bluuebunny/crossref_metadata_2025_split huggingface dataset:
Dynamics of prostate protectors assortment in the state formulary of medicines of 1-9 issues
Authors: Gadyak І. V. , Hromovyk B. P. 
Published: October 2018

Prostatitis is one of the most frequent urology diseases of men of reproductive age. Recommendations for rational pharmacotherapy prostatitis are included into the State Formulary of Medicines, which is reviewed and updated annually. Thus, the aim of our work was to study the dynamics of the assortment of prostate protectors.The State Formulary of Medicines of 1–9 issues and the State Register of Medicines of Ukraine dated 01. 08. 2017 were the materials of the research. The methods of search, content analysis, statistics, comparison and generalization were applied. It was established that the first, second and third issues of State Formulary of Medicines include three therapeutic and chemical subgroups of prostate protectors: alpha-adrenergic receptors antagonists (G04CA), testosterone-5-alpha reductase inhibitors (G04CB), other drugs used in benign prostatic hypertrophy (G04CX). And since the fourth issue – only the first two subgroups of prostate protectors were icnluded. Assortment prostate protectors was stabilized in State Formulary of Medicines of 8, 9 issues. Depth of assortment of the State Formulary of Medicines of the ninth issue is 55,8% in comparison with the State Register of Medicines of Ukraine along with 100% index for prostate protectors trade names based on alfuzosin, terazosin (G04CA – Аntagonists of alpha adrenergic receptors), finasteride and dutasteride (G04CB – Inhibitors of testosterone-5-alpha reductase), as well as the absence of drugs based on silodosin, dutasteride-tamsulosin, solifenacin-tamsulosin (G04CA – Antagonists of alpha-adrenergic receptors) and prostate protectors with G04CX – Other drugs used in benign prostatic hypertrophy.
PENGEMBANGAN KURIKULUM BERBASIS KEMAJEMUKAN
Authors: Zaman Kamilus 
Published: October 2018

Guru agama seharusnya menjadikan peserta didik menjadi yang berperadaban, berbudaya, berakhlak, berkarakter, ala Indonesia. dengan menjunjung tinggi nilai-nilai al-qur’an, dan pancasila, menghargai kemajmukan, suku, agama ras, sesuai dengan ajaran Islam yang dibawa Oleh Nabi Muhammad SAW, yang membangun Kota Yastrib menjadi kota Madinah yang didalamnya juga bermajmuk. Sebagai upaya Pengembangan Kurikulum PAI Berbasis Kemajemukan , disini lembaga harus mencoba mengembangkan dan merekontruksi kembali kurikulum Pemerintah dari yang sentralisasi menjadi Desentralisasi, agar Tujuan Pendidikan Agama Islam di lembaga tersebut tercapai, Untuk merealisasikannya Maka:1). Pengembangan kurikulum PAI: pengembangan kurikulum Pendidikan Agama Islam (PAI) dapat berarti: (1) kegiatan menghasilkan kurikulum PAI; atau (2) proses yang mengaitkan satu komponen dengan yang lainnya untuk menghasilkan kurikulum PAI yang lebih baik; dan/atau (3) kegiatan penyusunan (desain), pelaksanaan, penilaian dan penyempur¬naan kurikulum PAI. 2). Langkah-Langkah dalam Pengembangan Kurikulum PAI Berbasis Kemajemukan, dari berbagai Aspek: (1) aspek Tujuan: Menjaga akidah dan ketakwaan peserta didik. 2) Menjadi landasan untuk lebih rajin mempelajari dan mendalami ilmu-ilmu agama. 3) Mendorong peserta didik untuk lebih kritis, kreatif dan inovatif. 4) Menjadi landasan perilaku dalam kehidupan sehari-hari didalam masyarakat. Dengan demikian bukan hanya mengajarkan pengetahuan secara teori semata tetapi juga untuk dipraktekkan atau diamalkan dalam kehidupan sehari-hari (membangun etika sosial). 5) Nasionalis 6) Membentuk Pribadi Muslim (2) Aspek Materi: Memperluas/menambah indikator, Muatan lokal, konten pelajarannya tidak harus sejarah tentang perang dan kesenjangan antara Islam dan non Islam, yang diajarkan karya Tokoh-Tokoh Nusantara. Materi yang disajikan hendaknya lebih bersifat fungsional (3) Aspek Lembaga: Lembaga Pendidikan Agama Islam harus toleran terhadap kemajemukan siswa baik Ras, Suku bahkan Agama.
Optimal and Efficient Streak Detection in Astronomical Images
Authors: Nir Guy , Zackay Barak , Ofek Eran O. 
Published: October 2018

Abstract
Identification of linear features (streaks) in astronomical images is important for several reasons, including: detecting fast-moving near-Earth asteroids; detecting or flagging faint satellites streaks; and flagging or removing diffraction spikes, pixel bleeding, line-like cosmic rays and bad-pixel features. Here we discuss an efficient and optimal algorithm for the detection of such streaks. The optimal method to detect streaks in astronomical images is by cross-correlating the image with a template of a line broadened by the point-spread function of the system. To do so efficiently, the cross-correlation of the streak position and angle is performed using the Radon transform, which is the integral of pixel values along all possible lines through an image. A fast version of the Radon transform exists, which we here extend to efficiently detect arbitrarily short lines. While the brute force Radon transform requires

operations for a N × N image, the fast Radon transform has a complexity of

. We apply this method to simulated images, recovering the theoretical signal-to-noise ratio, and to real images, finding long streaks of low-Earth-orbit satellites and shorter streaks of Global Positioning System satellites. We detect streaks that are barely visible to the eye, out of hundreds of images, without a-priori knowledge of the streaks’ positions or angles. We provide implementation of this algorithm in Python and MATLAB.
Three Pathways for Observed Resonant Chains
Authors: MacDonald Mariah G. , Dawson Rebekah I. 
Published: October 2018

Abstract
A question driving many studies is whether the thousands of exoplanets known today typically formed where we observe them or formed further out in the disk and migrated in. Early discoveries of giant exoplanets orbiting near their host stars and exoplanets in or near mean motion resonances were interpreted as evidence for migration and its crucial role in the beginnings of planetary systems. Long-scale migration has been invoked to explain systems of planets in mean motion resonant chains consisting of three or more planets linked by integer period ratios. However, recent studies have reproduced specific resonant chains in systems via short-scale migration, and eccentricity damping has been shown to capture planets into resonant chains. We investigate whether the observed resonant chains in Kepler-80, Kepler-223, Kepler-60, and TRAPPIST-1 can be established through long-scale migration, short-scale migration, and/or only eccentricity damping by running suites of N-body simulations. We find that, for each system, all three mechanisms are able to reproduce the observed resonant chains. Long-scale migration is not the only plausible explanation for resonant chains in these systems, and resonant chains are potentially compatible with in situ formation.
MOA-2016-BLG-319Lb: Microlensing Planet Subject to Rare Minor-image Perturbation Degeneracy in Determining Planet Parameters
Authors: Han Cheongho , Bond Ian A. , Gould Andrew , Albrow Michael D. , Chung Sun-Ju , Jung Youn Kil , Hwang Kyu-Ha , Lee Chung-Uk , Ryu Yoon-Hyun , Shin In-Gu , Shvartzvald Yossi , Yee Jennifer C. , Cha Sang-Mok , Kim Dong-Jin , Kim Hyoun-Woo , Kim Seung-Lee , Lee Dong-Joo , Lee Yongseok , Park Byeong-Gon , Pogge Richard W. , Kim Chun-Hwey ,   (The KMTNet Collaboration), Abe Fumio , Barry Richard , Bennett David P. , Bhattacharya Aparna , Donachie Martin , Fukui Akihiko , Hirao Yuki , Itow Yoshitaka , Kawasaki Kohei , Kondo Iona , Koshimoto Naoki , Li Man Cheung Alex , Matsubara Yutaka , Muraki Yasushi , Miyazaki Shota , Nagakane Masayuki , Ranc Clément , Rattenbury Nicholas J. , Suematsu Haruno , Sullivan Denis J. , Sumi Takahiro , Suzuki Daisuke , Tristram Paul J. , Yonehara Atsunori ,   (The MOA Collaboration)
Published: October 2018

Abstract
We present the analysis of the planetary microlensing event MOA-2016-BLG-319. The event light curve is characterized by a brief (∼3 days) anomaly near the peak produced by minor-image perturbations. From modeling, we find two distinct solutions that describe the observed light curve almost equally as well. From the investigation of the lens-system configurations, we find that the confusion in the lensing solution is caused by the degeneracy between the two solutions resulting from the source passages on different sides of the planetary caustic. These degeneracies can be severe for major-image perturbations, but it is known that they are considerably less severe for minor-image perturbations. From the comparison of the lens-system configuration with those of two previously discovered planetary events, for which similar degeneracies were reported, we find that the degeneracies are caused by the special source trajectories that passed the star–planet axes at approximately right angles. By conducting a Bayesian analysis, it is estimated that the lens is a planetary system in which a giant planet with a mass

(

) is orbiting a low-mass M-dwarf host with a mass

. Here the planet masses in and out of the parentheses represent the masses for the individual degenerate solutions. The projected host-planet separations are a
⊥ ∼ 0.95 and ∼1.05 au for the two solutions. The identified degeneracy indicates the need to check similar degeneracies in future analyses of planetary lensing events with minor-image perturbations.
Binary Red Supergiants: A New Method for Detecting B-type Companions
Authors: Neugent Kathryn F. , Levesque Emily M. , Massey Philip 
Published: October 2018

Abstract
With the exception of a few well-known and studied systems, the binary population of red supergiants (RSGs) remains relatively uncharacterized. Famous systems such as VV Cep, 31 Cyg, and ζ Aur contain RSG + B star binaries, and here we explore whether B stars are the main type of companion we expect from an evolutionary point of view. Using the Geneva evolutionary models, we find that this is indeed the case. However, few such systems are known, and we use model spectra to determine how easy such binaries would be to detect observationally. We find that it should be quite difficult to hide a B-type companion given a reasonable signal-to-noise in the optical/blue portion of the spectrum. We next examine spectra of Magellanic Cloud RSGs and newly acquired spectra of Galactic RSGs looking for new systems and refining our conclusions about what types of stars could be hidden in the spectra. Finally, we develop a set of photometric criteria that can help select likely binaries in the future without the overhead of large periodic or spectroscopic surveys.
The Gemini/Hubble Space Telescope Galaxy Cluster Project: Stellar Populations in the Low-redshift Reference Cluster Galaxies
Authors: Jørgensen Inger , Chiboucas Kristin , Webb Kristi , Woodrum Charity 
Published: October 2018

Abstract
In order to study stellar populations and galaxy structures at intermediate and high redshift (z = 0.2–2.0) and link these properties to those of low-redshift galaxies, there is a need for well-defined local reference samples. Especially for galaxies in massive clusters, such samples are often limited to the Coma cluster galaxies. We present consistently calibrated velocity dispersions and absorption-line indices for galaxies in the central 2 R
500 × 2 R
500 of four massive clusters at z < 0.1: Abell 426/Perseus, Abell 1656/Coma, Abell 2029, and Abell 2142. The measurements are based on data from the Gemini Observatory, McDonald Observatory, and Sloan Digital Sky Survey. For bulge-dominated galaxies, the samples are 95% complete in Perseus and Coma and 74% complete in A2029 and A2142, to a limit of M
B,abs ≤ −18.5 mag. The data serve as the local reference for our studies of galaxy populations in the higher-redshift clusters that are part of the Gemini/HST Galaxy Cluster Project (GCP). We establish the scaling relations between line indices and velocity dispersions as a reference for the GCP. We derive stellar population parameters, ages, metallicities [M/H], and abundance ratios from line indices, both averaged in bins of velocity dispersion and from individual measurements for galaxies in Perseus and Coma. The zero points of relations between the stellar population parameters and the velocity dispersions limit the allowed cluster-to-cluster variation of the four clusters to ±0.08 dex in age, ±0.06 dex in [M/H], ±0.07 dex in [CN/Fe], and ±0.03 dex in [Mg/Fe].
Marvel Analysis of the Measured High-resolution Rovibronic Spectra of 90Zr16O
Authors: McKemmish Laura K. , Borsovszky Jasmin , Goodhew Katie L. , Sheppard Samuel , Bennett Aphra F. V. , Martin Alfie D. J. , Singh Amrik , Sturgeon Callum A. J. , Furtenbacher Tibor , Császár Attila G. , Tennyson Jonathan 
Published: October 2018

Abstract
Zirconium oxide (ZrO) is an important astrophysical molecule that defines the S-star classification class for cool giant stars. Accurate, empirical rovibronic energy levels, with associated labels and uncertainties, are reported for nine low-lying electronic states of the diatomic

molecule. These 8088 empirical energy levels are determined using the Measured Active Rotational-Vibrational Energy Levels algorithm with 23,317 input assigned transition frequencies, 22,549 of which were validated during this study. A temperature-dependent partition function is presented alongside updated spectroscopic constants for the nine low-lying electronic states.
Actions Are Weak Stellar Age Indicators in the Milky Way Disk
Authors: Beane Angus , Ness Melissa K. , Bedell Megan 
Published: October 2018

Abstract
The orbital properties of stars in the Milky Way disk are signatures of their formation, but they are also expected to change over time due to the dynamical evolution of the Galaxy. Stellar orbits can be quantified by the three dynamical actions, J

r
, L

z
, and J

z
, which provide measures of the orbital eccentricity, guiding radius, and non-planarity, respectively. Changes in these dynamical actions over time reflect the strength and efficiency of the evolutionary processes that drive stellar redistributions. We examine how dynamical actions of stars are correlated with their age using two samples of stars with well-determined ages: 78 solar twin stars (with ages precise to ∼5%) and 4376 stars from the APOKASC2 sample (∼20%). We compute actions using spectroscopic radial velocities from previous surveys and parallax and proper motion measurements from Gaia DR2. We find weak gradients with significant scatter for all actions as a function of stellar age. These gradients and their associated variances provide strong constraints on the efficiency of the mechanisms that drive the redistribution of stellar orbits over time and demonstrate that actions are informative as to stellar age. However, the shallow action–age gradients combined with the large dispersion in each action at a given age render the prospect of age inference from orbits of individual stars bleak. Using the precision measurements of [Fe/H] and [α/Fe] we find that, similarly to our stellar age results, the dynamical actions afford little discriminating power between individual low- and high-α stars.
The Time Evolution of the HH 1 Jet Modeled as a Variable Outflow
Authors: Castellanos-Ramírez A. , Raga A. C. , Rodríguez-González A. 
Published: October 2018

Abstract
The HH 1 jet is a chain of knots extending out to ∼20″ from the VLA 1 source of the HH 1/2 system. Four epochs of [S ii] images obtained with the Hubble Space Telescope over a ∼20 yr period show that these knots have a time-evolving intensity as they travel away from the outflow source. We present an axisymmetric, gas-dynamic simulation of a two-sinusoidal-mode variable ejection velocity jet (including a treatment of the non-equilibrium ionization of the gas) from which we obtain predictions of the time evolution of the chain of knots close to the outflow source. Both the intensity versus position dependence (for the successive knots) and the time evolution of the [S ii] intensities of the individual knots obtained from the simulations agree in a very impressive way with the HH 1 jet observations. This is one of the most striking illustrations of the success of variable jet models at reproducing the observed properties of HH jets. Also, this work represents the first attempted comparison between models and observations of astrophysical jets with both time and spatial resolution.
Fully Coupled Simulation of Cosmic Reionization. III. Stochastic Early Reionization by the Smallest Galaxies
Authors: Norman Michael L. , Chen Pengfei , Wise John H. , Xu Hao 
Published: October 2018

Abstract
Previously we identified a new class of early galaxy that we estimate contributes up to 30% of the ionizing photons responsible for reionization. These are low-mass halos in the range

= 106.5–108

that have been chemically enriched by supernova ejecta from prior Population III star formation. Despite their low star formation rates, these metal cooling halos (MCs) are significant sources of ionizing radiation, especially at the onset of reionization, owing to their high number density and ionizing escape fractions. Here we present a fully coupled radiation hydrodynamic simulation of reionization that includes these MCs, as well the more massive hydrogen atomic line cooling halos. Our method is novel: we perform halo finding in line with the radiation hydrodynamical simulation and assign escaping ionizing fluxes to halos using a probability distribution function (pdf) measured from the galaxy-resolving Renaissance Simulations. The pdf captures the mass dependence of the ionizing escape fraction, as well as the probability that a halo is actively forming stars. With MCs, reionization starts earlier than if only halos of 108

and above are included; however, the redshift when reionization completes is only marginally affected, as this is driven by more massive galaxies. Because star formation is intermittent in MCs, the earliest phase of reionization exhibits a stochastic nature, with small H ii regions forming and recombining. Only later, once halos of mass ∼109

and above begin to dominate the ionizing emissivity, does reionization proceed smoothly in the usual manner deduced from previous studies. This occurs at z ≈ 10 in our simulation.
La formation à l’échelle NBAS comme instrument de cohésion des équipes face à des mères vulnérables et un accès à la relation précoce difficile
Authors: Belot Rose-Angélique , Piquard Caroline , Candilis-Huisman Drina 
Published: October 2018

Si la formation à l’échelle de Brazelton permet d’utiliser cet outil de façon optimale pour l’observation du bébé et le développement des liens père-mère-bébé « classique », la formation apporte également pour chaque utilisateur de la NBAS de nombreux autres repères pour prendre en compte aussi d’autres axes essentiels. La présentation de vignettes cliniques montre l’importance de définir en amont un dispositif précis avec les équipes. Par ailleurs, l’outil Brazelton favorise non seulement au sein d’une équipe l’alliance, mais procure aussi un outil au service du développement des réseaux. Ceux-ci constituent un atout précieux pour l’accès aux relations précoces plus difficiles.
L’anxiété du patient en situation de maladie grave : la réponse palliative
Authors: Mboua Pierre Célestin , Nguepy Keubo François Roger , Bianke Patrice 
Published: October 2018

L’anxiété dans l’attente d’une opération chirurgicale peut s’avérer préoccupante pour la réussite de l’intervention et l’intégrité psychique du patient. Cet article porte sur un cas clinique dont le suivi psychosocial s’est fondé sur le modèle de prise en charge intégrée. L’observation du patient au cours du suivi a mis en évidence un vécu anxieux envahissant. Dans ce contexte, la compétence du patient a été un facteur anxiogène majeur. Il a été mis en évidence le fait que dans une intervention chirurgicale relative à une maladie grave et/ou chronique, « le savoir » du patient, réputé « auxiliaire » de santé peut devenir un facteur de contrainte qu’il faut intégrer dans la réponse globale. Le cas étudié permet de poser les jalons d’un modèle de réponse palliative intégrée dans cette prise en charge qui valorise la notion de compétence du patient.
Sortir de la bulle et entrer dans le rond d’un premier cercle social
Authors: Vamos Julianna 
Published: October 2018

Il est proposé toutes les semaines, à la maternité des Bluets, à Paris, un atelier de rencontre pour les parents et leur nouveau-né : « Hello Baby ! Mais comment naissent les parents ». Pendant leur séjour, les parents sont invités à présenter leur bébé, à échanger autour de leur accouchement et de leur expériences émotionnelles : leur désarroi, leur émerveillement dans la rencontre avec leur bébé. Se tissent alors dans une atmosphère conviviale une écoute groupale et sociale des différents récits de leur vécus. Certaines thèmes émergent régulièrement et résonnent collectivement : la fatigue, le sentiment de solitude, le fantasme de perfection parentale et la culpabilité qui lui est associée.
« Bébé Trucs »
Authors: Breton Joanne 
Published: October 2018

Une formule très simple et conviviale : « Bébé Trucs » est une activité gratuite, ouverte sans rendez-vous aux parents d’enfants entre 0 et 2 ans de Sherbrooke (Québec) et des environs, tous les mercredis entre 13 heures et 16 h 30. Les professionnelles de santé sont sur place pour répondre aux préoccupations des parents, suivre le développement de leur tout-petit, les soutenir pour l’allaitement au besoin, etc.
La Cour Européenne des Droits de l'Homme procède à une condamnation en demi-teinte de la surveillance “de masse”.
Authors: Foegle Jean-Philippe 
Published: October 2018

Particulièrement riche mais également particulièrement décevant, l'arrêt Big Brother Watch pousse à son paroxysme la logique de procéduralisation de la vie privée à l'oeuvre dans le cadre du droit de l'Union Européenne et du droit de la Convention Européenne des Droits de l'Homme. Tout en condamnant un système de surveillance particulièrement intrusif, la Cour Européenne des Droits de l’Homme procède à une légitimation de facto du recours à des systèmes de surveillance digitale « de masse ». De manière similaire, les juges de Strasbourg réaffirment la nécessité d’instaurer un contrôle indépendant des activités de surveillance digitale tout en neutralisant l'exigence d'un contrôle judiciaire préalable de celles-ci