bluuebunny/crossref_metadata_2025_split huggingface dataset:
Indisciplina escolar na visão de alunos e professores: investigando concepções
Authors: Trevisan Andreia Cristina Rodrigues , Letícia Zoz Driéle , Paulo Trevisan Eberson 
Published: September 2021

A pesquisa apresentada tem como objetivo principal identificar concepções de alunos e professores sobre a indisciplina escolar e compreender sua implicação para o processo de ensino e aprendizagem. A pesquisa se configurou como uma investigação de abordagem qualitativa, na qual buscamos, através de questionários aplicados a 144 alunos e 12 professores, pertencentes à uma escola da rede pública estadual de Mato Grosso, produzir dados referentes a problemática indisciplina nesse ambiente escolar. Os resultados obtidos através dos questionários dos alunos e professores evidenciaram que a indisciplina vem sendo entendida como um comportamento inadequado para o ambiente escolar, que atrapalha o processo de ensino e aprendizagem. Em relação as atitudes relacionadas à indisciplina, xingar o professor foi a mais listada pelos alunos, seguida por atos que atrapalham o processo de ensino e aprendizagem, como por exemplo, não participar da aula, conversas paralelas e não fazer a lição. Para os professores participantes da pesquisa um dos casos mais comuns de indisciplina em sala de aula é alunos inquietos, que não cooperam com o professor e que se mostram desinteressados. Em relação as atitudes tomadas diante dos alunos indisciplinados o que mais se destacou foi o diálogo entre professor e aluno. O fato que se deve levar em consideração é que o diálogo tem se configurado como o principal instrumento do professor no processo de ensino e aprendizagem, sendo que devemos sempre lembrar que em sala de aula nos deparamos com alunos que possuem suas particularidades e que o respeito a isso é o primeiro passo para amenizar o problema da indisciplina no espaço escolar, evitando com isso prejuízos ao processo de aprendizagem.
Palavras-chaves: Indisciplina escolar, processo de ensino e aprendizagem, concepções de professores e alunos.
HIGHWAY IMPACT STUDY OF THE EFFICIENCY OF COATING AND BASE COMPACTION WITH THREE-ROLLER TANDEM COMPACTORS
Authors: Нилов Владимир Александрович , Жулай Владимир Алексееич , Тюнин Виталий Леонидович , Щиенко Алексей Николаевич 
Published: September 2021

Приведено технико-экономическое обоснование повышения эффективности уплотнения покрытий и оснований за счет использования трехвальцевых дорожных катков тандемного типа. Выполнены расчеты, показывающие возможность последовательного увеличения вертикального нагружения вальцев катка по мере возрастания прочности уплотняемой поверхности в широких пределах (до 1,1 веса серийного катка) за счет применения дополнительной управляемой секции. Установлена возможность уменьшения числа проходов катка за счет увеличения количества его вальцев. Проведен технико-экономический расчет, подтверждающий целесообразность применения таких дорожных катков, выполненных на базе серийных двухвальцевых машин, которая обусловлена увеличением производительности в 1,27…1,5 раза.
We present a highway impact study for increasing efficiency of compaction of coatings and bases through the use of three-roller tandem compactors. Calculations have been performed showing the possibility of a sequential increase in the vertical loading of the rollers of a compactor as the strength of the compacted surface increases over a wide range (up to 1.1 of the weight of a serial compactor) due to the use of an additional controlled section. The possibility of reducing the number of passes of the compactor by increasing the number of its rollers has been established. A technical and economic calculation was carried out confirming the feasibility of using such road compactors made on the basis of serial two- roller tandem compactors, which is due to an increase in productivity by 1,27…1,5 times.
MouseView.js: Reliable and valid attention tracking in web-based experiments using a cursor-directed aperture
Authors: Anwyl-Irvine Alexander L. , Armstrong Thomas , Dalmaijer Edwin S. 
Published: September 2021

AbstractPsychological research is increasingly moving online, where web-based studies allow for data collection at scale. Behavioural researchers are well supported by existing tools for participant recruitment, and for building and running experiments with decent timing. However, not all techniques are portable to the Internet: While eye tracking works in tightly controlled lab conditions, webcam-based eye tracking suffers from high attrition and poorer quality due to basic limitations like webcam availability, poor image quality, and reflections on glasses and the cornea. Here we present MouseView.js, an alternative to eye tracking that can be employed in web-based research. Inspired by the visual system, MouseView.js blurs the display to mimic peripheral vision, but allows participants to move a sharp aperture that is roughly the size of the fovea. Like eye gaze, the aperture can be directed to fixate on stimuli of interest. We validated MouseView.js in an online replication (N = 165) of an established free viewing task (N = 83 existing eye-tracking datasets), and in an in-lab direct comparison with eye tracking in the same participants (﻿N = 50). Mouseview.js proved as reliable as gaze, and produced the same pattern of dwell time results. In addition, dwell time differences from MouseView.js and from eye tracking correlated highly, and related to self-report measures in similar ways. The tool is open-source, implemented in JavaScript, and usable as a standalone library, or within Gorilla, jsPsych, and PsychoJS. In sum, MouseView.js is a freely available instrument for attention-tracking that is both reliable and valid, and that can replace eye tracking in certain web-based psychological experiments.
Nano-scale friction and wear of polymer coated with graphene
Authors: Vacher Robin S , de Wijn Astrid S 
Published: September 2021

Background: Friction and wear of polymers at the nano scale is a challenging problem due to the complex viscoelastic properties and structure. Using molecular-dynamics simulations, we investigate how a graphene sheet on top of a semicrystalline polymer (PVA) affects the friction and wear.Results: Our setup is meant to resemble an AFM experiment with a silicon tip. We have used two different graphene sheets: an unstrained, flat sheet, and one that has been crumpled before being deposited on the polymer.Conclusion: The graphene protects the top layer of the polymer from wear and reduces the friction. The unstrained flat graphene is stiffer, and we find that it constrains the polymer chains and reduces the indentation depth.
Antidiabetic green leafy vegetables currently sold in Trincomalee District in Sri Lanka
Authors: SHANMUGALİNGAM Vinujan , VİVEKANANDARAJAH SATHASİVAMPİLLAİ Saravanan , SEBASTİAN Pholtan Rajeev 
Published: September 2021

Diabetes is a disease in which the body does not produce insulin or cannot use insulin effectively. In Sri Lanka, 1.2 million people among the age group of 20 to 79 were affected by diabetes in 2019. Biomedicine antidiabetic medications cause common side effects such as bladder cancer, dehydration, sinusitis, kidney illness, and urinary infections. Consumption of green leafy vegetables minimizes the risk of developing diabetes. Hence, this work aims to identify and document the green leafy vegetables currently sold in Trincomalee District in Sri Lanka by performing fieldwork visits to the main markets and the surrounding green leafy vegetable kiosks, shops, superstores, and streets from January 2019 to June 2021. The levels of antidiabetic scientific evidence available for the identified green leafy vegetable species were assessed by recognizing the relevant published works in the electronic databases Web of Science, PubMed, Scopus, etc., until September 2021. A total of 99 green leafy vegetable species from 43 families were recognized. The majority of the green leafy vegetables had in vivo (33%), followed by in vitro (16%) and clinical (9%) as scientific evidences. Also, 49 antidiabetic compounds were already isolated from the identified green leafy vegetables. This study forms a foundation for further studies using the green leafy vegetable species in Trincomalee.
FIM DO IMPÉRIO. MUDANÇAS SOCIAIS E CONTEXTOS HISTÓRICOS E POLÍTICOS. POSICIONAMENTO DO BRASIL EM RELAÇÃO A SI PRÓPRIO E AS RELAÇÕES COM O EXTERIOR
Authors: De Abreu Rodrigues Fabiano 
Published: September 2021

O objetivo deste trabalho é compreender de que forma o panorama político alterou toda uma sociedade, de que forma o fim do império mudou os contextos históricos, sociais e econômicos de todo o país. É ainda de ressaltar a mudança na forma como o Brasil se posicionou em relação a si próprio e ao exterior com o fim do império. Documentação e outros textos de investigação sobre o tema foram usados para a elaboração deste trabalho. Para a realização do trabalho foram analisados vários documentos desdediscursos parlamentares, cartas pessoais, artigos e editoriais jornalísticos, além das principais obras que compõem a bibliografia sobre o assunto. As três últimas décadas do Império Brasileiro serão as mais focadas, desde a guerra Paraguai vs Brasil (13/12/1864) e finalização no golpe militar que derrubou o último gabinete do Império, e na seqüência o próprio regime monárquico 15/11/1889). Para uma melhor compreensão do processo que culminou com a mudança de regime no Brasil, procedemos a investigação dos principais eventos que lhe precederam, e também a busca de apreensão do sentido da ação de seus principais agentes históricos, permitindo-nos assim vislumbrar as conjunções entre História e personalidade.
TESS Data for Asteroseismology: Photometry
Authors: Handberg Rasmus , Lund Mikkel N. , White Timothy R. , Hall Oliver J. , Buzasi Derek L. , Pope Benjamin J. S. , Hansen Jonas S. , von Essen Carolina , Carboneau Lindsey , Huber Daniel , Vanderspek Roland K. , Fausnaugh Michael M. , Tenenbaum Peter , Jenkins Jon M. ,   The T’DA Collaboration
Published: September 2021

Abstract
Over the last two decades, asteroseismology has increasingly proven to be the observational tool of choice for the study of stellar physics, aided by the high quality of data available from space-based missions such as CoRoT, Kepler, K2, and the Transiting Exoplanet Survey Satellite (TESS). TESS in particular will produce more than an order of magnitude more such data than has ever been available before. While the standard TESS mission products include light curves from 120 s observations suitable for both exoplanet and asteroseismic studies, they do not include light curves for the vastly larger number of targets observed by the mission at a longer 1800 s cadence in Full Frame Images (FFIs). To address this lack, the TESS Data for Asteroseismology (T’DA) group under the TESS Asteroseismic Science Consortium (TASC) has constructed an open-source pipeline focused on producing light curves for all stars observed by TESS at all cadences, currently including stars down to a TESS magnitude of 15. The pipeline includes target identification, background estimation and removal, correction of FFI time stamps, and a range of potential photometric extraction methodologies, though aperture photometry is currently the default approach. For the brightest targets, we transparently apply a halo photometry algorithm to construct a calibrated light curve from unsaturated pixels in the image. In this paper, we describe in detail the algorithms, functionality, and products of this pipeline and summarize the noise metrics for the light curves. Companion papers will address the removal of systematic noise sources from our light curves, and a stellar variability classification from these.
L 98-59: A Benchmark System of Small Planets for Future Atmospheric Characterization
Authors: Pidhorodetska Daria , Moran Sarah E. , Schwieterman Edward W. , Barclay Thomas , Fauchez Thomas J. , Lewis Nikole K. , Quintana Elisa V. , Villanueva Geronimo L. , Domagal-Goldman Shawn D. , Schlieder Joshua E. , Gilbert Emily A. , Kane Stephen R. , Kostov Veselin B. 
Published: September 2021

Abstract
The M3V dwarf star L 98-59 hosts three small (R < 1.6 R
⊕) planets. The host star is bright (K = 7.1) and nearby (10.6 pc), making the system a prime target for follow-up characterization with the Hubble Space Telescope (HST) and the upcoming James Webb Space Telescope (JWST). Herein, we use simulated transmission spectroscopy to evaluate the detectability of spectral features with HST and JWST assuming diverse atmospheric scenarios (e.g., atmospheres dominated by H2, H2O, CO2, or O2). We find that H2O and CH4 present in a low mean molecular weight atmosphere could be detected with HST in one transit for the two outermost planets, while H2O in a clear steam atmosphere could be detected in six transits or fewer with HST for all three planets. We predict that observations using JWST/NIRISS would be capable of detecting a clear steam atmosphere in one transit for each planet and H2O absorption in a hazy steam atmosphere in two transits or less. In a clear, desiccated atmosphere, O2 absorption may be detectable for all three planets with NIRISS. If the L 98-59 planets possess a clear, Venus-like atmosphere, NIRSpec could detect CO2 within 26 transits for each planet, but the presence of H2SO4 clouds would significantly suppress CO2 absorption. The L 98-59 system is an excellent laboratory for comparative planetary studies of transiting multiplanet systems, and observations of the system via HST and JWST would present a unique opportunity to test the accuracy of the models presented in this study.
Synthetic Absorption Lines from Simulations of Multiphase Gas in Galactic Winds
Authors: de la Cruz Lita M. , Schneider Evan E. , Ostriker Eve C. 
Published: September 2021

Abstract
Supernova-driven galactic winds are multiphase streams of gas that are often observed flowing at a range of velocities out of star-forming regions in galaxies. In this study, we use high-resolution 3D simulations of multiphase galactic winds modeled with the hydrodynamics code Cholla to investigate the connection between numerical studies and observations. Using a simulated interaction between a hot T ∼ 107 K supernova-driven wind and a cool T ∼ 104 K cloud of interstellar material, we create mock observables, including the optical depth (τ) and covering fraction (C

f
), of six commonly observed ions (Si ii, C ii, Si iv, C iv, N v, and O vi) as a function of gas velocity. We compare our mock observables to surveys of galactic winds in the literature, finding good agreement with velocities and profiles of the low ions. We then compute “empirical” values for the optical depth and covering fraction following observational techniques, and compare them to the values calculated directly from the simulation data. We find that the empirically computed values tend to underestimate the “true” value of τ for ions with high optical depth and overestimate the “true” value of τ for ions with low optical depth relative to the simulated data. The empirically estimated covering fractions match our direct calculations very well for the low-ionization ions; for the high-ionization ions, the empirical covering fractions underestimate the directly computed values by up to ∼40%.
Magnetic Energy Release, Plasma Dynamics, and Particle Acceleration in Relativistic Turbulent Magnetic Reconnection
Authors: Guo Fan , Li Xiaocan , Daughton William , Li Hui , Kilian Patrick , Liu Yi-Hsin , Zhang Qile , Zhang Haocheng 
Published: September 2021

Abstract
In strongly magnetized astrophysical plasma systems, magnetic reconnection is believed to be the primary process during which explosive energy release and particle acceleration occur, leading to significant high-energy emission. Past years have witnessed active development of kinetic modeling of relativistic magnetic reconnection, supporting this magnetically dominated scenario. A much less explored issue in studies of relativistic reconnection is the consequence of three-dimensional dynamics, where turbulent structures are naturally generated as various types of instabilities develop. This paper presents a series of three-dimensional, fully kinetic simulations of relativistic turbulent magnetic reconnection (RTMR) in positron–electron plasmas with system domains much larger than kinetic scales. Our simulations start from a force-free current sheet with several different modes of long-wavelength magnetic field perturbations, which drive additional turbulence in the reconnection region. Because of this, the current layer breaks up and the reconnection region quickly evolves into a turbulent layer filled with coherent structures such as flux ropes and current sheets. We find that plasma dynamics in RTMR is vastly different from its 2D counterpart in many aspects. The flux ropes evolve rapidly after their generation, and can be completely disrupted by the secondary kink instability. This turbulent evolution leads to superdiffusive behavior of magnetic field lines as seen in MHD studies of turbulent reconnection. Meanwhile, nonthermal particle acceleration and the timescale for energy release can be very fast and do not depend strongly on the turbulence amplitude. The main acceleration mechanism is a Fermi-like acceleration process supported by the motional electric field, whereas the nonideal electric field acceleration plays a subdominant role. We also discuss possible observational implications of three-dimensional RTMR in high-energy astrophysics.
The Study of X-Ray Flux Variability of M87
Authors: Imazawa Ryo , Fukazawa Yasushi , Takahashi Hiromitsu 
Published: September 2021

Abstract
We searched for a short-term X-ray variability of the M87 core and jet from archival X-ray data with long exposure data taken by the Suzaku, Chandra, and NuSTAR telescopes. We found the intraday variability for the Suzaku data obtained in 2006, and for the Chandra core obtained in 2017. The intraday variability suggested a minute emission region about the size of the Schwarzschild radius of the M87 supermassive black hole. Suzaku could not resolve a core and HST-1; however, in 2006, HST-1 was much brighter than the core, and thus, the variability is likely due to the HST-1. Since the photon index in 2006 was 2.38, the emission was possibly synchrotron emission from the local shock region in the HST-1, indicating that the particle acceleration of TeV electrons occurred far away (∼100 pc) from the core. Assuming the fading time to be equal to the synchrotron cooling time, the magnetic field is constrained to be B ∼ 1.94 δ
1/3 mG. Moreover, the photon index of the core in 2017 was approximately 1.96; thus, the possible emission was from the radiative inefficiency accretion flow of the core or inverse Compton scattering in the jet. Intraday time variability prefers the latter possibility.
The Nature of Jets in Double-peaked Emission-line AGN in the KISSR Sample
Authors: Kharb P. , Subramanian S. , Das M. , Vaddi S. , Paragi Z. 
Published: September 2021

Abstract
Double-peaked emission-line AGN (DPAGN) have been regarded as binary black hole candidates. We present here results from parsec-scale radio observations with the Very Long Baseline Array (VLBA) of five DPAGN belonging to the KISSR sample of emission-line galaxies. This work concludes our pilot study of nine type 2 Seyfert and LINER DPAGN from the KISSR sample. In the nine sources, dual compact cores are only detected in the “offset AGN,” KISSR 102. However, the overall incidence of jets in the eight sources that were detected with the VLBA is ≥60%. We find a difference in the “missing flux density” going from the Very Large Array to VLBA scales between Seyferts and LINERs, with LINERs showing less missing flux density on parsec-scales. Using the emission-line modeling code, MAPPINGS III, we find that the emission lines are likely to be influenced by jets in 5/9 sources. Jet-medium interaction is the likely cause of the emission-line splitting observed in the SDSS spectra of these sources. Jets in radio-quiet AGN are therefore energetically capable of influencing their parsec- and kpc-scale environments, which makes them agents of “radio AGN feedback” (similar to radio-loud AGN).
Thresholds for Particle Clumping by the Streaming Instability
Authors: Li 李 Rixin 日新 , Youdin Andrew N. 
Published: September 2021

Abstract
The streaming instability (SI) is a mechanism to aerodynamically concentrate solids in protoplanetary disks and trigger the formation of planetesimals. The SI produces strong particle clumping if the ratio of solid to gas surface density—an effective metallicity—exceeds a critical value. This critical value depends on particle sizes and disk conditions such as radial drift-inducing pressure gradients and levels of turbulence. To quantify these thresholds, we perform a suite of vertically stratified SI simulations over a range of dust sizes and metallicities. We find a critical metallicity as low as 0.4% for the optimum particle sizes and standard radial pressure gradients (normalized value of Π = 0.05). This subsolar metallicity is lower than previous results, due to improved numerical methods and computational effort. We discover a sharp increase in the critical metallicity for small solids, when the dimensionless stopping time (Stokes number) is ≤0.01. We provide simple fits to the size-dependent SI clumping threshold, including generalizations to different disk models and levels of turbulence. We also find that linear, unstratified SI growth rates are a surprisingly poor predictor of particle clumping in nonlinear, stratified simulations, especially when the finite resolution of simulations is considered. Our results widen the parameter space for the SI to trigger planetesimal formation.
Clustered Star Formation in the Center of NGC 253 Contributes to Driving the Ionized Nuclear Wind
Authors: Mills E. A. C. , Gorski M. , Emig K. L. , Bolatto A. D. , Levy R. C. , Leroy A. K. , Ginsburg A. , Henshaw J. D. , Zschaechner L. K. , Veilleux S. , Tanaka K. , Meier D. S. , Walter F. , Krieger N. , Ott J. 
Published: September 2021

Abstract
We present new 3 mm observations of the ionized gas toward the nuclear starburst in the nearby (D ∼ 3.5 Mpc) galaxy NGC 253. With ALMA, we detect emission from the H40α and He40α lines in the central 200 pc of this galaxy on spatial scales of ∼4 pc. The recombination line emission primarily originates from a population of approximately a dozen embedded super star clusters in the early stages of formation. We find that emission from these clusters is characterized by electron temperatures ranging from 7000 to 10,000 K and measures an average singly ionized helium abundance 〈Y
+〉 = 0.25 ± 0.06, both of which are consistent with values measured for H ii regions in the center of the Milky Way. We also report the discovery of unusually broad line width recombination line emission originating from seven of the embedded clusters. We suggest that these clusters contribute to the launching of the large-scale hot wind observed to emanate from the central starburst. Finally, we use the measured recombination line fluxes to improve the characterization of overall embedded cluster properties, including the distribution of cluster masses and the fractional contribution of the clustered star formation to the total starburst, which we estimate is at least 50%.