bluuebunny/crossref_metadata_2025_split huggingface dataset:
Authors: Abdullah Abdullah , Usman Usman , Efendi M 
Published: March 2018

<p class="Judul2">Abstrak</p><p>Klasifikasi kualitas kopra dengan bantuan komputer menggunakan pengolahan citra dapat membantu mempercepat pekerjaan manusia. Teknik data mining dapat dimanfaatkan untuk klasifikasi kualitas kopra berdasarkan warna RGB (<em>red, green, blue</em>) dan tekstur (<em>energy, contrast, correlation, homogeneity</em>), . Permasalahannya adalah kesulitan dalam memprediksi kualitas kopra dalam kelas A (80-85%), kelas B (70-75%) dan kelas C (60-65%). Tujuan dari penelitian ini ialah membangun aplikasi untuk klasifikasi kualitas kopra berdasarkan warna dan tekstur. Adapun metode klasifikasi yang digunakan adalah <em>n</em><em>earest </em><em>m</em><em>ean </em><em>c</em><em>lassifier</em> (NMC). Sebelum proses klasifikasi dilakukan praproses <em>background subtraction </em>dengan metode pixel subtraction untuk memisahkan objek dengan latarnya. Manfaat dari penelitian ini antara lain dapat menghemat waktu dalam melakukan klasifikasi kualitas kopra dan dapat mempermudah penentuan harga jual beli kopra. Berdasarkan hasil evaluasi metode <em>cross</em><em> </em><em>validation</em> diperoleh ketelitian rata-rata adalah 80.67% dengan simpangan baku 1.17%.</p><p> <strong><em>Kata Kunci</em></strong><em>: Klasifikasi, </em><em>citra, kopra, n</em><em>earest </em><em>m</em><em>ean </em><em>c</em><em>lassifier</em><em>, pixel subtraction, warna RGB, tekstur</em></p><p><em><br /></em></p><p class="Judul2">Abstract</p><p class="Abstract">The classification of copra quality with the help of computer by using image processing can help to speed up human work. Data mining techniques can be utilized for copra quality classification based on RGB color (red, green, blue) and texture (energy, contrast, correlation, homogeneity). The problem is the difficulty in predicting the quality of copra in grade of A (80-85%), grade of B (70-75%) and grade of C (60-65%). The purpose of this study is to develope an application for the classification of copra quality based on color and texture. The method used is the nearest mean classifier (NMC). Preprocessing is done before the classification process for background subtraction by using pixel subtraction method to separate the image of object against the background. The benefits of this research are it can save time in classifying the quality of copra and can facilitate the determination of copra price. Based on the evaluation result by using cross validation method obtained the average accuracy is 80.67% with standard deviation is 1.17%.</p><p> <strong>Keywords</strong>: <em>c</em><em>lassification, </em><em>image, copra, nearest </em><em>mean </em><em>classifier,</em><em> </em><em>pixel subtraction, RGB color, texture</em><em> </em></p>
Hastanemizde 2014-2017 yıllarında üreyen Corynebacterium izolatlarının değerlendirilmesi
Authors: TANRIVERDİ Yeliz , KORKMAZ Ferhan , BİRİNCİ Asuman 
Published: March 2018

Amaç: Corynebacterium türlerinin çoğu deri ve mukoz membranların florasında bulunmaktadır. Genellikle fırsatçı enfeksiyon etkenidirler ve patojenik potansiyelleri kontaminasyon ve kolonizasyondan dolayı çok uzun yıllar göz ardı edilmiştir. Son yıllarda, uygulanan invaziv işlemlerin, geniş spektrumlu antibiyotik kullanımının ve immünsupresif hasta sayısının artması Corynebacterium cinsi bakterilere bağlı enfeksiyonların sayısında artışa neden olmuştur. Bu çalışmada amacımız son 3 yılda hastanemizde etken olarak kabul edilen Corynebacterium cinsi bakterilerin duyarlılığını ortaya koymak ve son yıllarda enfeksiyon oranlarındaki artışa dikkat çekmektir.Yöntem: Çalışmamızda Ocak 2014 ile Aralık 2016 yılları arasında çeşitli kliniklerden laboratuvarımıza gönderilen örnekler incelenmiştir. Etken olarak kabul edilen örnekler çalışmaya alınmıştır. Tür düzeyinde tanımlanma Vitek MS (Biomeriux, Fransa) otomotize sistemle antibiyotik duyarlılıkları ise Kirby Bauer disk difüzyon yöntemiyle belirlenmiştir. Sonuçlar EUCAST (The European Committee on Antimicrobial Susceptibility Testing) önerileri doğrultusunda değerlendirilmiştir.Bulgular: Toplam 199 Corynebacterium izolatı (C. amycolatum n=3, C. jeikeum n=7, C. striatum n=123, Corynebacterium spp. n=66) izole edilmiştir. Corynebacterium cinsi bakteriler en çok alt solunum yollarına ait örneklerden (%55,2) izole edilirken, ikinci sırayı yara kültürü almıştır. En çok örnek dahili bilimlerden (%53,2) gelmiş olmakla beraber yoğun bakım ünitelerinde yıllara göre azalma dikkat çekmektedir. Tüm izolatlarda antibiyotik duyarlılık testine göre çoklu ilaç direnci olduğu görülmüştür. Linezolide dirençli bir suş saptanmışken vankomisine direnç saptanmamıştır. En sık direnç siprofloksasine(%97,7) karşı gelişmiştir.Sonuç: Laboratuvarımızda Corynebacterium izolatlarının son yıllarda gittikçe artması ve çoklu ilaç direncinin olması dikkat çekmektedir. Risk faktörlerinin artması Corynebacterium enfeksiyonlarının artışına sebep olmaktadır. Laboratuvara gelen örnekler etken-kolonizasyon-kontaminasyon açısından değerlendirilmeli, gerekli durumlarda klinisyen ile iletişime geçilmeli, etken kabul edilen izolatlara mutlaka identifikasyon yapılıp duyarlılık çalışılmalı ve duyarlılık sonucuna göre uygun tedavi protokolü oluşturulmalıdır.
Study on a Ternary Surfactant System of Disodium Hexadecyl Diphenyl Ether Disulfonate, Dodecyldimethyl Hydroxyethyl Ammonium Chloride and Fatty Alcohol Polyoxyethylene Ether
Authors: Li Xiaobang , Xu Hujun , Ding Zhenjun 
Published: March 2018

AbstractThis study was focused on a ternary complex system composed of hexadecyl diphenyl ether disulfonate (C16-MADS), dodecyl dimethyl hydroxyethyl ammonium chloride (K3) and fatty alcohol polyoxyethylene ether (AEO9). The binary mixture C-K consisting of C16-MADS and K3 was investigated and the maximum synergism was obtained when the mole ratio was 0.33:0.67. Subsequently, AEO9 was added to the binary C-K complex system to investigate whether the behavior of the new complex system, in which C-K is thought to be a surfactant, can be explained by the theory of regular solution. The maximum synergism was achieved when the molar ratio of C-K and AEO9 was 7:3. The regular solution theory could well explain the synergism in mixed micelle formation and the synergism in surface tension reduction efficiency, but the synergism in surface tension reduction effectiveness did not match with the experimental data. So, there still exist some deficiencies in the application of the regular solution theory to a complex system of three surfactants.
Comparative study of antibacterial properties of polystyrene films with TiOx and Cu nanoparticles fabricated using cluster beam technique
Authors: Popok Vladimir N , Jeppesen Cesarino M , Fojan Peter , Kuzminova Anna , Hanuš Jan , Kylián Ondřej 
Published: March 2018

Background: Antibacterial materials are of high importance for medicine, and for the production and conservation of food. Among these materials, polymer films with metal nanoparticles (NPs) are of considerable interest for many practical applications.Results: The paper describes a novel approach for the formation of bactericidal polymer thin films (polystyrene in this case), produced by spin-coating, with Ti and Cu NPs deposited from cluster beams. Ti NPs are treated in three different ways in order to study different approaches for oxidation and, thus, efficiency in formation of the particles with semiconducting properties required for the catalytic formation of reactive oxygen species. Cu NPs are used as deposited. Partial NP embedding into polystyrene is realised in a controllable manner using thermal annealing in order to improve surface adhesion and make the particles resistant against wash-out. The formed composite films with TiOx and Cu species are tested as bactericidal media using E.coli bacteria as model microorganisms.Conclusion: The obtained results show considerable efficiency in destroying the bacteria and a good possibility of multiple re-use of the same composite films making the suggested approach attractive for the cases requiring reusable polymer-based antibacterial media.
Shallow Transits—Deep Learning. I. Feasibility Study of Deep Learning to Detect Periodic Transits of Exoplanets
Authors: Zucker Shay , Giryes Raja 
Published: March 2018

Abstract
Transits of habitable planets around solar-like stars are expected to be shallow, and to have long periods, which means low information content. The current bottleneck in the detection of such transits is caused in large part by the presence of red (correlated) noise in the light curves obtained from the dedicated space telescopes. Based on the groundbreaking results deep learning achieves in many signal and image processing applications, we propose to use deep neural networks to solve this problem. We present a feasibility study, in which we applied a convolutional neural network on a simulated training set. The training set comprised light curves received from a hypothetical high-cadence space-based telescope. We simulated the red noise by using Gaussian Processes with a wide variety of hyper-parameters. We then tested the network on a completely different test set simulated in the same way. Our study proves that very difficult cases can indeed be detected. Furthermore, we show how detection trends can be studied and detection biases quantified. We have also checked the robustness of the neural-network performance against practical artifacts such as outliers and discontinuities, which are known to affect space-based high-cadence light curves. Future work will allow us to use the neural networks to characterize the transit model and identify individual transits. This new approach will certainly be an indispensable tool for the detection of habitable planets in the future planet-detection space missions such as PLATO.
Revisiting the Phase Curves of WASP-43b: Confronting Re-analyzed Spitzer Data with Cloudy Atmospheres
Authors: Mendonça João M. , Malik Matej , Demory Brice-Olivier , Heng Kevin 
Published: March 2018

Abstract
Recently acquired Hubble and Spitzer phase curves of the short-period hot Jupiter WASP-43b make it an ideal target for confronting theory with data. On the observational front, we re-analyze the 3.6 and 4.5 μm Spitzer phase curves and demonstrate that our improved analysis better removes residual red noise due to intra-pixel sensitivity, which leads to greater fluxes emanating from the nightside of WASP-43b, thus reducing the tension between theory and data. On the theoretical front, we construct cloud-free and cloudy atmospheres of WASP-43b using our Global Circulation Model (GCM), THOR, which solves the non-hydrostatic Euler equations (compared to GCMs that typically solve the hydrostatic primitive equations). The cloud-free atmosphere produces a reasonable fit to the dayside emission spectrum. The multi-phase emission spectra constrain the cloud deck to be confined to the nightside and have a finite cloud-top pressure. The multi-wavelength phase curves are naturally consistent with our cloudy atmospheres, except for the 4.5 μm phase curve, which requires the presence of enhanced carbon dioxide in the atmosphere of WASP-43b. Multi-phase emission spectra at higher spectral resolution, as may be obtained using the James Webb Space Telescope, and a reflected-light phase curve at visible wavelengths would further constrain the properties of clouds in WASP-43b.
Fundamental Properties of Co-moving Stars Observed by Gaia
Authors: Bochanski John J. , Faherty Jacqueline K. , Gagné Jonathan , Nelson Olivia , Coker Kristina , Smithka Iliya , Desir Deion , Vasquez Chelsea 
Published: March 2018

Abstract
We have estimated fundamental parameters for a sample of co-moving stars observed by Gaia and identified by Oh et al. We matched the Gaia observations to the 2MASS and Wide-Field Infrared Survey Explorer catalogs and fit MIST isochrones to the data, deriving estimates of the mass, radius, [Fe/H], age, distance, and extinction to 9754 stars in the original sample of 10606 stars. We verify these estimates by comparing our new results to previous analyses of nearby stars, examining fiducial cluster properties, and estimating the power-law slope of the local present-day mass function. A comparison to previous studies suggests that our mass estimates are robust, while metallicity and age estimates are increasingly uncertain. We use our calculated masses to examine the properties of binaries in the sample and show that separation of the pairs dominates the observed binding energies and expected lifetimes.
Ab-initio Pulsar Magnetosphere: Particle Acceleration in Oblique Rotators and High-energy Emission Modeling
Authors: Philippov Alexander A. , Spitkovsky Anatoly 
Published: March 2018

Abstract
We perform global particle-in-cell simulations of pulsar magnetospheres, including pair production, ion extraction from the surface, frame-dragging corrections, and high-energy photon emission and propagation. In the case of oblique rotators, the effects of general relativity increase the fraction of the open field lines that support active pair discharge. We find that the plasma density and particle energy flux in the pulsar wind are highly non-uniform with latitude. A significant fraction of the outgoing particle energy flux is carried by energetic ions, which are extracted from the stellar surface. Their energies may extend up to a large fraction of the open field line voltage, making them interesting candidates for ultra-high-energy cosmic rays. We show that pulsar gamma-ray radiation is dominated by synchrotron emission, produced by particles that are energized by relativistic magnetic reconnection close to the Y-point and in the equatorial current sheet. In most cases, the calculated light curves contain two strong peaks, which is in general agreement with Fermi observations. The radiative efficiency decreases with increasing pulsar inclination and increasing efficiency of pair production in the current sheet, which explains the observed scatter in L

γ
versus

. We find that the high-frequency cutoff in the spectra is regulated by the pair-loading of the current sheet. Our findings lay the foundation for quantitative interpretation of Fermi observations of gamma-ray pulsars.
Properties of Short Gamma-ray Burst Pulses from a BATSE TTE GRB Pulse Catalog
Authors: Hakkila Jon , Horváth István , Hofesmann Eric , Lesage Stephen 
Published: March 2018

Abstract
We analyze pulse properties of short gamma-ray bursts (GRBs) from a new catalog containing 434 pulses from 387 BATSE time-tagged event (TTE) GRBs. Short GRB pulses exhibit correlated properties of duration, fluence, hardness, and amplitude, and they evolve hard to soft while undergoing similar triple-peaked light curves similar to those found in long/intermediate bursts. We classify pulse light curves using their temporal complexities, demonstrating that short GRB pulses exhibit a range of complexities from smooth to highly variable. Most of the bright, hard, chaotic emission seen in complex pulses seems to represent a separate highly variable emission component. Unlike long/intermediate bursts, as many as 90% of short GRBs are single-pulsed. However, emission in short multipulsed bursts is coupled such that the first pulse’s duration is a predictor of both the interpulse separation and subsequent pulse durations. These results strongly support the idea that external shocks produce the prompt emission seen in short GRBs. The similarities between the triple-peaked structures and spectral evolution of long, short, and intermediate GRBs then suggests that external shocks are responsible for the prompt emission observed in all GRB classes. In addition to these findings, we identify a new type of gamma-ray transient in which peak amplitudes occur at the end of the burst rather than at earlier times. Some of these “crescendo” bursts are preceded by rapid-fire “staccato” pulses, whereas the remaining are preceded by a variable episode that could be unresolved staccato pulses.
ALMA’s Polarized View of 10 Protostars in the Perseus Molecular Cloud
Authors: Cox Erin G. , Harris Robert J. , Looney Leslie W. , Li Zhi-Yun , Yang Haifeng , J. Tobin John , Stephens Ian 
Published: March 2018

Abstract
We present 870 μm ALMA dust polarization observations of 10 young Class 0/I protostars in the Perseus Molecular Cloud. At ∼0.″35 (80 au) resolution, all of our sources show some degree of polarization, with most (9/10) showing significantly extended emission in the polarized continuum. Each source has incredibly intricate polarization signatures. In particular, all three disk-candidates have polarization vectors roughly along the minor axis, which is indicative of polarization produced by dust scattering. On ∼100 au scales, the polarization is at a relatively low level (≲1%) and is quite ordered. In sources with significant envelope emission, the envelope is typically polarized at a much higher (≳5%) level and has a far more disordered morphology. We compute the cumulative probability distributions for both the small (disk-scale) and large (envelope-scale) polarization percentage. We find that the two are intrinsically different, even after accounting for the different detection thresholds in the high/low surface brightness regions. We perform Kolmogorov–Smirnov and Anderson–Darling tests on the distributions of angle offsets of the polarization from the outflow axis. We find disk-candidate sources are different from the non-disk-candidate sources. We conclude that the polarization on the 100 au scale is consistent with the signature of dust scattering for disk-candidates and that the polarization on the envelope-scale in all sources may come from another mechanism, most likely magnetically aligned grains.
Solar Magnetoseismology with Magnetoacoustic Surface Waves in Asymmetric Magnetic Slab Waveguides
Authors: Allcock Matthew , Erdélyi Robert 
Published: March 2018

Abstract
Solar magnetoseismology is an indirect method to approximate plasma parameters that are traditionally difficult to measure in the solar atmosphere using observations of magnetohydrodynamic waves. A magnetic slab can act as waveguide for magnetoacoustic waves that approximates magnetic structures in the solar atmosphere. The asymmetry of the slab caused by different plasma parameters in each external region affects both the eigenfrequencies and eigenfunctions differently at each side of the slab, that is, both the temporal and spatial profiles of the eigenmodes of propagation along the slab are influenced by the equilibrium asymmetry. We present two novel diagnostic tools for solar magnetoseismology that use this distortion to estimate the slab magnetic field strength using the spatial distribution of magnetoacoustic surface waves: the amplitude ratio and the minimum perturbation shift techniques. They have the potential to estimate background equilibrium parameters in inhomogeneous solar structures such as elongated magnetic bright points, prominences, and the clusters of magnetic brightenings rooted in sunspot light bridges known as light bridge surges or light walls, which may be locally approximated as slabs.
The Origin of r-process Elements in the Milky Way
Authors: Côté Benoit , Fryer Chris L. , Belczynski Krzysztof , Korobkin Oleg , Chruślińska Martyna , Vassh Nicole , Mumpower Matthew R. , Lippuner Jonas , Sprouse Trevor M. , Surman Rebecca , Wollaeger Ryan 
Published: March 2018

Abstract
Some of the heavy elements, such as gold and europium (Eu), are almost exclusively formed by the rapid neutron capture process (r-process). However, it is still unclear which astrophysical site between core-collapse supernovae and neutron star–neutron star (NS–NS) mergers produced most of the r-process elements in the universe. Galactic chemical evolution (GCE) models can test these scenarios by quantifying the frequency and yields required to reproduce the amount of europium (Eu) observed in galaxies. Although NS–NS mergers have become popular candidates, their required frequency (or rate) needs to be consistent with that obtained from gravitational wave measurements. Here, we address the first NS–NS merger detected by LIGO/Virgo (GW170817) and its associated gamma-ray burst and analyze their implication for the origin of r-process elements. The range of NS–NS merger rate densities of 320–4740 Gpc−3 yr−1 provided by LIGO/Virgo is remarkably consistent with the range required by GCE to explain the Eu abundances in the Milky Way with NS–NS mergers, assuming the solar r-process abundance pattern for the ejecta. Under the same assumption, this event has produced about 1–5 Earth masses of Eu, and 3–13 Earth masses of gold. When using theoretical calculations to derive Eu yields, constraining the role of NS–NS mergers becomes more challenging because of nuclear astrophysics uncertainties. This is the first study that directly combines nuclear physics uncertainties with GCE calculations. If GW170817 is a representative event, NS–NS mergers can produce Eu in sufficient amounts and are likely to be the main r-process site.
Diffusion and Mixing in Globular Clusters
Authors: Meiron Yohai , Kocsis Bence 
Published: March 2018

Abstract
Collisional relaxation describes the stochastic process with which a self-gravitating system near equilibrium evolves in phase-space due to the fluctuating gravitational field of the system. The characteristic timescale of this process is called the relaxation time. In this paper, we highlight the difference between two measures of the relaxation time in globular clusters: (1) the diffusion time with which the isolating integrals of motion (i.e., energy E and angular momentum magnitude L) of individual stars change stochastically and (2) the asymptotic timescale required for a family of orbits to mix in the cluster. More specifically, the former corresponds to the instantaneous rate of change of a star’s E or L, while the latter corresponds to the timescale for the stars to statistically forget their initial conditions. We show that the diffusion timescales of E and L vary systematically around the commonly used half-mass relaxation time in different regions of the cluster by a factor of ∼10 and ∼100, respectively, for more than 20% of the stars. We define the mixedness of an orbital family at any given time as the correlation coefficient between its E or L probability distribution functions and those of the whole cluster. Using Monte Carlo simulations, we find that mixedness converges asymptotically exponentially with a decay timescale that is ∼10 times the half-mass relaxation time.