bluuebunny/crossref_metadata_2025_split huggingface dataset:
NEONATAL SUPRAVENTRİKÜLER TAŞİARİTMİ TEDAVİSİNDE GÜNCEL YAKLAŞIMLAR: OLGU SERİSİ
Authors: DİLLİ Dilek , ÇİTLİ Rumeysa , ÖZGÜR Senem , TAŞOĞLU İrfan , ÖRÜN Utku Arman , AYDOĞAN Seda , ÖZGÜNER İsmet Faruk , ZENCİROĞLU Ayşegül 
Published: August 2020

Amaç: Yenidoğanlarda kardiyak aritminin
bütün şekilleri görülebileceği gibi, en sık görülen aritmi tipi
supraventriküler taşikardilerdir (SVT). Bu makalede henüz ortak bir yaklaşım olmayan
bu taşiaritmi tipinde güncel tedavi seçeneklerinin tartışılması amaçlanmıştır. Olgular: Hastalarımızda
ortalama SVT gelişme yaşı 7,4 gün ve kalp tepe atımı (KTA) 234/dk idi. Tüm
olgular medikal tedaviye cevap vermiş olup elektrofizyolojik çalışma
gerekmemiştir. Serimizde, tüm olgularda SVT atağında tedavide ilk seçenek
olarak adenozin uygulanmış olup tekrarlayan SVT atakları için ek medikal tedavilere
gereksinim doğmuştur.
Olgularımızdan altı (%85,7) hastaya yineleyen SVT atakları nedeniyle
propranolol tedavisi gerekmiştir. Adenozine yanıtsız SVT gelişen bir olgumuzda
amiodaron infüzyonunun tedricen azaltılması sırasında propranolol tedavisine ek
olarak flekainid eklenmiştir. Tedavi sonrası SVT atağı gözlenmemiştir.

Sonuç: Yenidoğanda uzun süre devam eden
SVT ataklarının kalp yetmezliği ve multiorgan disfonksiyonuna sebep olabileceği
göz önüne alınarak tedavide kullanılan farklı ilaçlar servislerde hazır
bulundurulmalı ve vakalar yoğun bakım şartlarında multidisipliner bir yaklaşımla izlenmelidir.
S62 and S4711: Indications of a Population of Faint Fast-moving Stars inside the S2 Orbit—S4711 on a 7.6 yr Orbit around Sgr A*
Authors: Peißker Florian , Eckart Andreas , Zajaček Michal , Ali Basel , Parsa Marzieh 
Published: August 2020

Abstract
We present high-pass filtered NACO and SINFONI images of the newly discovered stars S4711–S4715 between 2004 and 2016. Our deep H+K-band (SINFONI) and K-band (NACO) data show the S-cluster star S4711 on a highly eccentric trajectory around Sgr A* with an orbital period of 7.6 yr and a periapse distance of 144 au to the supermassive black hole (SMBH). S4711 is hereby the star with the shortest orbital period and the smallest mean distance to the SMBH during its orbit to date. The used high-pass filtered images are based on coadded data sets to improve the signal to noise. The spectroscopic SINFONI data let us determine detailed stellar properties of S4711 like the mass and the rotational velocity. The faint S-cluster star candidates, S4712–S4715, can be observed in a projected distance to Sgr A* of at least temporarily ≤120 mas. From these stars, S4714 is the most prominent, with an orbital period of 12 yr and an eccentricity of 0.985. The stars S4712–S4715 show similar properties, with magnitudes and stellar masses comparable to those of S4711. The MCMC simulations determine confidently precise uncertainties for the orbital elements of S62 and S4711–S4715. The presence of S4711 in addition to S55, S62, and the also newly found star S4714 implies a population of faint stars that can be found at distances to Sgr A* that are comparable to the size of our solar system. These short orbital time period stars in the dense cluster around the SMBH in the center of our Galaxy are perfect candidates to observe gravitational effects such as the periapse shift.
Near-infrared [Fe II] and H2 Line Mapping of the Supernova Remnant IC 443 with the IRSF/SIRIUS
Authors: Kokusho Takuma , Torii Hiroki , Nagayama Takahiro , Kaneda Hidehiro , Sano Hidetoshi , Ishihara Daisuke , Onaka Takashi 
Published: August 2020

Abstract
We investigate properties of the interstellar medium (ISM) interacting with shocks around the Galactic supernova remnant IC 443, using the results of near-infrared [Fe ii] and H2 line mapping with the InfraRed Survey Facility/Simultaneous Infrared Imager for Unbiased Survey. In the present study, we newly performed H2 1–0 S(1) and 2–1 S(1) line mapping with the narrowband filters tuned for these lines, covering the entire remnant (

30
′
×

35
′

). Combined with an [Fe ii] line map, our result shows that the H2 line emission is significantly detected in the southern region, while the [Fe ii] line emission is detected all over the remnant, suggesting that slow and fast shocks propagate through the southern region and the entire remnant, respectively. In particular, the H2 line emission is relatively strong compared to the [Fe ii] line emission in the southwestern region, where TeV γ-ray emission is detected. As the strong H2 line emission indicates the dominance of the dense ISM, this result supports the scenario that the γ-ray emission is likely to be produced through a heavy interaction between cosmic-ray protons and the dense ISM in the southwestern shell. We also find that the H2 and [Fe ii] line emissions show an anti-correlated spatial distribution in the same region, suggesting the presence of the clumpy ISM. Such a clumpy morphology of the ISM around IC 443 may assist cosmic-ray protons to efficiently interact with large amounts of the ISM protons.
Inferring Contributions from Unresolved Point Sources to Diffuse Emissions Measured in UV Sky Surveys: General Method and SOHO/SWAN Case Study
Authors: Strumik M. , Bzowski M. , Kowalska-Leszczynska I. , Kubiak M. A. 
Published: August 2020

Abstract
In observations of diffuse emissions like, e.g., the Lyα heliospheric glow, contributions to the observed signal from point sources (e.g., stars) are considered to be a contamination. There are relatively few bright point sources that are usually properly resolved and can be subtracted or masked. We present results of an analysis of the distribution of point sources using UV sky-survey maps from the Solar and Heliospheric Observatory (SOHO)/Solar Wind ANisotropy (SWAN) instrument and spectrophotometry data from the International Ultraviolet Explorer satellite. The estimated distribution suggests that the number of these sources increases with decreasing intensity. Below a certain threshold, these sources cannot be resolved against the diffuse signal from the backscatter glow, that results in a certain physical background from unresolved point sources. Detection, understanding, and subtraction of the point-source background has implications for proper characterization of diffuse emissions and accurate comparison with models. Stars are also often used as standard candles for in-flight calibration of satellite UV observations, thus proper understanding of signal contributions from the point sources is important for the calibration process. We present a general approach to quantify the background radiation level from unresolved point sources in UV sky-survey maps. In the proposed method, a distribution of point sources as a function of their intensity is properly integrated to compute the background signal level. These general considerations are applied to estimate the unresolved-point-source background in the SOHO/SWAN observations that on average amounts to 28.9 R. We also discuss the background radiation anisotropies and general questions related to modeling the point-source contributions to diffuse UV-emission observations.
New Conductive Opacities for White Dwarf Envelopes
Authors: Blouin Simon , Shaffer Nathaniel R. , Saumon Didier , Starrett Charles E. 
Published: August 2020

Abstract
Thanks to their continuous cooling and relative simplicity, white dwarf stars are routinely used to measure the ages of stellar populations. The usefulness of white dwarfs as cosmochronometers depends on the availability of accurate cooling models. A key ingredient of those models is conductive opacities, which largely govern the cooling rate. In this work, we present improved conductive opacities for the regime of moderate coupling and moderate degeneracy that characterizes an important portion of the envelopes of DA and DB white dwarfs. We find differences of up to a factor of 3 between our calculations and the commonly used opacities of Cassisi et al., which we attribute to an improved account of electron–electron scattering. The cooling models are strongly affected by those changes in the conductive opacities: the age of a 4000 K white dwarf can be reduced by as much as 2 Gyr. We provide analytical fits to our new opacities to facilitate the implementation of this important effect in white dwarf evolution codes.
‘Oumuamua’s Rotation with the Mechanical Torque Produced by Interstellar Medium
Authors: Zhou Wen Han 
Published: August 2020

Abstract
The first interstellar object ‘Oumuamua was discovered in 2017. When ‘Oumuamua travels in interstellar space, it keeps colliding with the interstellar medium (ISM). Given a sufficiently long interaction time, its rotation state may change significantly because of the angular momentum transfer with the interstellar medium. Using generated Gaussian random spheres with dimension ratios 6:1:1 and 5:5:1, this paper explores the ISM torque curve and proposes that ISM collision may account for ‘Oumuamua’s tumbling with the simple constant-torque analytical method. The statistic results show that the asymptotic obliquities distribute mostly at 0° and 180° and most cases spin down at the asymptotic obliquity, indicating that the ISM collision effect is similar to the Yarkovsky–O’Keefe–Radzievskii–Paddack (YORP) effect with zero heat conductivity assumed. Given a long time of deceleration of the spin rate, an initial major-axis rotation may evolve into tumbling motion under ISM torque. Using a constant-torque analytical model, the timescales of evolving into tumbling for the sample of 200 shapes are found to range from several gigayears to tens of gigayears, highly dependent on the chosen shape. The mean value is about 8.5 ± 0.5 Gyr for prolate shapes and 7.3 ± 0.4 Gyr for oblate shapes. Rotation of asteroids in the Oort cloud might also be dominated by the ISM collision effect since the YORP effect is quite weak at such a long distance from the Sun. Although this paper assumes an ideal mirror reflection and a constant relative velocity of ‘Oumuamua, the results still show the importance of the ISM collision effect.
Asteroseismic Analyses of Slowly Pulsating B Star KIC 8324482: Ultraweak Element Mixing beyond the Central Convective Core
Authors: Wu Tao , Li Yan , Deng Zhen-min , Lin Gui-fang , Song Han-feng , Jiang Chen 
Published: August 2020

Abstract
Asteroseismology is a powerful tool for probing the inner structure and determining the evolutionary status and the fundamental parameters of stars. The oscillation spectra of slowly pulsating B (SPB) stars show almost uniform period spans, whose pattern is sensitive to the structure of the μ-gradient shell beyond the central convective core and hence can be used to efficiently describe their shapes and constrain the convective core. The SPB star KIC 8324482 was observed by Kepler for over 1470 days with a long-cadence pattern. Nearly equidistant period spacing patterns are found for the 14 connective dipolar modes that are extracted from the oscillation spectrum by Zhang et al. In the present work, we analyze them in depth with the χ
2-matching method and determine their χ
2-minimization models (CMMs). Based on those calculated CMMs, we find that KIC 8324482 is a young (

Myr), metal-poor (

dex), and intermediate-mass (

) star with a convective core of

in mass and

in radius and with a surface rotation velocity

. The central hydrogen abundance is of

. Asteroseismic analyses indicate that the “propagation time” of g-mode in KIC 8324482 is of

μHz. To well match with the observed period spacing pattern, an extra diffusion mixing (

) should be considered, but the normal core overshooting f
ov must be fixed as zero in the best-fitting model. Such ultraweak mixing beyond the convective core corresponds to a fast rotation that is about 20–30 times the asteroseismic suggested rotation Ωrot ≃ 0.2 μHz, if it is thought of as shear mixing induced completely by differential rotation.
A Comparison of the Stellar, CO, and Dust-continuum Emission from Three Star-forming HUDF Galaxies at z ∼ 2
Authors: Kaasinen Melanie , Walter Fabian , Novak Mladen , Neeleman Marcel , Smail Ian , Boogaard Leindert , Cunha Elisabete da , Weiss Axel , Liu Daizhong , Decarli Roberto , Popping Gergö , Diaz-Santos Tanio , Cortés Paulo , Aravena Manuel , Werf Paul van der , Riechers Dominik , Inami Hanae , Hodge Jacqueline A. , Rix Hans-Walter , Cox Pierre 
Published: August 2020

Abstract
We compare the extent of the dust, molecular gas, and stars in three star-forming galaxies, at z = 1.4, 1.6, and 2.7, selected from the Hubble Ultra Deep Field based on their bright carbon monoxide (CO) and dust-continuum emission as well as their large rest-frame optical sizes. The galaxies have high stellar masses,

, and reside on, or slightly below, the main sequence of star-forming galaxies at their respective redshifts. We probe the dust and molecular gas using subarcsecond Atacama Large Millimeter/submillimeter Array observations of the 1.3 mm continuum and CO line emission, respectively, and probe the stellar distribution using Hubble Space Telescope observations at 1.6 μm. We find that for all three galaxies the CO emission appears ≳30% more compact than the stellar emission. For the z = 1.4 and 2.7 galaxies, the dust emission is also more compact, by ≳50%, than the stellar emission, whereas for the z = 1.6 galaxy, the dust and stellar emission have similar spatial extents. This similar spatial extent is consistent with observations of local disk galaxies. However, most high-redshift observations show more compact dust emission, likely because of the ubiquity of central starbursts at high redshift and the limited sensitivity of many of these observations. Using the CO emission line, we also investigate the kinematics of the cold interstellar medium in the galaxies, and find that all three have kinematics consistent with a rotation-dominated disk.
A Redshifted Inner Disk Atmosphere and Transient Absorbers in the Ultracompact Neutron Star X-Ray Binary 4U 1916–053
Authors: Trueba Nicolas , Miller J. M. , Fabian A. C. , Kaastra J. , Kallman T. , Lohfink A. , Proga D. , Raymond J. , Reynolds C. , Reynolds M. , Zoghbi A. 
Published: August 2020

Abstract
The very small accretion disks in ultracompact X-ray binaries are special laboratories in which to study disk accretion and outflows. We report on three sets of new (250 ks total) and archival (50 ks) Chandra/HETG observations of the “dipping” neutron star X-ray binary 4U 1916–053, which has an orbital period of P ≃ 50 minutes. We find that the bulk of the absorption in all three spectra originates in a disk atmosphere that is redshifted by v ≃ 220–290 km s−1, corresponding to the gravitational redshift at a radius of R ∼ 1200 GM/c
2. This shift is present in the strongest, most highly ionized lines (Si xiv and Fe xxvi), with a significance of 5σ. Absorption lines observed during dipping events (typically associated with the outermost disk) instead display no velocity shifts and serve as a local standard of rest, suggesting that the redshift is intrinsic to an inner disk atmosphere and not due to radial motion in the galaxy or a kick. In two spectra, there is also evidence of a more strongly redshifted component that would correspond to a disk atmosphere at R ∼ 70 GM/c
2; this component is significant at the 3σ level. Finally, in one spectrum, we find evidence of a disk wind with a blueshift of

. If real, this wind would require magnetic driving.
Une réforme politique ancrée dans la longue durée : le Grand atour de Metz (1405)
Authors: Adrian Dominique 
Published: August 2020

En 1405, le gouvernement patricien messin est renversé par des contestataires qui remplacent les patriciens exilés, tout en réformant les institutions municipales. Cette réforme est beaucoup plus limitée que celles qui, dans les villes germanophones de l’Empire, conduisent à la création de régimes fondés sur la représentation de corps de métier. Pourtant, elle témoigne d’une réflexion sur la légitimation politique et sociale : la longue charte connue comme « Grand atour » qui lui donne une mise en forme écrite commence par une critique radicale du gouvernement patricien, puis énumère une longue série de mesures de détail qui vise certainement à rendre acceptables les mesures prises. Le retour à l’ordre ancien, avec répression violente, a lieu dès 1406, mais la mémoire des événements et du texte reste vivace pendant au moins un siècle, ce dont témoigne une transmission manuscrite révélatrice des usages de long terme de ce texte contestataire.
L’expertise de la signature du roi Louis XI à l’aide des méthodes judiciaires
Authors: Nosova Ekaterina 
Published: August 2020

Lors de la description et du catalogage des documents, les autographes des monarques doivent souvent être vérifiés en raison de la pratique consistant à avoir des secrétaires qui peuvent signer des documents au nom du roi. L’un des premiers rois de France à avoir eu de tels administrateurs fut Louis XI. Comme les secrétaires de la main étaient des calligraphes qualifiés, la tâche semble difficile et nécessite la mise au point d’un appareil de recherche traditionnel. Nous avons essayé d’utiliser les méthodes d’expertise judiciare. La marque de l’imitation de l’écriture d’une autre personne est la diminution de la coordination des mouvements, qui se manifeste par la sinuosité et l’angularité des traits, la prédominance des attachements sur l’écriture conjointe, les débuts et les fins de traits émoussés, les arrêts injustifiés de la plume, ainsi que les pressions indifférenciées. En examinant les autographes de Louis XI provenant des Archives historiques et scientifiques de l’Institut d’histoire à Saint-Pétérsbourg on a découvert tous ces signes, ce qui indique que les signatures n’ont pas été exécutées par le roi lui-même. paléographie
Un cas d’appropriation temporelle d’une doctrine canonique : l’argument de la necessitas comme justification de l’exception en matière fiscale
Authors: Le Mauff Julien 
Published: August 2020

Connu à partir du xiii e siècle dans la pratique fiscale temporelle, particulièrement en Angleterre et en France, l’usage de la nécessité dans les discours de justification de décisions exceptionnelles est précisément inauguré par Henri III Plantagenêt. Or, la levée fiscale décidée par celui-ci en 1225 et justifiée par la nécessité est précédée d’une intervention d’Honorius III, qui recourt au même argument, et apparaît comme source d’inspiration décisive pour le pouvoir royal. De fait, l’argument de la necessitas comme justification de l’exception est ancré dans une doctrine canonique qu’illustrent le principe necessitas non habet legem , la théorie canonique de la dispense, ou encore diverses occurrences antérieures dans les discours pontificaux. Aussi la taxation de 1225 fait-elle apparaître un véritable mécanisme d’appropriation d’une doctrine canonique par la pratique temporelle, sous l’influence directe de la papauté.
La journée mondiale de l’accident vasculaire cérébral, une opportunité pour les professionnels de développer des compétences en éducation pour la santé
Authors: Jonniaux Sandrine , Margat Aurore 
Published: August 2020

Une équipe pluriprofessionnelle se mobilise chaque année pour la journée mondiale de l’Accident vasculaire cérébral (AVC) afin de prévenir et sensibiliser la population à cette pathologie. Malgré l’absence de formation officielle en promotion de la santé, ces professionnels contribuent aux éducations en santé. Le processus mis en œuvre dans l’organisation et la réalisation de la journée permet-il le développement de compétences éducatives des professionnels impliqués ? Les objectifs de cette recherche étaient d’identifier et catégoriser les compétences éducatives développées lors du processus d’organisation et de mise en œuvre de la journée mondiale AVC, et de cerner les éléments du processus contributifs au développement de ces compétences. Dans cette étude qualitative descriptive, les données ont été recueillies au moyen d’un focus group effectué auprès de professionnels impliqués dans la journée, puis ont fait l’objet d’une analyse de contenu. Cette journée permet le développement de compétences éducatives, elle est pour les professionnels l’occasion de transférer leurs apprentissages. L’organisation mise en place dans le cadre de cette journée est une opportunité d’augmenter le rapport au savoir et le sentiment d’appartenance des professionnels. L’interprofessionnalité et le contexte apprenant permettent le développement d’une attitude éducative. D’autres recherches permettraient de comprendre les conditions de transférabilité du processus.
La pratique infirmière en soins palliatifs auprès de patients atteints de cancer en fin de vie au sein d’une équipe interdisciplinaire : une étude de cas au Liban
Authors: Saouma Nehmé Mona , Desbiens Jean-François , Gagnon Johanne 
Published: August 2020

Au Liban, les infirmières sont peu préparées à délivrer des soins palliatifs (SP), et la pratique dans ce domaine est peu documentée. Cette étude descriptive qualitative visait à comprendre l’exercice de la pratique infirmière en SP auprès de patients cancéreux en fin de vie, au sein d’une équipe interdisciplinaire. Une étude de cas simple a été réalisée auprès de onze infirmières, trois familles, une équipe interdisciplinaire et d’experts nationaux en SP. L’analyse des données effectuée par une double triangulation de méthodes et de sources a mis en relief une relation humaniste empreinte de caring , transcendant les cinq thèmes centraux émergeants : la perception des SP comme un moyen d’offrir une meilleure qualité de vie, la prise en charge globale du patient, l’interdisciplinarité, la spiritualité et l’accompagnement de la famille en SP. Les résultats pourront fournir des assises empiriques pour guider le développement de la pratique infirmière en SP dans le pays.
L’éducation précédant la sortie de l’hôpital : nouvelle forme d’éducation thérapeutique. Critères de qualité et perspectives d’application à notre contexte
Authors: Albano Maria Grazia , Gagnayre Rémi , de Andrade Vincent , d’Ivernois Jean-François 
Published: August 2020

L’ETP sh (Éducation thérapeutique précédant la sortie de l’hôpital) est une pratique développée sous le nom de « discharge education » dans les pays anglo-saxons. Cette nouvelle forme d’éducation thérapeutique s’adresse à des patients aigus ou chroniques et intéresse toutes les spécialités hospitalières ; elle vise à faciliter la transition hôpital-domicile et éviter les réadmissions précoces. Cet examen de 43 études scientifiques porte spécifiquement sur la description, l’analyse et l’évaluation de l’ETP sh, ainsi que sur des recommandations. Près de la moitié des études sont publiées dans des revues de sciences infirmières. L’ETP sh est une intervention éducative intense et brève (de 30 minutes à une heure) délivrée majoritairement dans des situations aiguës. La pédiatrie représente, avec les soins postopératoires, le plus grand nombre de publications. Dans la plupart des études, l’ETP sh se révèle efficace pour améliorer des paramètres cliniques et psychosociaux, réduire les réadmissions précoces, augmenter les compétences et l’observance des patients. Pour atteindre ses buts, l’ETP sh doit être structurée et comporter un suivi systématique. Centrée sur les besoins, les capacités d’apprentissage du patient, elle fait appel à une pédagogie spécifique, interactive, à laquelle les soignants doivent être formés. L’analyse de la recherche internationale ne laisse aucun doute sur les apports positifs de l’ETP sh. Il serait important que soignants et décideurs s’en saisissent comme une opportunité d’améliorer la qualité des soins et de les humaniser.