bluuebunny/crossref_metadata_2025_split huggingface dataset:
Faktor-Faktor Yang Berhubungan Dengan Kejadian Infeksi Luka Setelah Dijahit Di Instalasi Gawat Darurat
Authors: Inabulu Maria Veronika , Widani Ni Luh , Rasmada Sada 
Published: July 2022

Luka adalah terputusnya kontinuitas jaringan kulit normal. Penanganan luka robek akibat trauma salah satunya dengan penjahitan, yang berisiko menjadi infeksi karena berbagai faktor. Tujuan penelitian untuk mengetahui faktor-faktor yang berhubungan dengan kejadian infeksi luka setelah dijahit di IGD RSUD Kaimana. Metode penelitian kuantitatif dengan pendekatan deskripsi korelasional dan desain cross-sectional, dilaksanakan pada Bulan Desember 2019-Januari 2020. Pengumpulan data menggunakan kuesioner dan obervasi luka 2 hari post penjahitan. Sampel adalah pasien yang mengalami luka robek baru, berusia ≥ 17 tahun, sebanyak 74 responden, diambil secara total sampling. Hasil analisis univariat: mayoritas luka jahit tidak infeksi 64,9%; pengetahuan baik 93,2%; sikap buruk 52,7%; perilaku buruk 55,4% tentang infeksi luka. Analisis bivariat chi square secara statistik menunjukkan ada hubungan bermakna lokasi luka (p=0,006), riwayat penyakit (p=0,034); (p<0,05) dan tidak ada hubungan usia (p=0,071), lama luka (p=0,156), ukuran luka (p=0,644), pengetahuan (p=0,319), sikap (p=0,732), perilaku (p=0,435);(p>0,05) dengan kejadian infeksi luka setelah dijahit. Kesimpulan: lokasi luka, riwayat penyakit berhubungan dengan kejadian infeksi luka setelah dijahit. Saran: perawatan luka sesuai SOP, monitoring pasien luka di rumah sakit untuk mengurangi angka kejadian infeksi luka setelah dijahit, edukasi perawatan luka di rumah terutama luka pada lokasi yang mudah kotor.
Epidemiology of falls in St. Petersburg (based on research by the Department of Family Medicine)
Authors: Turusheva A. V. , Bogdanova Т. A. , Frolova E. V. , Logunov D. L. , Isaeva Т. V. , Zhelvakova L. Ya. 
Published: July 2022

Introduction:prevention of falls and fractures in older adults is a strategic task of the geriatric service.Aim:to estimate the prevalence of falls and its risk factors, as well as their association with geriatric syndromes in St. Petersburg.Materials and methods:analysis of the results of four studies conducted in St. Petersburg between 2009 and 2019. The total number of participants was 1398 persons aged 60 years and older. Main parameters: comprehensive geriatric assessment, measurement of cardio-ankle vascular index (CAVI) using Vasera VS-1500 volumetric sphygmography computer complex, detection of silent atrial fibrillation using «MyDiagnostick 1001R» device.Results:every third person falls at the age of 65 to 74 years old, and every second person falls at the age of 85 and older. In 50% of cases, falls are accompanied by injuries. The main factors associated with a higher risk of falls were arterial hypertension, atrial fibrillation, stroke/transient ischemic attack, cognitive impairment, sensory deficits, urinary incontinence, decreased physical functioning and CAVI above predicted value. Vision correction reduced the risk of falls by 46.7%, improved/good nutrition status according to self-assessment data by 55.3%, correction of urinary incontinence by 55.8%, improved cognitive functioning by 73.3%, and eating two or more fruits and vegetables a day by 66.0%. Individualized analysis of fall risk factors and development of fall prevention programs can reduce the risk of falls by a factor of nine within the first year.Conclusion:Screening to assess the risk of falls and compiling individual fall prevention programs can significantly reduce the risk of falls in older and senile age. The effectiveness of individual fall risk reduction programs decreases after the first year of implementation. Consequently, it is necessary to conduct annual screening of older patients to assess the risk of falls and subsequent adjustment of personalized fall prevention plan.
On the Energy Dependence of Galactic Cosmic Ray Anisotropies in the Very Local Interstellar Medium
Authors: Nikoukar Romina , Hill Matthew E. , Brown Lawrence , Kota Jozsef , Decker Robert B. , Dialynas Konstantinos , Hamilton Douglas C. , Krimigis Stamatios M. , Lasley Scott , Roelof Edmond C. , Mitchell J. Grant , Florinski Vladimir. , Giacalone Joe. , Richardson John , Opher Merav 
Published: July 2022

Abstract
We report on the energy dependence of Galactic cosmic rays (GCRs) in the very local interstellar medium (VLISM) as measured by the Low Energy Charged Particle (LECP) instrument on the Voyager 1 spacecraft. The LECP instrument includes a dual-ended solid-state detector particle telescope mechanically scanning through 360° across eight equally spaced angular sectors. As reported previously, LECP measurements showed a dramatic increase in GCR intensities for all sectors of the ≥211 MeV count rate (CH31) at the Voyager 1 heliopause (HP) crossing in 2012; however, since then the count rate data have demonstrated systematic episodes of intensity decrease for particles around 90° pitch angle. To shed light on the energy dependence of these GCR anisotropies over a wide range of energies, we use Voyager 1 LECP count rate and pulse height analyzer (PHA) data from ≥211 MeV channel together with lower-energy LECP channels. Our analysis shows that, while GCR anisotropies are present over a wide range of energies, there is a decreasing trend in the amplitude of second-order anisotropy with increasing energy during anisotropy episodes. A stronger pitch angle scattering at higher velocities is argued as a potential cause for this energy dependence. A possible cause for this velocity dependence arising from weak rigidity dependence of the scattering mean free path and resulting velocity-dominated scattering rate is discussed. This interpretation is consistent with a recently reported lack of corresponding GCR electron anisotropies.
Asteroseismology of the DAV Star L19-2
Authors: Chen Yanhui 
Published: July 2022

Abstract
L19-2 is a DAV star, which was intermittently observed from 1976 to 2013. Five independent pulsation modes of 350, 192, 143, 118, and 113 s are identified. The five modes can be used to constrain the fitting models. The rates of period change can be obtained through the O–C method for the modes of 192 and 113 s, which can be used to study the evolution effect of DAV stars. Using the White Dwarf Evolution Code (WDEC; 2018 version), a large sample of DAV star models are evolved. The theoretical modes are calculated and used to fit the observed modes. After fine model fittings, we obtain an optimal model with an absolute difference of Φ = 0.06 s. By parameterizing the core oxygen profile, the WDEC procedure can greatly reduce the fitting error of asteroseismological models. According to our optimal model, the distance obtained through the model luminosity is only 1% different from that reported by the Gaia Data Release 2. L19-2 is a massive and hot DAV star with a relatively thick H atmosphere and a thick He layer. The stellar parameters and the rates of period change of our optimal model are slightly modified from that of the previous work. Our optimal model has a large central oxygen abundance. The central oxygen abundance is strongly correlated with the previous physical process of stellar evolution. A lot of asteroseismological work on white dwarfs presents an opportunity to explore the progenitor stars.
A Novel Solution for Resonant Scattering Using Self-consistent Boundary Conditions
Authors: McClellan B. Connor , Davis Shane W. , Arras Phil 
Published: July 2022

Abstract
We present two novel additions to the semianalytic solution of Lyα radiative transfer in spherical geometry: (1) implementation of the correct boundary condition for a steady source, and (2) solution of the time-dependent problem for an impulsive source. For the steady-state problem, the solution can be represented as a sum of two terms: a previously known analytic solution of the equation with mean intensity J = 0 at the surface, and a novel, semianalytic solution which enforces the correct boundary condition of zero-ingoing intensity at the surface. This solution is compared to that of the Monte Carlo method, which is valid at arbitrary optical depth. It is shown that the size of the correction is of order unity when the spectral peaks approach the Doppler core and decreases slowly with line center optical depth, specifically as

(
a

τ

0

)

−
1

/

3

, which may explain discrepancies seen in previous studies. For the impulsive problem, the time, spatial, and frequency dependence of the solution are expressed using an eigenfunction expansion in order to characterize the escape time distribution and emergent spectra of photons. It is shown that the lowest-order eigenfrequency agrees well with the decay rate found in the Monte Carlo escape time distribution at sufficiently large line center optical depths. The characterization of the escape time distribution highlights the potential for a Monte Carlo acceleration method, which would sample photon escape properties from distributions rather than calculating every photon scattering, thereby reducing computational demand.
Quantifying Properties of Photospheric Magnetic Cancellations in the Quiet Sun Internetwork
Authors: Ledvina Vincent E. , Kazachenko Maria D. , Criscuoli Serena , Tilipman Dennis , Ermolli Ilaria , Falco Mariachiara , Guglielmino Salvatore , Jafarzadeh Shahin , van der Voort Luc Rouppe , Zuccarello Francesca 
Published: July 2022

Abstract
We analyzed spectropolarimetric data from the Swedish 1 m Solar Telescope to investigate the physical properties of small-scale magnetic cancellations in the quiet Sun photosphere. Specifically, we looked at the full Stokes polarization profiles along the Fe i 557.6 nm and of the Fe i 630.1 nm lines measured by the CRisp Imaging SpectroPolarimeter to study the temporal evolution of the line-of-sight magnetic field during 42.5 minutes of quiet Sun evolution. From this magnetogram sequence, we visually identified 38 cancellation events. We then used the Yet Another Feature Tracking Algorithm to characterize the physical properties of these magnetic cancellations. We found on average 1.6 × 1016 Mx of magnetic flux canceled in each event with an average cancellation rate of 3.8 × 1014 Mx s−1. The derived canceled flux is associated with strong downflows, with an average speed of V
LOS ≈ 1.1 km s−1. Our results show that the average lifetime of each event is 9.2 minutes with an average of 44.8% of initial magnetic flux being canceled. Our estimates of magnetic fluxes provide a lower limit since studied magnetic cancellation events have magnetic field values that are very close to the instrument noise level. We observed no horizontal magnetic fields at the cancellation sites and therefore cannot conclude whether the events are associated with structures that could cause magnetic reconnection.
On the Energy Dispersion of Magnetic Rossby Waves
Authors: Li 李 Yaokun 耀锟 
Published: July 2022

Abstract
The energy dispersion of magnetic Rossby waves has been investigated by applying the two-dimensional incompressible magnetohydrodynamic (MHD) equations in both uniform basic flow and basic magnetic field. The dispersion relation suggests that the magnetic Rossby waves can be divided into fast- and slow-propagating modes, respectively. The fast-propagating mode propagates eastward and is similar to the fast Alfvén waves. The energy dispersion speed is faster than the phase speed, which means the perturbation energy can lead the perturbations themselves to arrive downstream. The slow-propagating waves with smaller (larger) horizontal scales are similar to those of the slow Alfvén waves (Rossby waves). The zonal group velocity is slower than the zonal phase speed for the slow-propagating magnetic Rossby waves. For the slow-propagating waves that propagate eastward, this means that the perturbation energy may trigger new perturbations that are located upstream of the perturbations themselves. The group velocity vector is basically same as (opposite of) the wavevector for the fast-propagating (slow-propagating) magnetic Rossby waves that propagate eastward. The endpoints of the group velocity vectors and the wavevector multiplying a factor are located on a cycle in the wavenumber space. Due to the uniform basic flow and the uniform basic magnetic field, the energy dispersion paths (called rays) are straight lines. Along the straight-line rays, the wave action, wave energy, and amplitude keep their initial values, and the wave neither develops nor decays.
Heliospheric Compression Due to Recent Nearby Supernova Explosions
Authors: Miller Jesse A. , Fields Brian D. 
Published: July 2022

Abstract
The widespread detection of 60Fe in geological and lunar archives provides compelling evidence for recent nearby supernova explosions within ∼100 pc at 3 and 7 Myr ago. The blasts from these explosions had a profound effect on the heliosphere. We perform new calculations to study the compression of the heliosphere due to a supernova blast. Assuming a steady but non-isotropic solar wind, we explore a range of properties appropriate for supernova distances inspired by recent 60Fe data, and for a 20 pc supernova proposed to account for mass extinctions at the end-Devonian period. We examine the locations of the termination shock decelerating the solar wind and the heliopause that marks the boundary between the solar wind and supernova material. Pressure balance scaling holds, consistent with studies of other astrospheres. Solar wind anisotropy does not have an appreciable effect on shock geometry. We find that supernova explosions at 50 pc (95 pc) lead to heliopause locations at 16 au (23 au) when the forward shock arrives. Thus, the outer solar system was directly exposed to the blast, but the inner planets—including Earth—were not. This finding reaffirms that the delivery of supernova material to Earth is not from the blast plasma itself, but likely is from supernova dust grains. After the arrival of the forward shock, the weakening supernova blast will lead to a gradual rebound of the heliosphere, taking ∼few

×

100 kyr to expand beyond 100 au. Prospects for future work are discussed.
Single-pulse Variability in Gamma-Ray Pulsars
Authors: Kerr M. 
Published: July 2022

Abstract
The Fermi Large Area Telescope receives ≪1 photon per rotation from any γ-ray pulsar. However, out of the billions of monitored rotations of the bright pulsars Vela (PSR J0835−4510) and Geminga (PSR J0633+1746), a few thousand have ≥2 pulsed photons. These rare pairs encode information about the variability of pulse amplitude and shape. We have cataloged such pairs and find the observed number to be in good agreement with simple Poisson statistics, limiting any amplitude variations to <19% (Vela) and <22% (Geminga) at 2σ confidence. Using an array of basis functions to model pulse-shape variability, the observed pulse phase distribution of the pairs limits the scale of pulse-shape variations of Vela to <13%, while for Geminga we find a hint of ∼20% single-pulse-shape variability most associated with the pulse peaks. If variations last longer than a single rotation, more pairs can be collected, and we have calculated upper limits on amplitude and shape variations for assumed coherence times up to 100 rotations, finding limits of ∼1% (amplitude) and ∼3% (shape) for both pulsars. Because a large volume of the pulsar magnetosphere contributes to γ-ray pulse production, we conclude that the magnetospheres of these two energetic pulsars are stable over one rotation and very stable on longer timescales. All other γ-ray pulsars are too faint for similar analyses. These results provide useful constraints on rapidly improving simulations of pulsar magnetospheres, which have revealed a variety of large-scale instabilities in the thin equatorial current sheets where the bulk of GeV γ-ray emission is thought to originate.
New Theoretical Period–Luminosity–Metallicity Relations for RR Lyrae in the Rubin-LSST Filters
Authors: Marconi Marcella , Molinaro Roberto , Dall’Ora Massimo , Ripepi Vincenzo , Musella Ilaria , Bono Giuseppe , Braga Vittorio , Di Criscienzo Marcella , Fiorentino Giuliana , Leccia Silvio , Monelli Matteo 
Published: July 2022

Abstract
The revolutionary power of future Rubin-LSST observations will allow us to significantly improve the physics of pulsating stars, including RR Lyrae. In this context, an updated theoretical scenario predicting all the relevant pulsation observables in the corresponding photometric filters is mandatory. The bolometric light curves are based on a recently computed extensive set of nonlinear convective pulsation models for RR Lyrae stars, covering a broad range of metal content, and have been transformed into the Vera C. Rubin Observatory Legacy Survey of Space and Time (Rubin-LSST) photometric system. Predicted Rubin-LSST mean magnitudes and pulsation amplitudes have been adopted to build the Bailey diagrams (luminosity amplitude versus period) and the color–color diagrams in these bands. The current findings indicate that the g
LSST–r
LSST and r
LSST–i
LSST colors obey to a well-defined linear relation with the metal content. Moreover, the period–luminosity relations display in the reddest filters (r
LSST, i
LSST, z
LSST, y
LSST) a significant dependence on the assumed metal abundance. In particular, more metal-rich RR Lyrae are predicted to be fainter at a fixed period. Metal-dependent period–Wesenheit relations for different combinations of optical and near-infrared filters are also provided. These represent powerful tools to infer individual distances independently of reddening uncertainties, once the metal abundance is known and no relevant deviations from the adopted extinction law occur. Finally, we also derived new linear and quadratic absolute magnitude metallicity relations (g
LSST versus [Fe/H]) and the metallicity coefficient is consistent with previous findings concerning the B and the V band.
Metallicity Properties of the Galactic Bulge Stars Near and Far: Expectations from the Auriga Simulation
Authors: Chen Bin-Hui , Li Zhao-Yu 
Published: July 2022

Abstract
Using the high-resolution Milky Way–like model from Auriga simulation we study the chemical properties of the Galactic bulge, focusing on the metallicity difference between stars on the near side (in front of the Galactic center) and the far side (behind the Galactic center). In general, along certain sight lines the near side is more metal-rich than the far side, consistent with the negative vertical metallicity gradient of the disk, since the far side is located higher above the disk plane than the near side. However, at the region l < 0° and ∣b∣ ≤ 6°, the near side is even more metal-poor than the far side, and their difference changes with the Galactic longitude. This is mainly due to the fact that stars near the minor axis of the bar are more metal-poor than that around the major axis. Since the bar is tilted, in the negative longitude region, the near side is mainly populated by stars close to the minor-axis region rather than the far side resulting in such a metallicity difference. We extract stars in the X-shape structure by identifying the overdensities in the near and far sides. Their metallicity properties are consistent with the results of the whole Galactic bulge. The boxy/peanut-shaped bulge can naturally explain the metallicity difference of the double red clump stars in the observation. There is no need to involve a classical bulge component with different stellar populations.
De l’utopie !
Authors: Macherey Pierre , Roman Sébastien 
Published: July 2022

Pierre Macherey est philosophe, professeur honoraire à l’université de Lille. Rattaché à l’UMR « Savoirs Textes Langage » du CNRS, il continue d’animer un blog « La philosophie au sens large » dont les travaux sont publiés sur le net ( https://philolarge.hypotheses.org/ ). Il a écrit de nombreux ouvrages, aussi bien en philosophie (sur Spinoza, Hegel, Marx, Comte, Canguilhem, Foucault) qu’en littérature et sur la manière de philosopher avec la littérature ( Philosopher avec la littérature est la reprise de sa thèse soutenue en 1991 ; mais il y a aussi, par exemple : Proust. Entre littérature et philosophie ; En lisant Jules Verne ). Son dernier ouvrage s’intitule À l’essai (Paris, Kimé, 2019). Sur l’utopie, il a notamment écrit : De l’utopie ! (Le Havre, De l’incidence éditeur, 2011) ainsi que « Utopie et quotidien : les deux faces d’une même réalité ? », article publié dans Peggy Avez, Louis Carré et Sébastien Laoureux (dir.), Utopie et quotidien. Autour de Pierre Macherey (Bruxelles, Presses de l’Université Saint Louis, 2016).
Marketing et communication politique
Authors: Selmi Refk 
Published: July 2022

La 26 e Conférence des Nations unies sur le changement climatique à Glasgow, connue sous le nom de COP26, est un rendez-vous très important cinq ans après la COP21 au cours de laquelle plus de 2 000 gouvernements et entreprises ont pris l’engagement historique du 0 impact en se fixant des objectifs climatiques et énergétiques exigeants (COP21). Mais ces objectifs restent trop bas pour empêcher efficacement le pire des scénarios de changement climatique. Atteindre les objectifs climatiques de Paris en 2015 nécessite une décarbonation rapide des systèmes énergétiques dans le monde. Indépendamment du développement rapide et dynamique des marchés des énergies renouvelables dans le monde, la transition vers l’énergie durable reste un processus fortement politique. L’adoption de politiques et de réglementations appropriées et rapides semble d’une importance primordiale pour permettre le développement et la diffusion de technologies durables et pour conduire l’action climatique. Le soutien politique est indispensable pour légitimer des solutions politiques ambitieuses. Les gouvernements doivent promettre des réductions plus strictes des gaz à effet de serre pour lutter contre les conséquences des hausses nocives de la température mondiale. Même si les membres européens se sont publiquement engagés en faveur du Green Deal européen, ils sont divisés sur différentes questions critiques, notamment le mécanisme d’ajustement aux frontières carbone (MACF) proposé, le rôle de l’énergie nucléaire dans le futur bouquet énergétique de l’Europe, les technologies de transition dans la transition vers le zéro impact, ainsi que les impacts socio-économiques de la décarbonation du secteur de l’énergie ou de la transition vers une économie bas carbone. Dans l’ensemble, les politiques et les programmes restent à un stade de formation et l’incertitude politique est très élevée. Ce chapitre vise premièrement à comparer les plans climat menés par les différents États membres européens définissant des mesures pour garantir l’atteinte des objectifs de Paris. Deuxièmement à évaluer si certains gouvernements ont réagi plus rapidement que d’autres. Troisièmement, à identifier les principaux obstacles à la réalisation des objectifs climatiques et énergétiques. Et enfin, à fournir des réponses politiques possibles que les gouvernements peuvent prendre pour garantir que les mesures d’urgence, mises en œuvre pour faire face à la crise actuelle de la Covid, n’altèrent pas la transition environnementale.
Universitarisation des formations des auxiliaires médicaux en Normandie Occidentale : retour d’expérience
Authors: Lenesley Pauline , Bitker Catherine , Touzé Emmanuel 
Published: July 2022

Les métiers paramédicaux souffrent d’un manque d’attractivité, notamment en raison de perspectives d’évolution de carrière limitées. L’universitarisation des formations paramédicales constitue un enjeu majeur pour ces professions. Cependant, le processus est complexe, regroupant à la fois des dimensions pédagogiques, institutionnelles et professionnelles. Nous présentons ici la construction d’une expérimentation d’universitarisation selon le décret du 11 mai 2020. Nous montrons comment la dynamique de co-construction peut se mettre en place entre université et instituts de formation professionnalisants pour offrir aux étudiants des formations paramédicales les droits étudiants et les perspectives de toutes les formations universitaires.