bluuebunny/crossref_metadata_2025_split huggingface dataset:
РОЗРОБКА ТА ПСИХОМЕТРИЧНА ПЕРЕВІРКА ОПИТУВАЛЬНИКА «НАВЧАЛЬНА САМОЕФЕКТИВНІСТЬ ДОРОСЛОГО»
Authors: Galtseva Tetiana 
Published: July 2018

У статті представлено процедуру розробки та психометричної перевірки авторського опитувальника, що розкриває рівень навчальної самоефективності дорослого і її структурних компонентів. Для з’ясування внутрішньої будови опитувальника та перевірки його відповідності побудованій теоретичній моделі навчальної самоефективності застосовано факторний аналіз, що дав змогу з достатньо високим рівнем надійності диференціювати п’ять його шкал. Опиту­вальник складається з 32 тверджень. Шкали ідентифіковані як «Впевненість у власній навчальній здатності», «Ціннісно-смислове ставлення до навчальної діяльності», «Мотиваційно-цільова спрямованість у навчанні», «Відповідальність за навчання та саморозвиток», «Прогностично-рефлексивна здатність до навчання». Сумарний результат представлено шкалою «Загальний показник навчальної самоефективності». Розроблено тестові норми для кожної шкали.
Установлено статистично значущі кореляційні зв’язки між шкалами навчальної самоефективності дорослого й мотивацією успіху або запобігання невдачі (методика МУН А. А. Реана). Виявлено кореляційні зв’язки між шкалами навчальної самоефективності дорослого та шкалами тесту «Впевненості в собі» (В. Г. Ромек), шкалою загальної самоефективності особистості (Р. Шварцер, М. Єрусалем в адаптації В. Г. Ромека). Виявлено високу критеріальну валідність розробленої методики. Результати проведенного дослідження засвідчують, що авторський опитувальник може використовуватися широким колом дослідників і психологів-практиків у діагностичній, консультативній та дослідницькій роботі.
Ocular Morbidity Among Leprosy Patients at a Leprosy Centre
Authors: Shrestha Sabina , Shrestha Chunu , Shrestha Sushan Man , Manoranjan Aparajita , Dhungana Arun Prasad 
Published: July 2018

Introduction: Leprosy is one of the dreaded communicable disease due to its profound morbidity. In earlier days in Nepal, a different settlement was designated for leprosy patient and their families. Khokana of Lalitpur district of Nepal is one of them. The study was conducted to determine ocular morbidity among leprosy patients who had completed multi drug therapy. Methods: It was descriptive, quantitative and cross sectional study conducted at Khokana Leprosy Centre in Lalitpur district of Nepal. Leprosy patients who had completed multi drug therapy and consenting for the study were enrolled. Convenience sampling was done and the sample size was 70. After detail ophthalmic evaluation, socio-demographic profile of the participants and their ocular morbidities were documented and analysed.Results: Major findings were superciliary madarosis (78.57%), ciliary madarosis (61.4%), different grades of cataract (67.10% right eye and 60% left eye), pseudophakia (30% right eye and 37.10% left eye), tylosis (44.3%), corneal hypoesthesia (10% unilaterally and 15.7% bilaterally) and dry eye (10%). Entropion was present in 2.9% both unilaterally and bilaterally. Ectropion was present in 5.7% unilaterally and 10% bilaterally. Trichiasis was present in 1.4% unilaterally and 2.9% bilaterally. Similarly, eyelid nodule was present in 7.1% unilaterally and 1.4% bilaterally. Incomplete closure of the lids was present in 8.6% unilaterally and 2.9% bilaterally. Exposure keratitis was present in 7.1% unilaterally and 1.4% bilaterally, corneal opacity in 2.9% unilaterally and 1.4% bilaterally and corneal perforation in 2.9% unilaterally. Chronic iridocyclitis was present in 2.9% cases. Retinal pearls were seen in 2.86% of cases. According to WHO criteria of blindness, 2.9% patients were blind in the present study. 14 persons were unilaterally blind and among them, two had severe visual impairment in the other eye, eight had other eye moderate visual impairment and four had other eye mild visual impairment.Conclusions: Lid abnormalities, corneal abnormalities and cataract were the commonly encountered ocular morbidities among treated leprosy patients.
Risk Stratification of Coronary Heart Disease in Postmenopausal Women Using Framingham Scale in Eastern Nepal
Authors: Bajracharya Sujeeta , Rai Bijendra Kumar , Giri Rajani , Joshi Rinku 
Published: July 2018

Introduction: Cardiovascular disease (CVD) is one of the leading causes of mortality and morbidity in both developed and developing countries. CVD risk rises to double fold in women after menopause. We aim to stratify menopausal women of our region for having coronary heart disease in next 10 years. Methods: One year cross sectional study was conducted in General Out Patient Department (GOPD) of a tertiary care centre of Eastern Nepal. The Standard ATP calculator was used and the relevant necessary data was introduced into the calculator and the automated result was collected. Results: Among 272 participants, above 50% had Framingham score 1 to 5%. And the risk was greater within first five years after menopause in 50 to 59 years of age group. Similarly, with advancing age and longer duration of menopause the risk became significantly higher.Conclusions: Besides the established risk factors for CVD, postmenopausal state is additional risk for women and this study emphasises this factor as risk of CVD even in our set up.
The Socio-Economic Development of Cross-Border Territories: Statistical Monitoring
Authors: Motuzka О. М. , Parkhomenko V. V. 
Published: July 2018

Because the methodology for studying the socio-economic development of cross-border territories is still poorly developed in the Ukrainian science, this study aims to highlight its theoretical essence and justify the need for statistical monitoring and identification of practical problems related with its applications at personal, institutional and regional level.
Given the global market competition, the socio-economic development of cross-border territories is impossible without creating favorable financial, institutional and infrastructure environment. The socio-economic development of cross-border territories is determined by a set of indicators reflecting the capabilities of territories located on both sides of the border to produce a certain output of goods and services using the available human and material resources.
The importance of cross-border statistics grows with the expansion of cross-border cooperation. Cross-border statistics refers to the generalized information on the socio-economic development of cross-border territories; it has to support the CBC-related operation of central and local administration bodies and private entities in border regions, aimed at expanding business partnerships and meeting public needs on border territories.
The source of data for cross-border statistics is the statistics of border regions. The analysis shows that trial decisions used now in the Ukrainian statistics system for testing border region statistics, such as statistics of tourism, including travels abroad, are not capable to meet information needs of the regional development policy, foreign trade statistics and statistics of internal and external migration.
The statistics of cross-border regions has to face the following challenges: improve the comparability of statistical indicators by harmonizing statistical surveys’ methodology, terminology, definitions and classifications; expand and improve printing and publishing activities; develop analytical work; introduce and develop cross-border surveys; construct on-line cross-border database.
Time-resolved WISE/NEOWISE Coadds
Authors: Meisner A. M. , Lang D. , Schlegel D. J. 
Published: July 2018

Abstract
We have used the first ∼3 years of 3.4 μm (W1) and 4.6 μm (W2) observations from the WISE and NEOWISE missions to create a full-sky set of time-resolved coadds. As a result of the WISE survey strategy, a typical sky location is visited every six months and is observed during ≳12 exposures per visit, with these exposures spanning a ∼1 day time interval. We have stacked the exposures within such ∼1 day intervals to produce one coadd per band per visit—that is, one coadd every six months at a given position on the sky in each of W1 and W2. For most parts of the sky, we have generated six epochal coadds per band, with one visit during the fully cryogenic WISE mission, one visit during NEOWISE, and then, after a 33-month gap, four more visits during the NEOWISE-Reactivation mission phase. These coadds are suitable for studying long-timescale mid-infrared variability and measuring motions to ∼1.3 mag fainter than the single-exposure detection limit. In most sky regions, our coadds span a 5.5-year time period and therefore provide a >10× enhancement in time baseline relative to that available for the AllWISE catalog’s apparent motion measurements. As such, the signature application of these new coadds is expected to be motion-based identification of relatively faint brown dwarfs, especially those cold enough to remain undetected by Gaia.
Subaru/HiCIAO HKs Imaging of LKHa 330: Multi-band Detection of the Gap and Spiral-like Structures
Authors: Uyama Taichi , Hashimoto Jun , Muto Takayuki , Akiyama Eiji , Dong Ruobing , Leon Jerome de , Sakon Itsuki , Kudo Tomoyuki , Kusakabe Nobuhiko , Kuzuhara Masayuki , Bonnefoy Mickael , Abe Lyu , Brandner Wolfgang , Brandt Timothy D. , Carson Joseph C. , Currie Thayne , Egner Sebastian , Feldt Markus , Fung Jeffrey , Goto Miwa , Grady Carol A. , Guyon Olivier , Hayano Yutaka , Hayashi Masahiko , Hayashi Saeko S. , Henning Thomas , Hodapp Klaus W. , Ishii Miki , Iye Masanori , Janson Markus , Kandori Ryo , Knapp Gillian R. , Kwon Jungmi , Matsuo Taro , Mayama Satoshi , Mcelwain Michael W. , Miyama Shoken , Morino Jun-Ichi , Moro-Martin Amaya , Nishimura Tetsuo , Pyo Tae-Soo , Serabyn Eugene , Sitko Michael L. , Suenaga Takuya , Suto Hiroshi , Suzuki Ryuji , Takahashi Yasuhiro H. , Takami Michihiro , Takato Naruhisa , Terada Hiroshi , Thalmann Christian , Turner Edwin L. , Watanabe Makoto , Wisniewski John , Yamada Toru , Yang Yi , Takami Hideki , Usuda Tomonori , Tamura Motohide 
Published: July 2018

Abstract
We present H- and K
s-bands observations of the LkHα 330 disk with a multi-band detection of the large gap and spiral-like structures. The morphology of the outer disk (r ∼ 0.″3) at PA = 0°–45° and PA° = 180–290° is likely density wave-induced spirals, and comparison between our observational results and simulations suggests a planet formation. We have also investigated the azimuthal profiles at the ring and the outer-disk regions as well as radial profiles in the directions of the spiral-like structures and semimajor axis. Azimuthal analysis shows a large variety in wavelength and implies that the disk has non-axisymmetric dust distributions. The radial profiles in the major-axis direction (PA = 271°) suggest that the outer region (r ≥ 0.″25) may be influenced by shadows of the inner region of the disk. The spiral-like directions (PA = 10° and 230°) show different radial profiles, which suggests that the surfaces of the spiral-like structures are highly flared and/or have different dust properties. Finally, a color map of the disk shows a lack of an outer eastern region in the H-band disk, which may hint at the presence of an inner object that casts a directional shadow onto the disk.
A Study of the Hα Variability of Be Stars
Authors: Dimitrov Dinko P. , Kjurkchieva Diana P. , Ivanov Emil I. 
Published: July 2018

Abstract
This paper presents the results of 4 years of high-resolution spectral observations of 69 emission-line stars, 54 of them being newly discovered sources. We classified the stars on the basis of their position in the two-color IR diagram and some additional criteria: shape and width of the Hα profile, presence of He lines, proper motion and parallax, membership to open cluster and associations. Sixty of our targets turned out to be Be stars. We also found four late giants, four pre-MS stars, and one late dwarf. The Hα emission profiles of our Be stars range from single peaked to typical shell profiles that can also be highly asymmetric or single-peaked profiles with a narrow absorption core. The emission profiles appear almost constant with time or highly variable in intensity and in their V/R ratio. The detected long-term variability of the Hα emission is important for investigating the on/off switch phenomenon of Be stars. Our study led to an increase of the number of the emission-line stars of 16 open clusters.
Jupiter’s Mesoscale Waves Observed at 5 μm by Ground-based Observations and Juno JIRAM
Authors: Fletcher Leigh N. , Melin H. , Adriani A. , Simon A. A. , Sanchez-Lavega A. , Donnelly P. T. , Antuñano A. , Orton G. S. , Hueso R. , Kraaikamp E. , Wong M. H. , Barnett M. , Moriconi M. L. , Altieri F. , Sindoni G. 
Published: July 2018

Abstract
We characterize the origin and evolution of a mesoscale wave pattern in Jupiter’s North Equatorial Belt (NEB), detected for the first time at 5 μm using a 2016–17 campaign of “lucky imaging” from the VISIR instrument on the Very Large Telescope and the NIRI instrument on the Gemini observatory, coupled with M-band imaging from Juno’s JIRAM instrument during the first seven Juno orbits. The wave is compact, with a 1.°1–1.°4 longitude wavelength (wavelength 1300–1600 km, wavenumber 260–330) that is stable over time, with wave crests aligned largely north–south between 14°N and 17°N (planetographic). The waves were initially identified in small (10° longitude) packets immediately west of cyclones in the NEB at 16°N but extended to span wider longitude ranges over time. The waves exhibit a 7–10 K brightness temperature amplitude on top of an ∼210 K background at 5 μm. The thermal structure of the NEB allows for both inertio-gravity waves and gravity waves. Despite detection at 5 μm, this does not necessarily imply a deep location for the waves, and an upper tropospheric aerosol layer near 400–800 mbar could feature a gravity wave pattern modulating the visible-light reflectivity and attenuating the 5-μm radiance originating from deeper levels. Strong rifting activity appears to obliterate the pattern, which can change on timescales of weeks. The NEB underwent a new expansion and contraction episode in 2016–17 with associated cyclone–anticyclone formation, which could explain why the mesoscale wave pattern was more vivid in 2017 than ever before.
Millisecond Pulsar Origin of the Galactic Center Excess and Extended Gamma-Ray Emission from Andromeda: A Closer Look
Authors: Eckner Christopher , Hou Xian , Serpico Pasquale D. , Winter Miles , Zaharijas Gabrijela , Martin Pierrick , Mauro Mattia di , Mirabal Nestor , Petrovic Jovana , Prodanovic Tijana , Vandenbroucke Justin 
Published: July 2018

Abstract
A new measurement of a spatially extended gamma-ray signal from the center of the Andromeda galaxy (M31) has recently been published by the Fermi-LAT collaboration, reporting that the emission broadly resembles the so-called Galactic center excess (GCE) of the Milky Way (MW). The weight of the evidence is steadily accumulating on a millisecond pulsar (MSPs) origin for the GCE. These elements prompt us to compare these observations with what is, perhaps, the simplest model for an MSP population, which is solely obtained by rescaling of the MSP luminosity function that is determined in the local MW disk via the respective stellar mass of the systems. Remarkably, we find that without free fitting parameters, this model can account for both the energetics and the morphology of the GCE within uncertainties. For M31, the estimated luminosity due to primordial MSPs is expected to only contribute about a quarter of the detected emission, although a stronger contribution cannot be excluded given the large uncertainties. If correct, the model predicts that the M31 disk emission due to MSPs is not far below the present upper bound. We also discuss additional refinements of this simple model. Using the correlation between globular cluster gamma-ray luminosity and stellar encounter rate, we gauge the dynamical MSP formation in the bulge. This component is expected to contribute to the GCE only at a level of ≲5%, it could affect the signal’s morphology. We also comment on the limitations of our model and on future perspectives for improved diagnostics.
Observational Evidence for Langmuir Wave Collapse in the Source Region of a Solar Type III Radio Burst
Authors: Thejappa G. , MacDowall R. J. 
Published: July 2018

Abstract
High-time-resolution in situ wave observations show that Langmuir waves associated with solar type III radio bursts often occur as coherent localized one-dimensional magnetic-field-aligned wave packets with short durations of a few milliseconds and peak intensities well above the strong turbulence thresholds. In this paper, we report observations of a wave packet obtained by the time domain sampler of the STEREO WAVES experiment, which is unique in the sense that it is the most intense wave packet ever detected in association with a solar type III radio burst, with a peak intensity E

t
∼ 107 mVm−1. We show that this wave packet provides evidence for (1) oscillating two-stream instability (OTSI), (2) a collapsing soliton formed as a result of OTSI, (3) the formation of a soliton–caviton pair, and (4) excitation of second and third harmonic electromagnetic waves. We also show that the peak intensity and spatial width satisfy the threshold condition for this wave packet to be the collapsing Langmuir wave packet formed as a result of nucleation processes even when δn

b
> δn

p
, where δn

b
and δn

p
are the levels of background and ponderomotive-force-induced density fluctuations, respectively. Thus, these observations provide unambiguous evidence for the spatial collapse of Langmuir waves in the source region of a type III radio burst, and the observed spectral evidence for OTSI and the ponderomotive-force-induced density cavity strongly suggest that OTSI is mostly likely responsible for the collapse of the observed wave packet.
Deep Chandra Observations of X-Ray Point Sources in M87
Authors: Luan Luan , Jones Christine , Forman William R. , Bogdán Ákos , Andrade-Santos Felipe , Goulding Andy D. , Hickox Ryan C. , Hou Meicun , Li Zhiyuan 
Published: July 2018

Abstract
We present a study of X-ray source populations in M87, the cD galaxy of the Virgo cluster, using 12 archival Chandra observations with a total exposure of ∼680 ks spanning about a decade. A total of 346 point-like sources are detected down to a limiting 0.5–8 keV luminosity of 4 × 1037 erg s−1 and out to a galactocentric radius of ∼40 kpc. We cross-correlate the X-ray sources with published catalogs of globular clusters (GCs), derived from the ACS Virgo Cluster Survey and the Next Generation Virgo Cluster Survey. This results in 122 matches, making it one of the largest samples of GC-hosting X-ray sources in an external galaxy. These sources, most likely low-mass X-ray binaries (LMXBs), correspond to ∼5% of all known GCs within the Chandra field-of-view. Conversely, ∼50% of the detected X-ray sources are found in a GC. Moreover, red (metal-rich) GCs are ∼2.2 times more likely to host an X-ray source than blue (metal-poor) GCs. We also examine 76 currently known ultra-compact dwarf galaxies around M87 but find no significant X-ray counterparts. After statistically accounting for the cosmic X-ray background, we identify ∼110 field-LMXBs. The GC-LMXBs and field-LMXBs differ in their luminosity function and radial distribution, which indicates that the latter cannot be primarily originated from GCs. Using another set of deep Chandra observations toward ∼100 kpc northwest of the M87 center, we statistically constrain the abundance of field-LMXBs in the stellar halo, which is consistent with that found in the central region. We also identify 40 variable X-ray sources, among which one source is likely a black hole binary residing in a GC.
Fourier Analysis of Advection-dominated Accretion Flows
Authors: Habibi Asiyeh , Abbassi Shahram , Shadmehri Mohsen 
Published: July 2018

Abstract
We implement a new semi-analytical approach to investigate radially self-similar solutions for the steady-state advection-dominated accretion flows (ADAFs). We employ the usual α-prescription for the viscosity, and all components of the energy–momentum tensor are considered. In this case, in the spherical coordinate, the problem reduces to a set of eighth-order, nonlinear differential equations with respect to the latitudinal angle θ. Using the Fourier expansions for all the flow quantities, we convert the governing differential equations to a large set of nonlinear algebraic equations for the Fourier coefficients. We solve the algebraic equations via the Newton–Raphson method, and investigate the ADAF properties over a wide range of model parameters. We also show that the implemented series are truly convergent. The main advantage of our numerical method is that it does not suffer from the usual technical restrictions that may arise for solving ADAF differential equations near the polar axis. In order to check the reliability of our approach, we recover some widely studied solutions. Further, we introduce a new varying α viscosity model. New outflow and inflow solutions for ADAFs are also presented, using Fourier expansion series.
Identification of Multiple Hard X-Ray Sources in Solar Flares: A Bayesian Analysis of the 2002 February 20 Event
Authors: Sciacchitano Federica , Sorrentino Alberto , Emslie A Gordon , Massone Anna Maria , Piana Michele 
Published: July 2018

Abstract
The hard X-ray emission in a solar flare is typically characterized by a number of discrete sources, each with its own spectral, temporal, and spatial variability. Establishing the relationship among these sources is critical to determining the role of each in the energy release and transport processes that occur within the flare. In this paper we present a novel method to identify and characterize each source of hard X-ray emission. The method permits a quantitative determination of the most likely number of subsources present, and of the relative probabilities that the hard X-ray emission in a given subregion of the flare is represented by a complicated multiple source structure or by a simpler single source. We apply the method to a well-studied flare on 2002 February 20 in order to assess competing claims as to the number of chromospheric footpoint sources present, and hence to the complexity of the underlying magnetic geometry/topology. Contrary to previous claims of the need for multiple sources to account for the chromospheric hard X-ray emission at different locations and times, we find that a simple two-footpoint-plus-coronal-source model is the most probable explanation for the data. We also find that one of the footpoint sources moves quite rapidly throughout the event, a factor that presumably complicated previous analyses. The inferred velocity of the footpoint corresponds to a very high induced electric field, compatible with the fields in thin reconnecting current sheets.
Neutron Star Cooling with a Dynamic Stellar Structure
Authors: Dong J. M. , Wang L. J. , Zuo W. 
Published: July 2018

Abstract
The observations combined with theory of neutron star (NS) cooling play a crucial role in achieving the intriguing information of the stellar interior, such as the equation of state, composition, and superfluidity of dense matter. The traditional NS cooling theory is based on the assumption that the stellar structure does not change with time. The validity of such a static description has not yet been confirmed. We generalize the theory to a dynamic treatment; that is, continuous change of the NS structure (rearrangement of the stellar density distribution with the total baryon number fixed) as the decrease of temperature during the thermal evolution, is taken into account. It is found that the practical thermal energy used for the cooling is slightly lower than that estimated in a static situation, and hence the cooling of NSs is accelerated correspondingly but the effect is rather weak. Therefore, the static treatment is a good approximation in the calculations of NS cooling.