Abstract Objective To estimate the prevalence and comorbidity of the most common mental disorders in primary care practice in Spain, using the Primary Care Evaluation of Mental Disorders (PRIME-MD) ...questionnaire. Design A systematic sample of 7936 adult primary care patients was recruited by 1925 general practitioners in a large cross-sectional national epidemiological study. The PRIME-MD was used to diagnose psychiatric disorders. Setting 1356 primary care units proportionally distributed throughout the country. Results 53.6% of the sample presented one or more psychiatric disorder. The most prevalent were affective (35.8%), anxiety (25.6%), and somatoform (28.8%) disorders. 30.3% of the patients had more than one current mental disorder. 11.5% presented comorbidity between affective, anxiety, and somatoform disorders. Conclusions The study provides further evidence of the high prevalence and high comorbidity of mental disorders in primary care. Given the large overlap between affective, anxiety and somatoform disorders, future diagnostic classifications should reconsider the current separation between these entities.
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UL, UM, UPCLJ, UPUK
2.
Autochthonous Crimean–Congo Hemorrhagic Fever in Spain Negredo, Anabel; de la Calle-Prieto, Fernando; Palencia-Herrejón, Eduardo ...
The New England journal of medicine,
07/2017, Volume:
377, Issue:
2
Journal Article
Peer reviewed
Open access
Crimean–Congo hemorrhagic fever is a widely distributed tickborne illness. In this report, transmission in Spain is identified, increasing the geographic distribution of this pathogen.
Observations from the SABER (Sounding of the Atmosphere using Broadband Emission Radiometry) instrument on the TIMED (Thermosphere, Ionosphere, Mesosphere, Energetics and Dynamics) satellite show ...interannual variations of mesospheric ozone in the NH late winter. Ozone in the mid‐January to mid‐March period is significantly different in 2004, 2006, and 2009 than in other years (2002, 2003, 2005, 2007, 2008). The altitudes of the ozone secondary maximum (∼90–95 km), the minimum (∼80 km) and the tertiary maximum (∼72 km) are all lower by 3–5 km during the three anomalous winters. The ozone anomalies indicate enhanced downward motion and are consistent with other observations of unusual profiles of trace species. The ozone perturbations extend to at least 100 km while temperatures above 90 km are within the range found in the other years.
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FZAB, GIS, IJS, KILJ, NLZOH, NUK, OILJ, SBCE, SBMB, UL, UM, UPUK
Using a ground‐to‐exosphere general circulation model for Mars we have simulated the variability of the dayside temperatures at the exobase during eight Martian years (MY, from MY24 to MY31, ...approximately from 1998 to 2013), taking into account the observed day‐to‐day solar and dust load variability. We show that the simulated temperatures are in good agreement with the exospheric temperatures derived from Precise Orbit Determination of Mars Global Surveyor. We then study the effects of the solar variability and of two planetary‐encircling dust storms on the simulated temperatures. The seasonal effect produced by the large eccentricity of the Martian orbit translates in an aphelion‐to‐perihelion temperature contrast in every simulated year. However, the magnitude of this seasonal temperature variation is strongly affected by the solar conditions, ranging from 50 K for years corresponding to solar minimum conditions to almost 140 K during the last solar maximum. The 27 day solar rotation cycle is observed on the simulated temperatures at the exobase, with average amplitude of the temperature oscillation of 2.6 K but with a significant interannual variability. These two results highlight the importance of taking into account the solar variability when simulating the Martian upper atmosphere and likely have important implications concerning the atmospheric escape rate. We also show that the global dust storms in MY25 and MY28 have a significant effect on the simulated temperatures. In general, they increase the exospheric temperatures over the low latitude and midlatitude regions and decrease them in the polar regions.
Key Points
Eight Martian years simulated with global model including day‐to‐day variable solar flux and dust
Important effect of solar cycle and solar rotation on simulated exobase temperatures
Significant effects of planetary‐encircling dust storms on simulated exobase temperatures
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BFBNIB, FZAB, GIS, IJS, KILJ, NLZOH, NUK, OILJ, SBCE, SBMB, UL, UM, UPUK
We used temperature data from the Michelson Interferometer for Passive Atmospheric Sounding on board ESA's Envisat satellite to analyze the temperature responses in the mesosphere and thermosphere up ...to 170 km to a major stratospheric sudden warming (SSW) which occurred in January 2009. The temperature observations show clear signatures of a mesospheric cooling and a thermospheric warming, the latter peaking at 120–140 km in agreement with model predictions. From the analysis of the zonal temperature structure during the SSW a pronounced wave 1 pattern was found in the entire middle and upper polar atmosphere with maximum amplitudes around 50 and 140 km. In the mesosphere, the wave amplitude is significantly damped. The wave amplification above is most likely produced by in situ forced planetary waves in the mesosphere and lower thermosphere region. Our observations represent the first experimental evidence of a dynamical coupling of the lower atmosphere and the thermosphere in the 120–150 km range by means of satellite data.
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Jupiter's atmosphere has been sounded in transmission from the UV to the IR, as if it were a transiting exoplanet, by observing Ganymede while passing through Jupiter's shadow. The spectra show ...strong extinction due to the presence of aerosols and haze in Jupiter's atmosphere and strong absorption features of methane. Here, we report a new detailed analysis of these observations, with special emphasis on the retrievals of the vertical distribution of the aerosols and their sizes, and the properties and distribution of the stratospheric water ice. Our analysis suggests the presence of aerosols near the equator in the altitude range of 100 hPa up to at least 0.01 hPa, with a layer of small particles (mean radius of 0.1 m) in the upper part (above 0.1 hPa), an intermediate layer of aerosols with a radius of 0.3 m, extending between ∼10 and 0.01 hPa, and a layer with larger sizes of ∼0.6 m at approximately 100-1 hPa. The corresponding loads for each layer are ∼2 × 10−7 g cm−2, ∼3.4 × 10−7 g cm−2, and ∼1.5 × 10−6 g cm−2, respectively, with a total load of ∼2.0 × 10−6 g cm−2. The lower and middle layers agree well with previous measurements; but the finer particles of 0.1 m above 0.01 hPa have not been reported before. The spectra also show two broad features near 1.5 and 2.0 m, which we attribute to a layer of very small (∼10 nm) H2O crystalline ice in Jupiter's lower stratosphere (∼0.5 hPa). While these spectral signatures seem to be unequivocally attributable to crystalline water ice, they require a large amount of water ice to explain the strong absorption features.
We present a retrieval of several vibrational‐vibrational (V V) and vibrational‐thermal (V‐T) collisional rate coefficients affecting the populations of the CO2 levels emitting at 10, 4.3 and 2.7 μm ...from high‐resolution limb atmospheric spectra taken by Michelson Interferometer for Passive Atmospheric Sounding (MIPAS). This instrument has a high spectral resolution (0.0625 cm−1) and a wide spectral coverage (from 685 to 2410 cm−1) that allow measuring and discriminating among the many bands originating the atmospheric 4.3 μm radiance. Also its high sensitivity allows measuring the atmospheric limb emission in a wide altitude range, from 20 to 170 km in its middle and upper atmosphere modes, and hence obtain information on the temperature dependence of the collisional rates. In particular, we retrieve the rate coefficients and their temperature dependence in the 130–250 K range of the following processes: CO2(vd,v3)+N2⇌CO2(vd,v3−1)+N2(1) with vd=2v1+v2=2,3, and 4; CO2(v1,v2,l,1,r)+M⇌CO2(v1′,v2′,l′,1,r′)+M with Δvd=vd′−vd=0 and Δl = 0; and with Δvd=0 and Δl ≠ 0. In addition we have also retrieved the thermal relaxation of CO2(v3) into the v1 and v2 modes, e.g., CO2(vd,v3)+M⇌CO2(vd′,v3−1)+M with Δvd=2–4 and Δv3=−1 and the efficiency of the excitation of N2(1) by O(1D). All of them were retrieved with a much better accuracy than were known before. The new rates have very important effects on the atmospheric limb radiance in the 10, 4.3 and 2.7 μm spectral regions (5–8% at 4.3 μm) and allow a more accurate inversion of the CO2 volume mixing ratio in the mesosphere and lower thermosphere from measurements taken in those spectral regions.
Key Points
Crucial V‐V and V‐T rates controlling CO2 IR emission have been retrieved
These rates are very different from current values and are much more accurate
They are important for CO2 measurements in the mesosphere and lower thermosphere
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BFBNIB, FZAB, GIS, IJS, KILJ, NLZOH, NUK, OILJ, SBCE, SBMB, UL, UM, UPUK
The vast set of near‐global and continuous atmospheric measurements made by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument since 2002, including daytime and ...nighttime kinetic temperature (Tk) from 20 to 105 km, is available to the scientific community. The temperature is retrieved from SABER measurements of the atmospheric 15 μm CO2 limb emission. This emission separates from local thermodynamic equilibrium (LTE) conditions in the rarefied mesosphere and thermosphere, making it necessary to consider the CO2 vibrational state non‐LTE populations in the retrieval algorithm above 70 km. Those populations depend on kinetic parameters describing the rate at which energy exchange between atmospheric molecules take place, but some of these collisional rates are not well known. We consider current uncertainties in the rates of quenching of CO2(υ2) by N2, O2 and O, and the CO2(υ2) vibrational‐vibrational exchange to estimate their impact on SABER Tk for different atmospheric conditions. The Tk is more sensitive to the uncertainty in the latter two, and their effects depend on altitude. The Tk combined systematic error due to non‐LTE kinetic parameters does not exceed ±1.5 K below 95 km and ±4–5 K at 100 km for most latitudes and seasons (except for polar summer) if the Tk profile does not have pronounced vertical structure. The error is ±3 K at 80 km, ±6 K at 84 km and ±18 K at 100 km under the less favorable polar summer conditions. For strong temperature inversion layers, the errors reach ±3 K at 82 km and ±8 K at 90 km. This particularly affects tide amplitude estimates, with errors of up to ±3 K.
Blood pressure increases in cold periods, but its implications on prevalence of hypertension and on individual progression to hypertension remain unclear. Our aim was to develop a pre-screening test ...for identifying candidates to suffer hypertension only in cold months among non-hypertensive subjects.
We included 95,277 subjects registered on a primary care database from Girona (Catalonia, Spain), with ≥3 blood pressure measures recorded between 2003 and 2009 and distributed in both cold (October–March) and warm (April–September) periods. We defined four blood pressure patterns depending on the presence of hypertension through these periods. A Cox model determined the risk to develop vascular events associated with blood pressure patterns. A logistic regression distinguished those nonhypertensive individuals who are more prone to suffer cold-induced hypertension. Validity was assessed on the basis of calibration (using Brier score) and discrimination (using the area under the receiver operating characteristics).
In cold months, the mean systolic blood pressure increased by 3.3±0.1mmHg and prevalence of hypertension increased by 8.2%. Cold-induced hypertension patients were at higher vascular events risk (Hazard ratio=1.44 95% Confidence interval 1.15–1.81), than nonhypertensive individuals. We identified age, diabetes, body mass index and prehypertension as the major contributing factors to cold-induced hypertension onset.
Hypertension follows a seasonal pattern in some individuals. We recommend screening for hypertension during the cold months, at least in those nonhypertensive individuals identified as cold-induced hypertensive by this assessment tool.
•Some individuals might suffer hypertension only in cold months.•Seasonality of blood pressure should be considered when diagnosing hypertension.•Age >40, BMI >25kg/m2, diabetes and pre-hypertension promote cold-induced hypertension.•Cold-induced hypertensive candidates have to be screened during the cold months.
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GEOZS, IJS, IMTLJ, KILJ, KISLJ, NUK, OILJ, PNG, SAZU, SBCE, SBJE, UL, UM, UPCLJ, UPUK
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