bluuebunny/crossref_metadata_2025_split huggingface dataset:
Загальноклінічні чинники розвитку геморагічних подій і застосування міжнародних балових систем для їх прогнозування за гострого коронарного синдрому
Authors: Mishcheniuk O. Y. , Kostiukevych O. M. , Benkovska L. K. 
Published: November 2018

Мета – визначення предиктивної ефективності щодо розвитку геморагічних ускладнень (ГУ) за гострого коронарного синдрому (ГКС) загальноклінічних характеристик хворих і міжнародних бальних систем.
Матеріал і методи. Проаналізовано загальноклінічні, клініко-лабораторні дані 93 пацієнтів із ГКС, які лікувались у ДНУ «НПЦ ПКМ» ДУС 2016-2017 роками. Загальну предиктивну потужність показників (ЗП) оцінювали за допомогою ROC-аналізу з визначенням площі під кривими (ППК). Методи: загальноклінічні, клініко-лабораторні, статистичні.
Результати. Геморагічні ускладнення виникали у 21 з 93 (22,5%) хворих із ГКС. З метою оцінки ймовірності ГУ на тлі лікування ГКС рекомендовано враховувати наявність анемії (ППК=0,79; 95% ДІ 0,69-0,86; p<0,0001), віку понад 75 років (ППК=0,76; 95% ДІ 0,66-0,84; p=0,0001), застосування потрійної антитромботичної терапії – ПРАТ (ППК=0,87; 95% ДІ 0,73-0,93; p<0,0001). Поміж проаналізованих балових систем найвищу ЗП виявлено для REPLACE (ППК=0,88; 95% ДІ 0,80-0,94; р<0,0001) та ACUITY (ППК=0,83; 95% ДІ 0,74-0,90; р<0,0001), які мають «дуже добрий» показник ефективності. Рівень ефективності систем CRUSADE (ППК=0,78; 95% ДІ 0,65-0,88; р=0,0003) і RISK-PCI (ППК=0,73; 95% ДІ 0,57-0,86; р=0,0023) виявився «добрим».
Висновки. З метою прогнозування розвитку ГУ на тлі ГКС рекомендовано враховувати наявність анемії, віку понад 75 років і ПРАТ. Найбільший рівень ЗП щодо прогнозування виникнення ГУ розраховано для систем REPLACE та ACUITY, які мають «дуже добру» ефективність.
Peculiarities of 24 hour ambulatory blood pressure monitoring indices in patients with essential hypertension, stage II of different age groups
Authors: Pasko V. S. 
Published: November 2018

The aim of the study was to determine peculiarities of 24 hour ambulatory blood pressure monitoring indices of patients with essential hypertension, stage II of different age groups.
Material and methods. Indices of ambulatory blood pressure monitoring were identified in 57 middle-aged patients (45-59 years) (group I) and 43 elderly patients (60-74 years) (group II), who underwent two-week in-patient treatment. The control group consisted of 15 patients for every of the surveyed categories (group III - middle-aged and group IV – elderly respectively) matched with basic by age and gender.
Results. We have shown that one of the factors that determines the change in hemodynamics in patients with essential hypertension is age, with the age patients experience the decrease in diastolic blood pressure with steadily increased systolic blood pressure, that should be considered in the prescription of antihypertensive treatment. With age, a gradual increase in systolic blood pressure is associated with the increased aortic stiffness, partially with the increase in collagen and the decrease in elastic fibrils and the formation of isolated systolic hypertension. Thus, it is proved that in the formation of isolated hypertension the growth of pulse blood pressure for more than 60 mm Hg is unfavorable in a development of cerebrovascular events. Pulse arterial blood pressure was stronger risk factor than systolic blood pressure and diastolic blood pressure or average arterial pressure in the elderly. Recently, taking into account age characteristics, all three indices were recognized as comparable predictors at the age of 50-59 years as the transitional period, and at the age of 60-79 years diastolic blood pressure adversely affecting the cardiovascular risk, increased pulse blood pressure prognostically above the level of systolic arterial pressure.
FORMATION IN THE EARLY ADOLESCENCE OF THE WILLINGNESS TO ENSURE PERSONAL CYBERSECURITY
Authors: Chernova E. V. , Dokolin A. S. , Gavrilova I. V. 
Published: November 2018

The current stage of education development in the Russian Federation is characterized by early inclusion of children and adolescents in the information space, to resist the negative information impact of which they are often not ready. In spite of the fact that the formation of a person capable of ensuring resistance to cyber threats is an urgent need for school education, actively involving the student in the digital information environment, at the moment the lack of effective pedagogical cures of this problem is observed. This paper describes an experiment on the formation of younger adolescence schoolchildren readiness to ensure personal cybersecurity on the basis of the technique developed by authors affecting mainly extracurricular activities for young adolescents. Results of an experiment have confirmed efficiency of the developed pedagogical cures of the studied problem. Thus, authors managed to create a technique which can be recommended for work with school students of early teenage age which analogs don’t exist.
ANALYSIS OF LUMBO-SACRAL DISC PROLAPSE NEUROSURGICAL INTERVENTION
Authors: Neamah Mustafa Jarullah , Ali Liwa Abdullah , Nema Ihssan S. 
Published: November 2018

Background: Low back pain is a common cause of pain and there are many causes. Finding the exact cause of the pain can help guide treatment and management.
Objective: To evaluate the clinical presentation, diagnosis and surgical outcome of the treated patients with lumbar-disc prolapse.
Patients and Methods: Patients selection done using neuroimagings like plain radiographs and MRI Scan of lumbosacral spine. The surgical procedures applied were laminectomy, foraminatomy and evacuation of herniated disc material. Patients were analyzed postoperatively for outcome according to the symptoms resolved after surgery, objective clinical examinations and imaging studies.
Results: Fifty five patients, 25 (45%) males and 30 (55%) females. Predominant clinical presentation were low back pain with radiation to leg 36(65.4%), neurogenic claudication in 15 patients (27%), and neurological deficit (foot drop) 4 about (7.2%). Seventy four percent (about 41) of the herniated disc were found at L4 L5 and L5 SI levels. Rate of complications were 12.7% (about 7) with 4 cases infections and 3 with dural tear repaired intraopertively being commonest. Excellent to good surgical outcome were found in 90% (about 50) of the cases.
Conclusion: The results of the study depend mainly on selection of patients. Traditional laminectomy and discectomy still play a benefit for major group of patients. Foraminatomy, opening of roots foramen adds a benefit for the results.
Keywords: Laminectomy, MRI, disc, prolapse.
HUBUNGAN UMUR DAN STATUS GIZI DENGAN KADAR GULA DARAH PENDERITA DIABETES MELITUS TIPE II
Authors: Masruroh Eny - 
Published: November 2018

Diabetes Melitus (DM) tipe II merupakan tipe yang paling banyak ditemukan. DM tipe II dapat meningkat secara signifikan seiring perubahan gaya hidup masyarakat dan peningkatan umur lebih dari 40 tahun serta masalah obesitas, ditandai dengan adanya peningkatan indeks massa tubuh (IMT) ≥ 25 Kg/m2. IMT yang berlebih dapat menyebabkan kadar gula darah meningkat karena tubuh menjadi resisten terhadap insulin. Penelitian ini untuk mengetahui hubungan umur dan status gizi berdasarkan IMT dengan kadar gula darah pada penderita DM tipe II di Poli Penyakit Dalam RSUD dr. Iskak Tulungagung.Pengambilan data dilakukan pada tanggal 19-20 April 2017. Desain penelitian menggunakan analitik korelasional. Populasi seluruh penderita DM tipe II di Poli Penyakit Dalam RSUD dr. Iskak Tulungagung menggunakan teknik Quota Sampling dengan 30 responden. Pengambilan data variabel IMT menggunakan timbangan injak dan mikrotoa. Sedangkan variabel kadar gula darah menggunakan glucotest stick. Kemudian data dianalisis dengan uji statistik paired t test. Hasil penelitian ini rata-rata umur adalah 57 tahun, rata-rata IMT 25,77 Kg/m2 dengan rata-rata kadar gula darah 213,23 mg/dL. Dari hasil uji statistik menunjukkan ada hubungan antara umur dengan kadar gula darah dengan ditunjukkan p value = 0.00.begitu juga pada hasil uji status gizi dengan kadar gula darah pada penderita DM tipe II di Poli Penyakit Dalam RSUD dr. Iskak Tulungagung yang ditunjukkan dengan nilai p value = 0,000 yang berarti ada korelasi antara keduanya. Berdasarkan penelitian, yaitu ada hubungan antara umur dan status gizi dengan kadar gula darah maka disarankan bagi responden dengan IMT berlebih dapat mempertahankan berat badan yang ideal dan pada penderita DM tipe II pada umur lebih dari 40 tahun lebih menjaga pola hidup yang sehat sehingga dapat mencegah komplikasi diabetes akibat kadar gula darah yang tinggi.;
Mid-infrared Spectroscopic Observations of Comet 17P/Holmes Immediately After Its Great Outburst in 2007 October
Authors: Shinnaka Yoshiharu , Ootsubo Takafumi , Kawakita Hideyo , Yamaguchi Mitsuru , Honda Mitsuhiko , Watanabe Jun-ichi 
Published: November 2018

Abstract
Dust grains of crystalline silicate, which are rarely present in interstellar space, were found in cometary nuclei. These crystalline silicates are thought to have formed by annealing of amorphous silicate grains or direct condensation of gaseous materials near the Sun in the solar nebula (SN), and incorporated into cometary nuclei in the cold comet-forming region after radial transportation of grains in the SN. Abundances of the crystalline silicate dust grains were therefore expected to be smaller farther from the Sun. We aim to better understand the formation mechanism of minerals incorporated into comet 17P/Holmes based on its mineral abundances. To derive the mineral composition of comet 17P/Holmes, we applied a thermal emission model for cometary dust grains to mid-infrared spectra of comet 17P/Holmes taken with the Cooled Mid-Infrared Camera and Spectrograph mounted on the Subaru Telescope a few days later the great outburst in 2007 October. The resulting mass fraction of crystalline silicate, f
cry, and an olivine-to-pyroxene abundance ratio, f
OP, are f
cry = 0.31 ± 0.03 and f
OP = 1.20+0.16/−0.12, respectively. Based on a simple consideration of the mixing of dust grains originating in both the interstellar medium and SN, the minerals of 17P/Holmes formed by nonequilibrium condensation. This result is consistent with theoretical and experimental predictions for vaporization and condensation of olivine in the SN.
A First Catalog of Variable Stars Measured by the Asteroid Terrestrial-impact Last Alert System (ATLAS)
Authors: Heinze A. N. , Tonry J. L. , Denneau L. , Flewelling H. , Stalder B. , Rest A. , Smith K. W. , Smartt S. J. , Weiland H. 
Published: November 2018

Abstract
The Asteroid Terrestrial-impact Last Alert System (ATLAS) carries out its primary planetary defense mission by surveying about 13,000 deg2 at least four times per night. The resulting data set is useful for the discovery of variable stars to a magnitude limit fainter than r ∼ 18, with amplitudes down to 0.02 mag for bright objects. Here, we present a Data Release One catalog of variable stars based on analyzing the light curves of 142 million stars that were measured at least 100 times in the first two years of ATLAS operations. Using a Lomb–Scargle periodogram and other variability metrics, we identify 4.7 million candidate variables. Through the Space Telescope Science Institute, we publicly release light curves for all of them, together with a vector of 169 classification features for each star. We do this at the level of unconfirmed candidate variables in order to provide the community with a large set of homogeneously analyzed photometry and to avoid pre-judging which types of objects others may find most interesting. We use machine learning to classify the candidates into 15 different broad categories based on light-curve morphology. About 10% (427,000 stars) pass extensive tests designed to screen out spurious variability detections: we label these as “probable” variables. Of these, 214,000 receive specific classifications as eclipsing binaries, pulsating, Mira-type, or sinusoidal variables: these are the “classified” variables. New discoveries among the probable variables number 315,000, while 141,000 of the classified variables are new, including about 10,400 pulsating variables, 2060 Mira stars, and 74,700 eclipsing binaries.
Speckle Interferometry at the U.S. Naval Observatory. XXIII.
Authors: Mason Brian D. , Hartkopf William I. , Urban Sean E. , Josties Jordan D. 
Published: November 2018

Abstract
The results of 3989 intensified CCD observations of double stars, made with the 26-inch refractor of the U.S. Naval Observatory, are presented. Each observation of a system represents a combination of over 2000 short-exposure images. These observations are averaged into 1911 mean relative positions and range in separation from 0.″289 to 128.″638, with a median separation of 8.″669. Four orbits are improved. This is the 23rd in this series of papers and covers the period 2017 January 4 through 2017 September 13.
A More Informative Map: Inverting Thermal Orbital Phase and Eclipse Light Curves of Exoplanets
Authors: Rauscher Emily , Suri Veenu , Cowan Nicolas B. 
Published: November 2018

Abstract
Only one exoplanet has so far been mapped in both longitude and latitude, but the James Webb Space Telescope should provide mapping-quality data for dozens of exoplanets. The thermal phase mapping problem has previously been solved analytically, with orthogonal maps (spherical harmonics) yielding orthogonal light curves (sinusoids). The eclipse mapping problem, let alone combined phase+eclipse mapping, does not lend itself to such a neat solution. Previous efforts have adopted either spherical harmonics or various ad hoc map parameterizations, none of which produce orthogonal light curves. We use principal component analysis to construct orthogonal “eigencurves,” which we then use to fit published 8 μm observations of the hot Jupiter HD 189733b. This approach has a few advantages over previously used techniques: (1) the light curves can be precomputed, accelerating the fitting process, (2) the eigencurves are orthogonal to each other, reducing parameter correlations, and (3) the eigencurves are model-independent and are ranked in order of sensitivity. One notable result of our analysis is that eclipse-only mapping of HD 189733b is far more sensitive to the central concentration of dayside flux than to the eastward offset of that hot spot. Mapping can, in principle, suffer from degeneracies between spatial patterns and orbital parameters. Previous mapping efforts using these data have either assumed a circular orbit and precise inclination, or have been pessimistic about the prospects of eclipse mapping in the face of uncertain orbital parameters. We show that for HD 189733b the combined photometry and radial velocity are sufficiently precise to retire this concern. Lastly, we present the first map of brightness temperature, and we quantify the amplitude and longitude offset of the dayside hot spot.
Electron Acceleration and Jet-facilitated Escape in an M-class Solar Flare on 2002 August 19
Authors: Glesener Lindsay , Fleishman Gregory D. 
Published: November 2018

Abstract
Sudden jets of collimated plasma arise from many locations on the Sun, including active regions. The magnetic field along which a jet emerges is often open to interplanetary space, offering a clear “escape route” for any flare-accelerated electrons, making jets lucrative targets for studying particle acceleration and the solar sources of transient heliospheric events. Bremsstrahlung hard X-rays (HXRs) could, in principle, trace the accelerated electrons that escape along the paths of the jets, but measurements of the escaping electron beams are customarily difficult due to the low densities of the corona. In this work, we augment HXR observations with gyrosynchrotron emission observed in microwaves, as well as extreme ultraviolet (EUV) emission and modeling to investigate flare-accelerated electrons in a coronal jet. HXR and microwave data from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the Owens Valley Solar Array (OVSA), respectively, give complementary insight into electron spectra and locations, including the presence of accelerated electrons in the jet itself. High-time-resolution HXR data from the Konus-Wind instrument suggest electron acceleration timescales on the order of 1 s or shorter. We model the energetic electron distributions in the GX Simulator framework using the Solar and Heliospheric Observatory (SOHO)/Michelson Doppler Imager (MDI), the Transition Region and Coronal Explorer (TRACE), RHESSI, and OVSA data as constraints. The result is a modeled distribution, informed and constrained by measurements, of accelerated electrons as they escape the Sun. Combining the detection of microwave gyrosynchrotron emission from an open, rather than closed, magnetic configuration, with realistic 3D modeling constrained by magnetograms, EUV, and X-ray emission, we obtain the most stringent constraints to date on the accelerated electrons within a solar jet.
HAZMAT. IV. Flares and Superflares on Young M Stars in the Far Ultraviolet*
Authors: Parke Loyd R. O. , Shkolnik Evgenya L. , Schneider Adam C. , Barman Travis S. , Meadows Victoria S. , Pagano Isabella , Peacock Sarah 
Published: November 2018

Abstract
M stars are powerful emitters of far-ultraviolet light. Over long timescales, a significant, possibly dominant, fraction of this emission is produced by stellar flares. Characterizing this emission is critical to understanding the atmospheres of the stars producing it and the atmospheric evolution of the orbiting planets subjected to it. Ultraviolet emission is known to be elevated for several hundred million years after M stars form. Whether or not the same is true of ultraviolet flare activity is a key concern for the evolution of exoplanet atmospheres. Hubble Space Telescope (HST) observations by the HAZMAT program (HAbitable Zones and M dwarf Activity across Time) detected 18 flares on young (40 Myr) early M stars in the Tucana–Horologium association over 10 hr of observations, 10 having energy >1030 erg. These imply that flares on young M stars are 100–1000× more energetic than those occurring at the same rate on “inactive,” field age M dwarfs. However, when energies are normalized by quiescent emission, there is no statistical difference between the young and field age samples. The most energetic flare observed, dubbed the “Hazflare,” emitted an energy of 1032.1 erg in the FUV, 30× more energetic than any stellar flare previously observed in the FUV with HST’s COS or STIS spectrographs. It was accompanied by 15,500 ± 400 K blackbody emission bright enough to designate it as a superflare (E > 1033 erg), with an estimated bolometric energy of

erg. This blackbody emitted

% of its flux in the FUV (912–1700 Å), where molecules are generally most sensitive to photolysis. Such hot superflares in young, early M stars could play an important role in the evolution of nascent planetary atmospheres.
Magnetic Field Uniformity Across the GF 9-2 YSO, L1082C Dense Core, and GF 9 Filamentary Dark Cloud
Authors: Clemens Dan P. , El-Batal A. M. , Cerny C. , Kressy S. , Schroeder G. , Pillai T. 
Published: November 2018

Abstract
The orientation of the magnetic field (B field) in the filamentary dark cloud GF 9 was traced from the periphery of the cloud into the L1082C dense core that contains the low-mass, low-luminosity Class 0 young stellar object (YSO) GF 9-2 (IRAS 20503+6006). This was done using SOFIA HAWC+ dust thermal emission polarimetry (TEP) at 216 μm in combination with Mimir near-infrared background starlight polarimetry (BSP) conducted in the H band (1.6 μm) and K band (2.2 μm). These observations were augmented with published I-band (0.77 μm) BSP and Planck 850 μm TEP to probe B-field orientations with offset from the YSO in a range spanning 6000 au to 3 pc. No strong B-field orientation change with offset was found, indicating remarkable uniformity of the B-field from the cloud edge to the YSO environs. This finding disagrees with weak-field models of cloud core and YSO formation. The continuity of inferred B-field orientations for both TEP and BSP probes is strong evidence that both are sampling a common B field that uniformly threads the cloud, core, and YSO region. Bayesian analysis of Gaia DR2 stars matched to the Mimir BSP stars finds a distance to GF 9 of 270 ± 10 pc. No strong wavelength dependence of B-field orientation angle was found, contrary to previous claims.
Evolved Climates and Observational Discriminants for the TRAPPIST-1 Planetary System
Authors: Lincowski Andrew P. , Meadows Victoria S. , Crisp David , Robinson Tyler D. , Luger Rodrigo , Lustig-Yaeger Jacob , Arney Giada N. 
Published: November 2018

Abstract
The TRAPPIST-1 planetary system provides an unprecedented opportunity to study terrestrial exoplanet evolution with the James Webb Space Telescope (JWST) and ground-based observatories. Since M dwarf planets likely experience extreme volatile loss, the TRAPPIST-1 planets may have highly evolved, possibly uninhabitable atmospheres. We used a versatile, 1D terrestrial planet climate model with line-by-line radiative transfer and mixing length convection (VPL Climate) coupled to a terrestrial photochemistry model to simulate environmental states for the TRAPPIST-1 planets. We present equilibrium climates with self-consistent atmospheric compositions and observational discriminants of postrunaway, desiccated, 10–100 bar O2- and CO2-dominated atmospheres, including interior outgassing, as well as for water-rich compositions. Our simulations show a range of surface temperatures, most of which are not habitable, although an aqua planet TRAPPIST-1 e could maintain a temperate surface given Earth-like geological outgassing and CO2. We find that a desiccated TRAPPIST-1 h may produce habitable surface temperatures beyond the maximum greenhouse distance. Potential observational discriminants for these atmospheres in transmission and emission spectra are influenced by photochemical processes and aerosol formation and include collision-induced oxygen absorption (O2–O2), and O3, CO, SO2, H2O, and CH4 absorption features, with transit signals of up to 200 ppm. Our simulated transmission spectra are consistent with K2, Hubble Space Telescope, and Spitzer observations of the TRAPPIST-1 planets. For several terrestrial atmospheric compositions, we find that TRAPPIST-1 b is unlikely to produce aerosols. These results can inform JWST observation planning and data interpretation for the TRAPPIST-1 system and other M dwarf terrestrial planets.
Chemodynamics of Dwarf Galaxies under Ram Pressure
Authors: Williamson David , Martel Hugo 
Published: November 2018

Abstract
By implementing a dynamic wind tunnel model in a smoothed particle chemodynamic/hydrodynamic simulation suite, we have investigated the effects of ram pressure and tidal forces on dwarf galaxies similar to the Magellanic Clouds, within host galaxies with gas and dark matter halos that are varied, to compare the relative effects of tides and ram pressure. We concentrate on how the distributions of metals are affected by interactions. We find that while ram pressure and tidal forces have some effect on dwarf galaxy outflows, these effects do not produce large differences in the metal distributions of the dwarf disks, other than truncation in the outer regions in some cases, and that confinement from the host galaxy gas halo appears to be more significant than ram pressure stripping. We find that stochastic variations in the star formation rate can explain the remaining variations in disk metal properties. This raises questions on the cause of low metallicities in dwarf galaxies.