an increase in the abundance of H2O and HDO was observed at altitudes between 40 and 80 kilometres. We propose that these increased abundances may be the result of warmer temperatures during the dust storm causing stronger atmospheric circulation and preventing ice cloud formation, which may confine water vapour to lower altitudes through gravitational fall and subsequent sublimation of ice crystals3. The observed changes in H2O and HDO abundance occurred within a few days during the development of the dust storm, suggesting a fast impact of dust storms on the Martian atmosphere. © 2019, The Author(s), under exclusive licence to Springer Nature Limited. ; This project acknowledges funding by the Belgian Science Policy Office (BELSPO), with financial and contractual coordination by the ESA Prodex Office (PEA 4000103401, 4000121493); by the Spanish MICINN through its Plan Nacional and by European funds under grants ESP2015-65064-C2-1-P and ESP2017-87143-R (MINECO/FEDER); by the UK Space Agency through grants ST/R005761/1, ST/P001262/1, ST/R001405/1, ST/S00145X/1, ST/R001367/1, ST/P001572/1 and ST/R001502/1; and the Italian Space Agency through grant 2018-2-HH.0. The IAA/CSIC team acknowledges financial support from the State Agency for Research of the Spanish MCIU through the 'Center of Excellence Severo Ochoa' award for the Instituto de Astrofisica de Andalucia (SEV-2017-0709). This work was supported by the Belgian Fonds de la Recherche Scientifique - FNRS under grant number 30442502 (ET_HOME). The ACS experiment is led by IKI, Space Research Institute in Moscow, assisted by LATMOS in France. The project acknowledges funding by Roscosmos and CNES. The science operations of ACS are funded by Roscosmos and ESA. IKI affiliates acknowledge funding under grant number 14.W03.31.0017 and contract number 0120.0 602993 (0028-2014-0004) of the Russian government. ; Peer Reviewed

NOMAD (Nadir and Occultation for MArs Discovery) is one of the four instruments on board the ExoMars Trace Gas Orbiter, scheduled for launch in March 2016. It consists of a suite of three high-resolution spectrometers - SO (Solar Occultation), LNO (Limb, Nadir and Occultation) and UVIS (Ultraviolet and Visible Spectrometer). Based upon the characteristics of the channels and the values of Signal-to-Noise Ratio obtained from radiometric models discussed in (Vandaele et al., 2015a, 2015b; Thomas et al., 2016), the expected performances of the instrument in terms of sensitivity to detection have been investigated. The analysis led to the determination of detection limits for 18 molecules, namely CO, HO, HDO, CH, CH, CH, HCO, CH, SO, HS, HCl, HCN, HO, NH, NO, NO, OCS, O. NOMAD should have the ability to measure methane concentrations Inter-university Attraction Poles> programme financed by the Belgian Government (Planet TOPERS no P7-15) and a BRAIN Research Grant BR/143/A2/SCOOP. The research leading to these results has received funding from the European Community's Seventh Framework Programme (FP7/2007-2013) under Grant Agreement no. 607177 CrossDrive. UK funding is acknowledged under the UK Space Agency Grant ST/I003061/1. ; Peer Reviewed