bluuebunny/crossref_metadata_2025_split huggingface dataset:
اثر نظم المعلومات الإدارية في إدارة الأزمات - د ارسة تطبيقية على المستشفيات العاملة في مدينة بنغازي
Authors: الخفيفى د. مبروكة , عوض د. رجعة 
Published: February 2020

تهدف هذه الدراسة إلى التعرف على العناصر الفعالة في نظم المعلومات الإدارية وتأثيرها على حل الأزمات وتجسدت مشكلةالدراسة في الإجابة على التساؤل المتمثل ما هي إمكانية وجود تأثير دال إحصائيا المؤشرات نجاح نظم المعلومات الإدارية علىحل الأزمات. ولإجراء الدراسة اختار الباحثان عينة الدراسة المتكونة من جميع المدراء في الإدارة العليا و الإدارة الوسطى في جميعالمستشفيات العاملة حاليا في مواقعها ) خارج الاشتباكات( في مدينة بنغازي وتوصلت الدراسة إلى أهم النتائج التالية:2-هناك درجة متوسطة لوجود مؤشرات نجاح نظم المعلومات الإدارية في مجتمع الدراسة.2- وجود تأثير دال إحصائيا لنظم لمؤشرات نجاح نظم المعلومات الإدارية على قدرة المستشفيات قيد الدراسة في التعامل معالأزمات التي تتعرض لها.
3-أكثر المؤشرات في نظام المعلومات الإدارية تأثيرا على جميع مراحل الأزمات هما جودة المعلومات ورضا المستخدم في حين أنمؤشر جودة النظام ليس لديه أي تأثير على جميع مراحل إدارة الأزمات , أما مؤشر استخدام النظام فليس له تأثير على مرحلتينمن مراحل إدارة الأزمات وهما مرحلة اكتشاف إشارات الإنذار واحتواء الأزمات. كما أوصت الدراسة بمجموعة من التوصياتالتي تساعد الإدارة في التعامل مع إدارة ألازمات.
الذكاء الوجداني وعلاقته بكلاً من قلق المستقبل وفاعلية الذات لدى طلبة الجامعة في (قسم الإرشاد وعلم النفس وقسم الدراسات الإسلامية)
Authors: محمد حسنيه محمد آدم 
Published: February 2020

هدفت إلى معرفة العلاقة بين الذكاء الوجداني وقلق المستقبل وفاعلية الذات لدى طلبة قسم علم النفس والدراسات الإسلامية وشملت العينة (60) طالب من جامعة عمر المختار 2017عام وتوصلت إلى:
1- لا توجد علاقة ارتباطيه دالة بين الذكاء الوجداني وقلق المستقبل.2- توجد علاقة موجبة طرديه عند مستوى دلالة ( 0.01 ) بين الذكاء الوجداني وفاعلية الذات.3- لا توجد فروق ذات دلالة إحصائية بين متوسطات درجات الذكور والإناث في الذكاء الوجداني4- لا توجد فروق دالة بين متوسطات درجات الذكور والإناث في قلق المستقبل5- لا توجد فروق دالة بين متوسطات درجات الذكور والإناث في فاعلية الذات6- توجد فروق دالة عند مستوى (0.05 ) بين متوسطات درجات قسم علم النفس والدراسات الإسلامية في الذكاء الوجداني وفاعلية الذات لصالح قسم علم النفس7- لا توجد فروق دالة بين متوسطات درجات مرتفعي ومنخفضي قلق المستقبل في الذكاء الوجداني8- لا توجد فروق دالة بين متوسطات درجات مرتفعي ومنخفضي الذكاء الوجداني في فاعلية الذات
O livro didático e suas contribuições para o ensino religioso
Authors: Silva Maria da Penha Lima da , Pinheiro Danielle Ventura de Lima 
Published: February 2020

O livro didático é uma importante ferramenta de trabalho utilizada pelos professores e manuseada diariamente pelos alunos. No caso do Ensino Religioso, este material didático vem sofrendo mudanças ao longo dos anos, pois sai, paulatinamente, de um caráter prosélito para uma leitura plural do fenômeno religioso, consequência de um esforço contínuo de instituições como o Fórum Nacional Permanente do Ensino Religioso (FONAPER), que vem dando um novo direcionamento para as abordagens que precisam ser desenvolvidas em sala de aula tomando como base os Parâmetros Curriculares Nacionais do Ensino Religioso (PCNER). Estudar o livro didático para o Ensino Religioso, atentando para suas peculiaridades, limitações e capacidade de incentivo à leitura é o objetivo deste trabalho. Para tanto, partiu-se de um estudo de autores que atentam para essas questões próprias deste recurso metodológico, como também se refletiu sobre as abordagens mais específicas, destinadas ao Ensino Religioso. De antemão, o estudo propiciou a apresentação tanto das especificidades do livro didático nesta área do conhecimento, suas utilizações nem sempre adequadas ao que o aluno precisa como também foi capaz de ressaltar os seus pontos positivos partindo, especialmente, da obra de Carniato (2009) como apta a atender ao que vem sendo refletido pelos profissionais da área sobre a proposta para o Ensino Religioso.
Tracking two pleasures
Authors: Brielmann Aenne A. , Pelli Denis G. 
Published: February 2020

AbstractCan people track several pleasures? In everyday life, pleasing stimuli rarely appear in isolation. Yet, experiments on aesthetic pleasure usually present only one image at a time. Here, we ask whether people can reliably report the pleasure of either of two images seen in a single glimpse. Participants (N = 13 in the original; +25 in the preregistered replication) viewed 36 Open Affective Standardized Image Set (OASIS) images that span the entire range of pleasure and beauty. On each trial, the observer saw two images, side by side, for 200 ms. An arrow cue pointed, randomly, left, right, or bidirectionally. Left or right indicated which image (the target) to rate while ignoring the other (the distractor); bidirectional requested rating the combined pleasure of both images. In half the blocks, the cue came before the images (precuing). Otherwise, it came after (postcuing). Precuing allowed the observer to ignore the distractor, while postcuing demanded tracking both images. Finally, we obtained single-pleasure ratings for each image shown alone. Our replication confirms the original study. People have unbiased access to their felt pleasure from each image and the average of both. Furthermore, the variance of the observer’s report is similar whether reporting the pleasure of one image or the average pleasure of two. The undiminished variance for reports of the average pleasure of two images indicates either that the underlying pleasure variances are highly correlated, or, more likely, that the variance arises in the common reporting process. In brief, observers can faithfully track at least two visual pleasures.
Simultaneous tracking of psychophysical detection thresholds and evoked potentials to study nociceptive processing
Authors: van den Berg Boudewijn , Doll Robert J. , Mentink Alexander L.H. , Siebenga Pieter S. , Groeneveld Geert J. , Buitenweg Jan R. 
Published: February 2020

AbstractMeasuring altered nociceptive processing involved in chronic pain is difficult due to a lack of objective methods. Potential methods to characterize human nociceptive processing involve measuring neurophysiological activity and psychophysical responses to well-defined stimuli. To reliably measure neurophysiological activity in response to nociceptive stimulation using EEG, synchronized activation of nerve fibers and a large number of stimuli are required. On the other hand, to reliably measure psychophysical detection thresholds, selection of stimulus amplitudes around the detection threshold and many stimulus–response pairs are required. Combining the two techniques helps in quantifying the properties of nociceptive processing related to detected and non-detected stimuli around the detection threshold.The two techniques were combined in an experiment including 20 healthy participants to study the effect of intra-epidermal electrical stimulus properties (i.e. amplitude, single- or double-pulse and trial number) on the detection thresholds and vertex potentials. Generalized mixed regression and linear mixed regression were used to quantify the psychophysical detection probability and neurophysiological EEG responses, respectively.It was shown that the detection probability is significantly modulated by the stimulus amplitude, trial number, and the interaction between stimulus type and amplitude. Furthermore, EEG responses were significantly modulated by stimulus detection and trial number. Hence, we successfully demonstrated the possibility to simultaneously obtain information on psychophysical and neurophysiological properties of nociceptive processing. These results warrant further investigation of the potential of this method to observe altered nociceptive processing.
Multiwavelength Emission from Galactic Jets: The Case of the Microquasar SS433
Authors: Sudoh Takahiro , Inoue Yoshiyuki , Khangulyan Dmitry 
Published: February 2020

Abstract
SS433 is a Galactic microquasar with powerful jets, where very-high-energy particles are produced. We study particle acceleration in the jets of SS433 through the use of recent multiwavelength data from radio to TeV gamma-ray. We first present a general framework for the particle acceleration, cooling, and transport in relativistic jets. We then apply this to two X-ray knots in the jets of SS433, focusing on leptonic emission. Our detailed treatment of particle transport and evolution produces substantially different predictions from previous papers. For both regions, our model can account for the multiwavelength data except for the GeV data. This suggests that GeV emission is mostly from different regions and/or mechanisms. We find that the acceleration process should be efficient, which could be realized by diffusive shock acceleration close to the Bohm limit. Provided that protons are accelerated at the same efficiency as electrons, our results imply that SS433 is a PeVatron, i.e., can accelerate protons beyond a PeV. Future hard X-ray and MeV gamma-ray observations can critically test our models by detecting the spectral turnover or cutoff.
Asymmetries of Heavy Elements in the Young Supernova Remnant Cassiopeia A
Authors: Holland-Ashford Tyler , Lopez Laura A. , Auchettl Katie 
Published: February 2020

Abstract
Supernova remnants (SNRs) offer the means to study supernovae (SNe) long after the original explosion and can provide a unique insight into the mechanism that governs these energetic events. In this work, we examine the morphologies of X-ray emission from different elements found in the youngest known core-collapse SNR in the Milky Way, Cassiopeia A. The heaviest elements exhibit the highest levels of asymmetry, which we relate to the burning process that created the elements and their proximity to the center of explosion. Our findings support recent model predictions that the material closest to the source of explosion will reflect the asymmetries inherent to the SN mechanism. Additionally, we find that the heaviest elements are moving more directly opposed to the neutron star (NS) than the lighter elements. This result is consistent with NS kicks arising from ejecta asymmetries.
The Molecular Outflow from R Mon*
Authors: Sandell Göran , Vacca W. , Bouscasse L. , Güsten R. 
Published: February 2020

Abstract
We have mapped the young Herbig Be star R Mon in CO(3–2) and 13CO(3–2) with Atacama Pathfinder EXperiment in Chile and analyzed unpublished Herschel images. We find that R Mon is embedded in a small cloud with a gas temperature of ∼20 K and a total mass of ∼70

. We confirm that R Mon drives a bipolar molecular outflow, which is blueshifted north of R Mon. The blueshifted outflow has excavated the molecular cloud north of R Mon, creating the reflection nebula NGC 2261 and filling it with high-velocity gas. At “high” velocities the orientation of the outflow is approximately n–s, which agrees with the optical jet, suggesting that the accretion disk is e–w. The outflow velocities are modest, ±9 km s−1. The outflow is rather massive, ∼0.56

in the blueshifted outflow lobe. The outflow is completely optically thick in CO(3–2) toward R Mon, indicating that its envelope is ≲2000 au. The mass of the accretion disk and surrounding envelope determined from an isothermal graybody fit is ∼0.34

. We estimate a mass-loss rate of ∼(1–3) × 10−5

yr−1, corresponding to an accretion rate of (1–9) × 10−6

yr−1. We find that R Mon has bolometric luminosity of <1000

. R Mon is still in an active accretion phase, contributing to the observed luminosity. Hence, R Mon cannot be a B0 star; it must be a late B star or even an early A star.
Electrons in the Young Solar Wind: First Results from the Parker Solar Probe
Authors: Halekas J. S. , Whittlesey P. , Larson D. E. , McGinnis D. , Maksimovic M. , Berthomier M. , Kasper J. C. , Case A. W. , Korreck K. E. , Stevens M. L. , Klein K. G. , Bale S. D. , MacDowall R. J. , Pulupa M. P. , Malaspina D. M. , Goetz K. , Harvey P. R. 
Published: February 2020

Abstract
The Solar Wind Electrons Alphas and Protons experiment on the Parker Solar Probe (PSP) mission measures the three-dimensional electron velocity distribution function. We derive the parameters of the core, halo, and strahl populations utilizing a combination of fitting to model distributions and numerical integration for ∼100,000 electron distributions measured near the Sun on the first two PSP orbits, which reached heliocentric distances as small as ∼0.17 au. As expected, the electron core density and temperature increase with decreasing heliocentric distance, while the ratio of electron thermal pressure to magnetic pressure (β

e
) decreases. These quantities have radial scaling consistent with previous observations farther from the Sun, with superposed variations associated with different solar wind streams. The density in the strahl also increases; however, the density of the halo plateaus and even decreases at perihelion, leading to a large strahl/halo ratio near the Sun. As at greater heliocentric distances, the core has a sunward drift relative to the proton frame, which balances the current carried by the strahl, satisfying the zero-current condition necessary to maintain quasi-neutrality. Many characteristics of the electron distributions near perihelion have trends with solar wind flow speed, β

e
, and/or collisional age. Near the Sun, some trends not clearly seen at 1 au become apparent, including anticorrelations between wind speed and both electron temperature and heat flux. These trends help us understand the mechanisms that shape the solar wind electron distributions at an early stage of their evolution.
WISPR Imaging of a Pristine CME
Authors: Hess Phillip , Rouillard Alexis P. , Kouloumvakos Athanasios , Liewer Paulett C. , Zhang Jie , Dhakal Suman , Stenborg Guillermo , Colaninno Robin C. , Howard Russell A. 
Published: February 2020

Abstract
The Wide-field Imager for Solar Probe (WISPR) on board the Parker Solar Probe (PSP) observed a coronal mass ejection (CME) on 2018 November 1, the first day of the initial PSP encounter. The speed of the CME, approximately 200–300 km s−1 in the WISPR field of view, is typical of slow, streamer blowout CMEs. This event was also observed by the Large Angle and Spectrometric Coronagraph Experiment (LASCO) coronagraphs. WISPR and LASCO view remarkably similar structures that enable useful cross-comparison between the two data sets as well as stereoscopic imaging of the CME. An analysis is extended to lower heights by linking the white-light observations to extreme ultraviolet (EUV) data from the Atmospheric Imaging Assembly, which reveal a structure that erupts more than a full day earlier before the CME finally gathers enough velocity to propagate outward. This EUV feature appears as a brightness enhancement in cooler temperatures, such as 171 Å, but as a cavity in nominal coronal temperatures, such as 193 Å. By comparing this circular, dark feature in 193 Å to the dark, white-light cavity at the center of the eruption in WISPR and LASCO, this is one coherent structure is seen to exist prior to the eruption in the low corona before entering the heliosphere and likely corresponds to the core of the magnetic flux rope. It is also believed that the relative weakness of the event contributed to the clarity of the flux rope in WISPR, as the CME did not experience impulsive forces or strong interaction with external structures that can lead to more complex structural evolution.
Identification of Magnetic Flux Ropes from Parker Solar Probe Observations during the First Encounter
Authors: Zhao L.-L. , Zank G. P. , Adhikari L. , Hu Q. , Kasper J. C. , Bale S. D. , Korreck K. E. , Case A. W. , Stevens M. , Bonnell J. W. , Dudok de Wit T. , Goetz K. , Harvey P. R. , MacDowall R. J. , Malaspina D. M. , Pulupa M. , Larson D. E. , Livi R. , Whittlesey P. , Klein K. G. 
Published: February 2020

Abstract
The Parker Solar Probe (PSP) observed an interplanetary coronal mass ejection (ICME) event during its first orbit around the Sun, among many other events. This event is analyzed by applying a wavelet analysis technique to obtain the reduced magnetic helicity, cross helicity, and residual energy, the first two of which are magnetohydrodynamics (MHD) invariants. Our results show that the ICME, as a large-scale magnetic flux rope, possesses high magnetic helicity, very low cross helicity, and highly negative residual energy, thus pointing to a magnetic fluctuation dominated structure. Using the same technique, we also search for small-scale coherent magnetic flux rope structures during the period from 2018 October 22 to November 21, which are intrinsic to quasi-two-dimensional MHD turbulence in the solar wind. Multiple structures with durations between 8 and 300 minutes are identified from PSP in situ spacecraft measurements. The location and scales of these structures are characterized by wavelet spectrograms of the normalized reduced magnetic helicity, normalized cross helicity, and normalized residual energy. Transport theory suggests that these small-scale magnetic flux ropes may contribute to the acceleration of charged particles through magnetic reconnection processes, and the dissipation of these structures may be important for understanding the coronal heating processes.
Turbulence Transport Modeling and First Orbit Parker Solar Probe (PSP) Observations
Authors: Adhikari L. , Zank G. P. , Zhao L.-L. , Kasper J. C. , Korreck K. E. , Stevens M. , Case A. W. , Whittlesey P. , Larson D. , Livi R. , Klein K. G. 
Published: February 2020

Abstract
The Parker Solar Probe (PSP) achieved its first orbit perihelion on 2018 November 6, reaching a heliocentric distance of about 0.165 au (35.55 R
⊙). Here, we study the evolution of fully developed turbulence associated with the slow solar wind along the PSP trajectory between 35.55 R
⊙ and 131.64 R
⊙ in the outbound direction, comparing observations to a theoretical turbulence transport model. Several turbulent quantities, such as the fluctuating kinetic energy and the corresponding correlation length, the variance of density fluctuations, and the solar wind proton temperature are determined from the PSP Solar Wind Electrons Alphas and Protons (SWEAP) plasma data along its trajectory between 35.55 R
⊙ and 131.64 R
⊙. The evolution of the PSP derived turbulent quantities are compared to the numerical solutions of the nearly incompressible magnetohydrodynamic (NI MHD) turbulence transport model recently developed by Zank et al. We find reasonable agreement between the theoretical and observed results. On the basis of these comparisons, we derive other theoretical turbulent quantities, such as the energy in forward and backward propagating modes, the total turbulent energy, the normalized residual energy and cross-helicity, the fluctuating magnetic energy, and the correlation lengths corresponding to forward and backward propagating modes, the residual energy, and the fluctuating magnetic energy.
The Solar Probe Cup on the Parker Solar Probe
Authors: Case A. W. , Kasper Justin C. , Stevens Michael L. , Korreck Kelly E. , Paulson Kristoff , Daigneau Peter , Caldwell Dave , Freeman Mark , Henry Thayne , Klingensmith Brianna , Bookbinder J. A. , Robinson Miles , Berg Peter , Tiu Chris , Wright K. H. , Reinhart Matthew J. , Curtis David , Ludlam Michael , Larson Davin , Whittlesey Phyllis , Livi Roberto , Klein Kristopher G. , Martinović Mihailo M. 
Published: February 2020

Abstract
Solar Probe Cup (SPC) is a Faraday cup instrument on board NASA’s Parker Solar Probe (PSP) spacecraft designed to make rapid measurements of thermal coronal and solar wind plasma. The spacecraft is in a heliocentric orbit that takes it closer to the Sun than any previous spacecraft, allowing measurements to be made where the coronal and solar wind plasma is being heated and accelerated. The SPC instrument was designed to be pointed directly at the Sun at all times, allowing the solar wind (which is flowing primarily radially away from the Sun) to be measured throughout the orbit. The instrument is capable of measuring solar wind ions with an energy between 100 and 6000 V (protons with speeds from 139 to 1072 km s−1). It also measures electrons with an energy/charge between 100 and 1500 V. SPC has been designed to have a wide dynamic range that is capable of measuring protons and alpha particles at the closest perihelion (9.86 solar radii from the center of the Sun) and out to 0.25 au. Initial observations from the first orbit of PSP indicate that the instrument is functioning well.
The Heliospheric Current Sheet in the Inner Heliosphere Observed by the Parker Solar Probe
Authors: Szabo Adam , Larson Davin , Whittlesey Phyllis , Stevens Michael L. , Lavraud Benoit , Phan Tai , Wallace Samantha , Jones-Mecholsky Shaela I. , Arge Charles N. , Badman Samuel T. , Odstrcil Dusan , Pogorelov Nikolai , Kim Tae , Riley Pete , Henney Carl J. , Bale Stuart D. , Bonnell John W. , Case Antony W. , Dudok de Wit Thierry , Goetz Keith , Harvey Peter , Kasper Justin C. , Korreck Kelly E. , Koval Andriy , Livi Roberto , MacDowall Robert J. , Malaspina David M. , Pulupa Marc 
Published: February 2020

Abstract
The Parker Solar Probe (PSP) completed its first solar encounter in 2018 November, bringing it closer to the Sun than any previous mission. This allowed in situ investigation of the heliospheric current sheet (HCS) inside the orbit of Venus. The Parker observations reveal a well defined magnetic sector structure placing the spacecraft in a negative polarity region for most of the encounter. The observed current sheet crossings are compared to the predictions of both potential field source surface and magnetohydrodynamic models. All the model predictions are in good qualitative agreement with the observed crossings of the HCS. The models also generally agree that the HCS was nearly parallel with the solar equator during the inbound leg of the encounter and more significantly inclined during the outbound portion. The current sheet crossings at PSP are also compared to similar measurements made by the Wind spacecraft near Earth at 1 au. After allowing for orbital geometry and propagation effects, a remarkable agreement has been found between the observations of these two spacecraft underlying the large-scale stability of the HCS. Finally, the detailed magnetic field and plasma structure of each crossing is analyzed. Marked differences were observed between PSP and Wind measurements in the type of structures found near the HCS. This suggests that significant evolution of these small solar wind structures takes place before they reach 1 au.