bluuebunny/crossref_metadata_2025_split huggingface dataset:
МОДЕЛЮВАННЯ АЕРОДИНАМІЧНО РАЦІОНАЛЬНОГО РОЗПИЛЮВАЛЬНОГО ПРИСТРОЮ
Authors: Пастушенко А.С. 
Published: June 2021

Проблема хімічного захисту рослин набуває все більшого значення, оскільки аграрне виробництво держави втрачає від шкідників, хвороб та бур’янів, за окремими культурами, майже третину валового збору урожаю. Існуючий парк засобів хімічного захисту сільськогосподарських культур, цілеспрямований на підвищення ефективності цієї роботи, потребує розвитку і вдосконалення. Тематика статті обумовлена необхідністю розроблення нових аналітичних підходів щодо проєктування робочих органів обприскувачів рослин, які відповідають сучасним технологічним вимогам, шляхом покращення аеродинамічних показників проточної частини розпилювача. Конструкція розпилювача є досконалою в аеродинамічному відношенні, якщо відсутній відрив прикордонного шару від стінки або якщо область відриву розташована як можна нижче за течією. Для цього визначається місце відриву прикордонного шару від стінки на основі дослідження двофазного середовища робочої рідини та обмінних процесів, характеристик, що істотно впливають на формування та розвиток прикордонного шару і його відрив, а, отже, на мінімізацію опору обтічних поверхонь. Наслідком цього підходу є зниження втрат енергії. На основі дослідження відомих аналітичних рішень, які можна адаптувати до моделювання руху двофазних середовищ у каналі розпилювача робочої рідини, в комплексі із графоаналітичним методом конструювання поверхонь каналу, запропоновано підхід, що дозволяє профілювати робочі органи обприскувачів зі зменшеними втратами енергії.
Pengembangan Modul Kecerdasan Spiritual Sebagai Media Layanan Bimbingan dan Konseling Pribadi pada Siswa
Authors: Asi Nurhan G. , Madina Rena , Usman Irvan 
Published: June 2021

Penelitian ini bertujuan untuk menghasilkan produk pengembangan modul kecerdasan spiritual sebagai media layanan bimbingan dan konseling pada siswa SMP. Model penelitian ini menggunakan model pengembangan Sugiyono metode Researh & Development (R&D). Modul kecerdasan spiritual berlatar belakang oleh rendahnya kecerdasan spiritual pada siswa yang diperoleh hasil pengamatan dan observasi langsung pada saat melakukan Praktek Pengalaman Lapangan. Proses pengembangan modul kecerdasan spiritual ini dikembangkan menggunakan metode Researh & Development model Sugiyono yang terdapat tahapan-tahapan yang harus dilewati sehingga mendapatkan suatu produk yang layak digunakan. Penelitian pengembangan ini menghasilkan sebuah produk media bimbingan dan konseling yaitu “Modul Kecerdasan Spiritual Sebagai Media Layanan Bimbingan dan Konseling Pada Siswa SMP Negeri 1 Gorontalo”.Modul ini telah layak digunakan oleh guru Bimbingan dan Konseling untuk meningkatkan kecerdasan spiritual siswa, dengan kejelasan materi sudah sesuai dan mudah di pahami karena sudah melalui tahap uji validasi masing-masing oleh ahli/pakar desain media, ahli bahasa dan ahli bimbingan dan konseling.
Pengaruh Bakat Numerikal Terhadap Prestasi Belajar Siswa Sekolah Menegah Atas
Authors: Taulena Susana 
Published: June 2021

Sekolah Menengah Atas Negeri 4 Ambon memiliki Jumlah siswa kelas X sebanyak 365 orang dan kelas X-8 berjumlah 29 orang. Ada sebagian Siswa kelas X-8 yang memiliki Prestasi Belajar yang rendah atau tidak mencapai KKM yaitu 75. Prestasi Belajar yang rendah dipengaruhui oleh beberapa faktor salah satunya adalah bakat akademik yaitu bakat numerikal atau kemampuan memahami konsep yang berkaitan dengan angka-angka. Penelitian ini bertujuan untuk mengetahui Pengaruh Bakat Numerikal Terhadap Prestasi belajar Siswa Kelas X (Sepuluh). Populasi pada penelitian ini adalah kelas X yang berjumlah 365 orang dan dipilih sebagai sampel secara teknik sampling purposive. Sampling purposive adalah teknik pengambilan sampel atas pertimbangan tertentu, yang berjumlah 29 orang. Pengumpulan data dilakukan dengan tes tertulis kemampuan numerikal yaitu Tes Differential Aptitude Test (DAT), dan pendataan nilai prestasi belajar dari rapot semester ganjil-genap. Pengujian data dilakukan dengan menggunakan analisis regresi linear sederhana dan selanjutnya menggunakan program komputer SPSS – 20. Hasil penelitian dengan persamaan regresi : Ý = ß + (b1 .X1) Prestasi belajar matematika = 8,084 + (2.549 x X1) antara kemampuan numerikal mempunyai pengaruh yang signifikan terhadap prestasi belajar karena mempunyai nilai Thitung (17.4422) > Ttabel (1.699) dengan taraf signifikansi 0.05. ini berarti Hipotesa H0 ditolak dan Ha diterima artinya variabel bakat numerikal memiliki pengaruh yang signifikan terhadap prestasi belajar.
BVRcIc Observations, Third-body Orbital Study, and Analysis of the UV Leo-type, Pre-W UMA Binary V642 Virginis
Authors: Samec Ronald G. , Chamberlain Heather , Caton D. , Wolf Marek , Zasche Petr , Kučáková Hana , Hornoch Kamil , Morgan Shannon , Faulkner Danny R. 
Published: June 2021

Abstract
V642 Vir is a polar spotted, well-detached, UV Leo-type, low-mass, pre-WUMa (T1 ∼ 4250K, ∼K6V) eclipsing binary. It was observed in 2020 April, May, and June at the Dark Sky Observatory in North Carolina, USA with the 0.81 m reflector of Appalachian State University. A total of 88 timings were used in our 22-year period study which included 12 Transiting Exoplanet Survey Satellite (TESS) timings. The O − C plots show a low-amplitude oscillation of residuals that points to the existence of an orbiting third body, a dwarf of minimum mass, 0.15 M
⊙ in an eccentric orbit (e = 0.41), with an orbital period of 20.07 yr. The odd light curves of V642 Virginis indicate that it has polar spots similar to UV Leo and the recently published V1023 Per. Its present large polar spot region indicates that it must have a strong magnetic field and that it is synchronously rotating. The BVRcIc simultaneous Wilson–Devinney Program solution gives a detached binary (primary and secondary components are underfilling their respective Roche Lobes, with 76% and 78% fill outs respectively). The cool spot region models near the pole of the primary component (centered at 10° colatitude) and is angled toward the secondary component. Its large radius (68°) and T-fact (Tspot/Tsurface = 0.69) also attest to the conclusion of the strength of the magnetic field. The small ΔT in the components (∼318 K) and mass ratio near unity (0.9542 ± 0.0005) show that the stars are similar in spectral type (secondary ∼K9V). The inclination is high, ∼86.87 ± 0.04°, yet there is no time of constant light due to the two stars’ essentially equal radii.
Spectrum and Morphology of the Very-high-energy Source HAWC J2019+368
Authors: Albert A. , Alfaro R. , Alvarez C. , Arteaga-Velázquez J. C. , Arunbabu K. P. , Avila Rojas D. , Ayala Solares H. A. , Baghmanyan V. , Belmont-Moreno E. , Brisbois C. , Caballero-Mora K. S. , Capistrán T. , Carramiñana A. , Casanova S. , Cotzomi J. , Coutiño de León S. , De la Fuente E. , Diaz Hernandez R. , Dingus B. L. , DuVernois M. A. , Durocher M. , Engel K. , Espinoza C. , Fraija N. , Garcia D. , García-González J. A. , Giacinti G. , González M. M. , Goodman J. A. , Harding J. P. , Hinton J. , Hona B. , Huang D. , Hueyotl-Zahuantitla F. , Huentemeyer P. , Jardin-Blicq A. , Joshi V. , Lee W. H. , León Vargas H. , Linnemann J. T. , Longinotti A. L. , Luis-Raya G. , Lundeen J. , López-Coto R. , Malone K. , Martinez O. , Martínez-Castro J. , Matthews J. A. , Miranda-Romagnoli P. , Morales-Soto J. A. , Moreno E. , Mostafá M. , Nayerhoda A. , Nellen L. , Newbold M. , Nisa M. U. , Noriega-Papaqui R. , Olivera-Nieto L. , Omodei N. , Peisker A. , Pérez Araujo Y. , Pérez-Pérez E. G. , Rho C. D. , Rosa-González D. , Ruiz-Velasco E. , Salazar H. , Salesa Greus F. , Sandoval A. , Schneider M. , Schoorlemmer H. , Serna-Franco J. , Smith A. J. , Springer R. W. , Surajbali P. , Tollefson K. , Torres I. , Turner R. , Ureña-Mena F. , Weisgarber T. , Willox E. , Zhou H. , de León C. ,   HAWC Collaboration
Published: June 2021

Abstract
The MGRO J2019+37 region is one of the brightest sources in the sky at TeV energies. It was detected in the second HAWC catalog as 2HWC J2019+367 and here we present a detailed study of this region using data from HAWC. This analysis resolves the region into two sources: HAWC J2019+368 and HAWC J2016+371. We associate HAWC J2016+371 with the evolved supernova remnant CTB 87, although its low significance in this analysis prevents a detailed study at this time. An investigation of the morphology (including possible energy-dependent morphology) and spectrum for HAWC J2019+368 is the focus of this work. We associate HAWC J2019+368 with PSR J2021+3651 and its X-ray pulsar wind nebula, the Dragonfly nebula. Modeling the spectrum measured by HAWC and Suzaku reveals a ∼7 kyr pulsar and nebula system producing the observed emission at X-ray and γ-ray energies.
Beyond Simple AGN Unification with Chandra-observed 3CRR Sources at 0.5 < z < 1
Authors: Kuraszkiewicz Joanna , Wilkes Belinda J. , Atanas Adam , Buchner Johannes , McDowell Jonathan C. , Willner S. P. , Ashby Matthew L. N. , Azadi Mojegan , Barthel Peter , Haas Martin , Worrall Diana M. , Birkinshaw Mark , Antonucci Robert , Chini Rolf , Fazio Giovanni G. , Lawrence Charles , Ogle Patrick 
Published: June 2021

Abstract
Low-frequency radio selection finds radio-bright galaxies regardless of the amount of obscuration by gas and dust. We report Chandra observations of a complete 178 MHz–selected, and so orientation-unbiased, sample of 44 0.5 < z < 1 3CRR sources. The sample is comprised of quasars and narrow-line radio galaxies (NLRGs) with similar radio luminosities, and the radio structure serves as both an age and an orientation indicator. Consistent with unification, intrinsic obscuration (measured by N
H, X-ray hardness ratio, and X-ray luminosity) generally increases with inclination. However, the sample includes a population not seen in high-z 3CRR sources: NLRGs viewed at intermediate inclination angles with N
H < 1022 cm−2. Multiwavelength analysis suggests that these objects have lower L/L
Edd than typical NLRGs at similar orientation. Thus, both orientation and L/L
Edd are important, and a “radiation-regulated unification” provides a better explanation of the sample’s observed properties. In comparison with the 3CRR sample at 1 < z < 2, our lower-redshift sample shows a higher fraction of Compton-thin NLRGs (45% versus 29%) but a similar Compton-thick fraction (20%), implying a larger covering factor of Compton-thin material at intermediate viewing angles and thus a more “puffed-up” torus atmosphere. We posit that this is due to a range of L/L
Edd extending to lower values in this sample. In contrast, at high redshifts, the narrower range and high L/L
Edd values allowed orientation (and so simple unification) to dominate the sample’s observed properties.
A Tale of Two Grains: Impact of Grain Size on Ring Formation via Nonideal Magnetohydrodynamic Processes
Authors: Hu 胡 Xiao 晓 , Wang 王 Lile 力乐 , Okuzumi 奥 Satoshi 住 聡 , Zhu 朱 Zhaohuan 照 寰 
Published: June 2021

Abstract
Substructures in protoplanetary disks (PPDs), whose ubiquity was unveiled by recent Atacama Large Millimeter/submillimeter Array observations, are widely discussed regarding their possible origins. We carry out global 2D magnetohydrodynamic (MHD) simulations in axisymmetry, coupled with self-consistent ray-tracing radiative transfer, thermochemistry, and nonideal MHD diffusivities. The abundance profiles of grains are also calculated based on the global dust evolution calculation, including sintering effects. We found that dust size plays a crucial role in the ring formation around the snow lines of PPDs through the accretion process. Disk ionization structures and thus tensorial conductivities depend on the size of grains. When grains are significantly larger than polycyclic aromatic hydrocarbons (PAHs), the nonideal MHD conductivities change dramatically across each snow line of major volatiles, leading to a sudden change in the accretion process across the snow lines and the subsequent formation of gaseous rings/gaps there. Specific layout of magnetic fields can suppress wind launching in certain regions by canceling out different stress components. On the other hand, the variations of conductivities are a lot less with only PAH-sized grains in disks and then these disks retain smoother radial density profiles across snow lines.
Rotational Disruption of Porous Dust Aggregates due to Gas Flow in Protoplanetary Disks
Authors: Tatsuuma Misako , Kataoka Akimasa 
Published: June 2021

Abstract
We introduce a possible disruption mechanism of dust grains in planet formation by their spinning motion. This mechanism has been discussed as rotational disruption for the interstellar dust grains. We theoretically calculate whether porous dust aggregates can be disrupted by their spinning motion and whether it prohibits dust growth in protoplanetary disks. We assume radiative torque and gas-flow torque as driving sources of the spinning motion, assume that dust aggregates reach a steady-state rigid rotation, and compare the obtained tensile stress due to the centrifugal force with their tensile strength. We model the irregularly shaped dust aggregates by introducing a parameter, γ
ft, that mimics the conversion efficiency from force to torque. As a result, we find that porous dust aggregates are rotationally disrupted by their spinning motion induced by gas flow when their mass is larger than ∼108 g and their volume filling factor is smaller than ∼0.01 in our fiducial model, while relatively compact dust aggregates with volume filling factor more than 0.01 do not face this problem. If we assume the dust porosity evolution, we find that dust aggregates whose Stokes number is ∼0.1 can be rotationally disrupted in their growth and compression process. Our results suggest that the growth of dust aggregates may be halted due to rotational disruption or that other compression mechanisms are needed to avoid it. We also note that dust aggregates are not rotationally disrupted when γ
ft ≤ 0.02 in our fiducial model and the modeling of irregularly shaped dust aggregates is essential in future work.
The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). III. A Young Molecular Outflow Driven by a Decelerating Jet
Authors: Tafoya 多 Daniel 穂 谷 , Sanhueza Patricio , Zhang Qizhou , Li Shanghuo , Guzmán Andrés E. , Silva Andrea , de la Fuente Eduardo , Lu Xing , Morii Kaho , Tatematsu Ken’ichi , Contreras Yanett , Izumi Natsuko , Jackson James M. , Nakamura Fumitaka , Sakai Takeshi 
Published: June 2021

Abstract
We present a spatio-kinematical analysis of the CO (J = 2 → 1) line emission, observed with the Atacama Large Millimeter/submillimeter Array (ALMA), of the outflow associated with the most massive core, ALMA1, in the 70 μm dark clump G010.991–00.082. The position–velocity (PV) diagram of the molecular outflow exhibits a peculiar S-shaped morphology that has not been seen in any other star-forming region. We propose a spatio-kinematical model for the bipolar molecular outflow that consists of a decelerating high-velocity component surrounded by a slower component whose velocity increases with distance from the central source. The physical interpretation of the model is in terms of a jet that decelerates as it entrains material from the ambient medium, which has been predicted by calculations and numerical simulations of molecular outflows in the past. One side of the outflow is shorter and shows a stronger deceleration, suggesting that the medium through which the jet moves is significantly inhomogeneous. The age of the outflow is estimated to be τ ≈ 1300 yr, after correction for a mean inclination of the system of ≈57°.
Stellar Winds Drive Strong Variations in Exoplanet Evaporative Outflow Patterns and Transit Absorption Signatures
Authors: Harbach Laura M. , Moschou Sofia P. , Garraffo Cecilia , Drake Jeremy J. , Alvarado-Gómez Julián D. , Cohen Ofer , Fraschetti Federico 
Published: June 2021

Abstract
Stellar wind and photon radiation interactions with a planet can cause atmospheric depletion, which may have a potentially catastrophic impact on a planet’s habitability. While photon interactions with planetary atmospheres and outflows have been researched to some degree, studies of stellar wind interactions are in their infancy. Here, we use three-dimensional magnetohydrodynamic simulations to model the effect of the stellar wind on the magnetosphere and outflow of a hypothetical planet, modeled to have an H-rich evaporating envelope with a prescribed mass-loss rate, orbiting in the habitable zone close to a low-mass M dwarf. We take the TRAPPIST-1 system as a prototype, with our simulated planet situated at the orbit of TRAPPIST-1e. We show that the atmospheric outflow is accelerated and advected upon interaction with the wind, resulting in a diverse range of planetary magnetosphere morphologies and plasma distributions as local stellar wind conditions change along the orbit. We consider the implications of the wind–outflow interaction on potential hydrogen Lyα observations of the planetary atmosphere during transits. The Lyα observational signatures depend strongly on the local wind conditions at the time of the observation and can be subject to considerable variation on timescales as short as an hour. Our results indicate that observed variations in exoplanet transit signatures could be explained by wind–outflow interaction.
Impact of the Disk Thickness on X-Ray Reflection Spectroscopy Measurements
Authors: Tripathi Ashutosh , Abdikamalov Askar B. , Ayzenberg Dimitry , Bambi Cosimo , Liu Honghui 
Published: June 2021

Abstract
In a previous paper, we presented an extension of our reflection model relxill_nk to include the finite thickness of the accretion disk following the prescription in Taylor & Reynolds. In this paper, we apply our model to fit the 2013 simultaneous observations by the Nuclear Spectroscopic Telescope Array (NuSTAR) and XMM-Newton of the supermassive black hole in MCG-06-30-15 and the 2019 NuSTAR observation of the Galactic black hole in EXO 1846-031. The high-quality data of these spectra had previously led to precise black hole spin measurements and very stringent constraints on possible deviations from the Kerr metric. We find that the disk thickness does not change previous spin results found with a model employing an infinitesimally thin disk, which confirms the robustness of spin measurements in high radiative efficiency disks, where the impact of disk thickness is minimal. Similar analysis on lower accretion rate systems will be an important test for measuring the effect of disk thickness on black hole spin measurements.
Flux Ropes, Turbulence, and Collisionless Perpendicular Shock Waves: High Plasma Beta Case
Authors: Zank G. P. , Nakanotani M. , Zhao L. L. , Du S. , Adhikari L. , Che H. , le Roux J. A. 
Published: June 2021

Abstract
With the onset of solar maximum and the expected increased prevalence of interplanetary shock waves, Parker Solar Probe is likely to observe numerous shocks in the next few years. An outstanding question that has received surprisingly little attention has been how turbulence interacts with collisionless shock waves. Turbulence in the supersonic solar wind is described frequently as a superposition of a majority 2D and a minority slab component. We formulate a collisional perpendicular shock-turbulence transmission problem in a way that enables investigation of the interaction and transmission of quasi-perpendicular fluctuations such as magnetic flux ropes/islands and vortices as well as entropy and acoustic modes in the large plasma beta regime. We focus on the transmission of an upstream spectrum of these modes, finding that the downstream spectral amplitude is typically increased significantly (a factor of 10 or more), and that the upstream spectral index of the inertial range, and indeed the general spectral shape, is unchanged for the downstream magnetic variance, kinetic energy, and density variance. A comparison of the theoretically predicted downstream magnetic variance, kinetic energy, and density variance spectra with those observed at 1, 5, and 84 au by Wind, Ulysses, and Voyager 2 shows excellent agreement. The overall theoretically predicted characteristics of the transmission of turbulence across shocks observed in the solar wind appear to be largely consistent with recent observational studies by Pitňa et al. and Borovsky.
How Flat Can a Planetary System Get? I. The Case of TRAPPIST-1
Authors: Heising Matthew Z. , Sasselov Dimitar D. , Hernquist Lars , Luisa Tió Humphrey Ana 
Published: June 2021

Abstract
The seven planets orbiting TRAPPIST-1 in a compact near-resonant chain offer a unique case to study in planet formation theory. We demonstrate in this paper that the remarkable flatness of the system, exceeding that of any other known planetary system, is an important constraint on the mass of the gaseous disk in which it formed and attained its current configuration. We use three-dimensional hydrodynamic simulations of the gas and planets to study specific formation models. In particular, we report simulations motivated by the model proposed by Ormel et al.—in this model, the dispersal of the gas disk pushes the planets from an initial resonant chain into their present configuration. We find that a disk with the mass used in this model is consistent with the flatness of the TRAPPIST-1 system, but a more massive disk is not, with the transition occurring between 15 and 50 times the mass of the Ormel et al. disk. This upper limit on mass rules out certain models of the formation of the system, namely in situ formation and disk migration on long timescales.
Bismuth Classification of Bile Duct Injury and Its Association with Increasing 30 Days Mortality after Revision Surgery
Authors: Ida Bagus Budhi , Ida Bagus Metria , Ida Ayu Setyawati 
Published: June 2021

Background: The incidence rate of bile duct injury has not been changed for many years for both open or laparoscopic technique. Open cholecystectomy has risen from 0.5% to 1.4% when gallbladder removal is performed laparoscopically. Injuries of the bile duct system after laparoscopic cholecystectomy are more complex than that after an open approach, causing significant morbidity and even death. From initial classification published by Bismuth, there have been many classifications of common bile duct injury. We would reported the 30 days mortality rate following reconstruction after bile duct injury according to type of Bismuth classification.
Case Report: 7 cases of common bile duct injury were reported from 2016 until 2018 following cholecystectomy (both open and laparoscopic), all cases were diagnosed as early complication and without intra operative cholangiography performed. The most common bile duct injury was Bismuth type II and IV (2 patients in each type). Reconstruction has been done by hepatico jejunostomy for type III and IV. Choledoco Duodenostomy bypass was done for type I and II. 2 patients with bismuth type IV have long standing cholangitis and cannot survive during 30 days of follow up. 4 others patients could survive with no intra abdominal complication nor other morbidity.
Conclusion: Bismuth classification was the simpliest type to described the bile duct injury, Bismuth type IV was associated with the high risk of 30 days mortality rate.

Keywords: bismuth classification, bile duct injury, cholecystectomy, mortality