bluuebunny/crossref_metadata_2025_split huggingface dataset:
IMPROVING SPEAKING SKILL OF THE ELEVENTH-GRADE STUDENTS OF SMAN 8 DENPASAR IN ACADEMIC YEAR 2017/2018 THROUGH BRITISH PARLIAMENTARY STYLE DEBATE TECHNIQUE
Authors: Kristoforus Fransiskus Janggur  , Ni Wayan Krismayani  , Ni Luh Putu Dian Sawitri  
Published: October 2021

Abstract

This classroom action research was done in the area of speaking. It was found that the eleventh grade students of SMAN 8 Denpasar got difficulty in communicating and delivering ideas. The objective of this study was to figure out whether or not speaking skill of the eleventh-grade students of SMAN 8 Denpasar in academic year 2017/2018 could be improved through British Parliamentary Style Debate Technique. The research was undertaken based on the result of the interview with the teacher who taught the students. Pre-test was then carried out, and it was found that the subjects’ speaking skill was low. In order to settle down the problem, British Parliamentary Style Debate Technique was implemented as the technique to improve the subjects’ speaking skill. The study was conducted in two cycles. Furthermore, the result of post- test in each cycle showed that there were significant improvements on the subjects’ speaking skill after British Parliamentary Style Debate technique was applied. After the treatment of pre-test, the reflection or post-test was administered. The mean figure of the reflection or post-test scores obtained by the subjects under study in cycle I was 70.52. and in cycle II was 78.34. In addition, based on the data of the questionnaire, the subjects’ responses towards the application of the technique was positive. Therefore, it could be concluded that speaking skill of the eleventh- grade students of SMAN 8 Denpasar in academic year 2017/2018 could be improved through British Parliamentary Style Debate Technique.
Keywords: Improving, Speaking, British Parliamentary Style Debate Technique
COMMUNITY CORRECTIONS IN THE LIST OF THE MAIN CORRECTIONAL MEANS FOR CONVICTS: SOME ASPECTS
Authors: Малолеткина Наталья Сергеевна 
Published: October 2021

В статье рассматривается ряд теоретических проблем общественного воздействия как средства исправления осужденных (его содержание, субъекты осуществления, соотношение с другими средствами исправления и пр.) и недостатков правовой основы данного института. Приводятся практические примеры осуществления общественного воздействия в отношении осужденных к лишению свободы. Делается вывод, что общественное воздействие при ненадлежащем законодательном регулировании представляет собой важнейшее средство исправления осужденных (наряду с режимом), которое с учетом разносторонности субъектов его осуществления имеет многообразное содержание и фактически отчасти дублирует другие средства исправления.
The article examines a number of theoretical problems of community corrections as a means of correcting convicts (its content, subjects of implementation, correlation with other means of correction, etc.) and the shortcomings of the legal basis of this institution. Practical examples of the community corrections implementation in relation to persons sentenced to imprisonment are given. It is concluded that community corrections with improper legislative regulation is the most important means of correcting convicts (along with the regime), which, taking into account the versatility of the subjects of its implementation, has a diverse content and in fact partially duplicates other means of correction.
Peningkatan Produktivitas Bagian Pengepakan Menggunakan Basic Quality Tools di PT. XYZ
Authors: Kustiana Haerul , Sugiatna Angling , Yulianti Dini 
Published: October 2021

Abstract: This research is the application of quality control tools within the scope of increasing productivity of the packaging department at PT. XYZ. This study aims to determine the factors causing the decline in productivity in the packing warehouse area. The first step of the research is to analyze the input data using a Pareto diagram. The source of problems that occur from outside the packing area are four cases, namely Canceled Delivery, Part Received Without Documents, No Stock and Quality Issue. Meanwhile, for problems that occur from internal packaging, there are two, namely the No Packaging Box and No Operator Entering. By using the Ishikawa diagram and 5 whys, the sources of problems that occur in the internal packing area are analyzed further and obtained several sources of problems that contribute greatly to the decline in productivity in the packaging area, namely the process of purchasing packaging boxes which takes quite a long time and long working hours from the packaging team. Some of the solutions for internal problems offered include changing the carton box procurement process using blanket orders, upgrading the team leader's capabilities with order and budget monitoring capabilities, proposing changes in the production flow for semi-finished goods and a proposal to create a temporary warehouse for semi-finished goods.
Abstrak: Penelitian ini merupakan penerapan dari alat pengendalian qualitas dalam lingkup peningkatan produktivitas bagian pengepakan di PT. XYZ. Penelitian ini bertujuan untuk mengetahui faktor penyebab penurunan produktivitas diarea gudang pengepakan. Langkah awal penelitian dengan menganalisa data masukan menggunakan diagram Pareto. Sumber masalah yang terjadi dari luar area pengepakan ada empat kasus yaitu Pengiriman Dibatalkan, Part Diterima Tanpa Dokumen, Stock Tidak Ada dan Ada Issue Kualitas. Sementara untuk masalah yang terjadi dari internal pengepakan ada dua yaitu Box Pengemas Tidak ada dan Operator Tidak Masuk. Dengan menggunakan diagram Ishikawa dan 5 whys , sumber masalah yang terjadi di internal area pengepakan dianalisa lebih lanjut dan diperoleh beberapa sumber masalah yang berkontribusi besar terhadap penuruan produktivitas di area pengepakan yaitu proses pembelian box pengemas yang memakan waktu cukup lama dan jam kerja yang panjang dari tim pengepakan. Beberapa solusi untuk permasalah internal yang ditawarkan antara lain merubah proses pengadaan karton box dengan menggunakan blanket order, mengupgrade kemampuan team leader dengan kemampuan order dan budget monitoring, mengusulkan perubahan alur produksi untuk barang-barang setengah jadi serta usulan untuk membuat gudang sementara untuk barang setengah jadi.
Solar Anti-Hale Bipolar Magnetic Regions: A Distinct Population with Systematic Properties
Authors: Muñoz-Jaramillo Andrés , Navarrete Benjamín , Campusano Luis E. 
Published: October 2021

Abstract
Besides their causal connection with long and short-term magnetic variability, solar bipolar magnetic regions are our chief source of insight into the location, size, and properties of large-scale toroidal magnetic structures in the solar interior. The great majority of these regions (≈95%) follow a systematic east–west polarity orientation (Hale’s law) that reverses in opposite hemispheres and across even and odd cycles. These regions also present a systematic north–south polarity orientation (Joy’s law) that helps build the poloidal field that seeds the new cycle. Exceptions to Hale’s law are rare and difficult to study due to their low numbers. Here, we present a statistical analysis of the inclination (tilt) with respect to the equator of Hale versus anti-Hale regions spanning four solar cycles, considering two complementary tilt definitions adopted in previous studies. Our results show that anti-Hale regions belong to a separate population than Hale regions, suggesting a different originating mechanism. However, we find that anti-Hale region tilts present similar systematic tilt properties and similar latitudinal distributions to Hale regions, implying a strong connection between the two. We see this as evidence that they belong to a common toroidal flux system. We speculate that anti-Hale regions originate from poloidal field sheared and strengthened on the spot after the emergence of Hale regions with very strong poloidal contribution. Thus, they are not in contradiction with the idea of largely coherent toroidal flux systems inside the solar interior.
The Prominence Driven Forced Reconnection in the Solar Corona and Associated Plasma Dynamics
Authors: Srivastava A. K. , Mishra Sudheer K. , Jelínek P. 
Published: October 2021

Abstract
Using the multitemperature observations from SDO/AIA on 2019 December 30, we provide a signature of prominence driven forced magnetic reconnection in the corona and associated plasma dynamics from 09:20 UT to 10:38 UT. A hot prominence segment erupts with a speed of ≈21 km s−1 and destabilizes the entire prominence system. Thereafter, it rises upward in the north from 09:28 UT to 09:48 UT with a speed of 24 km s−1 . The eruptive prominence stretches overlying field lines upward with the speed of 27–28 km s−1, which further undergo the forced reconnection. The coronal plasma also flows southward with a speed of 7 km s−1, and both of these inflows trigger the reconnection at ≈09:48 UT. Thereafter, the eastward and westward magnetic channels are developed and separated. The east–west reorganization of the magnetic fields starts creating bidirectional plasma outflows toward the limb with their respective speeds of 28 and 37 km s−1. Their upper ends are diffused in the overlying corona, transporting another set of upflows with the speeds of ≈22 km and 19 km s−1. The multitemperature plasma (log T

e
= 6.0–7.2 K) evolves and elongates to a length of ≈105 km on the reorganized fields. The hot plasma and remaining prominence threads move from the reconnection region toward another segment of a prominence in the eastward direction. The prominence–prominence/loop interaction and associated reconnection generate jet-like eruptions with a speed of 178–183 km s−1. After the formation of the jet, the overlying magnetic channel disappears in the corona.
Kinematics of Crab Giant Pulses
Authors: Bij Akanksha , Lin Hsiu-Hsien , Li Dongzi , van Kerkwijk Marten H. , Pen Ue-Li , Lu Wenbin , Main Robert , Peterson Jeffrey B. , Quine Brendan , Vanderlinde Keith 
Published: October 2021

Abstract
The Crab Pulsar’s radio emission is unusual, consisting predominantly of giant pulses, with durations of about a microsecond but structure down to the nanosecond level, and brightness temperatures of up to 1037 K. It is unclear how giant pulses are produced, but they likely originate near the pulsar’s light cylinder, where corotating plasma approaches the speed of light. We report observations in the 400–800 MHz frequency band, where the pulses are broadened by scattering in the surrounding Crab Nebula. We find that some pulse frequency spectra show strong bands, which vary during the scattering tail, in one case showing a smooth upward drift. While the banding may simply reflect interference between nanosecond scale pulse components, the variation is surprising, as in the scattering tail the only difference is that the source is observed via slightly longer paths, bent by about an arcsecond in the nebula. The corresponding small change in viewing angle could nevertheless reproduce the observed drift by a change in Doppler shift, if the plasma that emitted the giant pulses moved highly relativistically, with a Lorentz factor γ ∼ 104 (and without much spread in γ). If so, this would support models that appeal to highly relativistic plasma to transform ambient magnetic structures to coherent gigahertz radio emission, be it for giant pulses or for potentially related sources, such as fast radio bursts.
Simulating Relic Gravitational Waves from Inflationary Magnetogenesis
Authors: Brandenburg Axel , Sharma Ramkishor 
Published: October 2021

Abstract
We present three-dimensional direct numerical simulations of the production of magnetic fields and gravitational waves (GWs) in the early universe during a low energy scale matter-dominated post-inflationary reheating era, and during the early subsequent radiative era, which is strongly turbulent. The parameters of the model are determined such that it avoids a number of known physical problems and produces magnetic energy densities between 0.03% and 0.5% of the critical energy density at the end of reheating. During the subsequent development of a turbulent magnetohydrodynamic cascade, magnetic fields and GWs develop a spectrum that extends to higher frequencies in the millihertz (nanohertz) range for models with reheating temperatures of around 100 GeV (150 MeV) at the beginning of the radiation-dominated era. However, even though the turbulent cascade is fully developed, the GW spectrum shows a sharp drop for frequencies above the peak value. This suggests that the turbulence is less efficient in driving GWs than previously thought. The peaks of the resulting GW spectra may well be in the range accessible to space interferometers, pulsar timing arrays, and other facilities.
Influence of Large-scale Field Structures on the Scaling Anisotropy in 3D MHD Turbulence
Authors: Yang Liping , Tu Chuanyi , He Jiansen , Wu Honghong , Wang Xin , Feng Xueshang 
Published: October 2021

Abstract
Magnetohydrodynamic (MHD) turbulence is revealed to have scaling anisotropy based on structure function calculations. Recent studies on solar wind turbulence found that the scaling anisotropy disappears when removing large-scale field structures. This finding raises questions as to whether numerical MHD turbulences have large-scale field structures. How do these structures affect the scaling anisotropy therein? Here we investigate these questions with a driven compressible three-dimensional MHD turbulence. We introduce a new method to check how the random stationarity condition is satisfied. We find for the first time in the numerical MHD turbulence that the large-scale field structures destroy the random stationarity of the local fields and make samplings nonparallel to the instantaneous fields be calculated as apparent parallel samplings. This mixture makes statistical calculations show anisotropic scaling of the turbulence. When we select only the random stationary data intervals, the statistical results show an isotropic nature. We also find that among the large-scale field structures, one-third are tangential discontinuities (TDs), one-third are rotational discontinuities (RDs), and the rest are EDs (either TD or RD). These results show that the large-scale structures in the numerical MHD turbulence have important influence on the structure function analysis.
The Large Early Galaxy Astrophysics Census (LEGA-C) Data Release 3: 3000 High-quality Spectra of K

s
-selected Galaxies at z > 0.6
Authors: van der Wel Arjen , Bezanson Rachel , D’Eugenio Francesco , Straatman Caroline , Franx Marijn , van Houdt Josha , Maseda Michael V. , Gallazzi Anna , Wu Po-Feng , Pacifici Camilla , Barisic Ivana , Brammer Gabriel B. , Munoz-Mateos Juan Carlos , Vervalcke Sarah , Zibetti Stefano , Sobral David , de Graaff Anna , Calhau Joao , Kaushal Yasha , Muzzin Adam , Bell Eric F. , van Dokkum Pieter G. 
Published: October 2021

Abstract
We present the third and final data release of the Large Early Galaxy Astrophysics Census (LEGA-C), an ESO/Very Large Telescope public spectroscopic survey targeting 0.6 < z < 1.0, Ks
-selected galaxies. The data release contains 3528 spectra with measured stellar velocity dispersions and stellar population properties, a 25-fold increase in sample size compared to previous work. This K

s
-selected sample probes the galaxy population down to ∼0.3L*, for all colors and morphological types. Along with the spectra, we publish a value-added catalog with stellar and ionized gas velocity dispersions, stellar absorption line indices, emission-line fluxes, and equivalent widths, complemented with structural parameters measured from Hubble Space Telescope Advanced Camera for Surveys imaging. With its combination of high precision and large sample size, LEGA-C provides a new benchmark for galaxy evolution studies.
Exploring the Solar Wind from Its Source on the Corona into the Inner Heliosphere during the First Solar Orbiter–Parker Solar Probe Quadrature
Authors: Telloni Daniele , Andretta Vincenzo , Antonucci Ester , Bemporad Alessandro , Capuano Giuseppe E. , Fineschi Silvano , Giordano Silvio , Habbal Shadia , Perrone Denise , Pinto Rui F. , Sorriso-Valvo Luca , Spadaro Daniele , Susino Roberto , Woodham Lloyd D. , Zank Gary P. , Romoli Marco , Bale Stuart D. , Kasper Justin C. , Auchère Frédéric , Bruno Roberto , Capobianco Gerardo , Case Anthony W. , Casini Chiara , Casti Marta , Chioetto Paolo , Corso Alain J. , Da Deppo Vania , De Leo Yara , Dudok de Wit Thierry , Frassati Federica , Frassetto Fabio , Goetz Keith , Guglielmino Salvo L. , Harvey Peter R. , Heinzel Petr , Jerse Giovanna , Korreck Kelly E. , Landini Federico , Larson Davin , Liberatore Alessandro , Livi Roberto , MacDowall Robert J. , Magli Enrico , Malaspina David M. , Massone Giuseppe , Messerotti Mauro , Moses John D. , Naletto Giampiero , Nicolini Gianalfredo , Nisticò Giuseppe , Panasenco Olga , Pancrazzi Maurizio , Pelizzo Maria G. , Pulupa Marc , Reale Fabio , Romano Paolo , Sasso Clementina , Schühle Udo , Stangalini Marco , Stevens Michael L. , Strachan Leonard , Straus Thomas , Teriaca Luca , Uslenghi Michela , Velli Marco , Verscharen Daniel , Volpicelli Cosimo A. , Whittlesey Phyllis , Zangrilli Luca , Zimbardo Gaetano , Zuppella Paola 
Published: October 2021

Abstract
This Letter addresses the first Solar Orbiter (SO)–Parker Solar Probe (PSP) quadrature, occurring on 2021 January 18 to investigate the evolution of solar wind from the extended corona to the inner heliosphere. Assuming ballistic propagation, the same plasma volume observed remotely in the corona at altitudes between 3.5 and 6.3 solar radii above the solar limb with the Metis coronagraph on SO can be tracked to PSP, orbiting at 0.1 au, thus allowing the local properties of the solar wind to be linked to the coronal source region from where it originated. Thanks to the close approach of PSP to the Sun and the simultaneous Metis observation of the solar corona, the flow-aligned magnetic field and the bulk kinetic energy flux density can be empirically inferred along the coronal current sheet with an unprecedented accuracy, allowing in particular estimation of the Alfvén radius at 8.7 solar radii during the time of this event. This is thus the very first study of the same solar wind plasma as it expands from the sub-Alfvénic solar corona to just above the Alfvén surface.
Observational Effects of Banded Repeating FRBs
Authors: Aggarwal Kshitij 
Published: October 2021

Abstract
Recent observations have shown that repeating fast radio bursts (FRBs) exhibit band-limited emission, whose frequency-dependent amplitude can be modeled using a Gaussian function. In this analysis, we show that banded emission of FRBs can lead to incompleteness across the observing band. This biases the detected sample of bursts and can explain the various shapes of cumulative energy distributions seen for repeating FRBs. We assume a Gaussian shape of the burst spectra and use simulations to demonstrate the above bias using an FRB 121102-like example. We recovered energy distributions that showed a break in power law and flattening of power law at low energies, based on the fluence threshold of the observations. We provide recommendations for single-pulse searches and analysis of repeating FRBs to account for this incompleteness. Primarily, we recommend that burst spectra should be modeled to estimate the intrinsic fluence and bandwidth of the burst robustly. Also, bursts that lie mainly within the observing band should be used for analyses of energy distributions. We show that the bimodality reported in the distribution of energies of FRB 121102 by Li et al. disappears when burst bandwidth, instead of the center frequency of the observation, is used to estimate energy. Subbanded searches will also aid in detecting band-limited bursts. All the analysis scripts used in this work are available in a Github repository (https://github.com/KshitijAggarwal/banded_repeater_analysis).
Star Formation Histories of Ultra-faint Dwarf Galaxies: Environmental Differences between Magellanic and Non-Magellanic Satellites?*
Authors: Sacchi Elena , Richstein Hannah , Kallivayalil Nitya , van der Marel Roeland , Libralato Mattia , Zivick Paul , Besla Gurtina , Brown Thomas M. , Choi Yumi , Deason Alis , Fritz Tobias , Geha Marla , Guhathakurta Puragra , Jeon Myoungwon , Kirby Evan , Majewski Steven R. , Patel Ekta , Simon Joshua D. , Tony Sohn Sangmo , Tollerud Erik , Wetzel Andrew 
Published: October 2021

Abstract
We present the color–magnitude diagrams and star formation histories (SFHs) of seven ultra-faint dwarf galaxies: Horologium 1, Hydra 2, Phoenix 2, Reticulum 2, Sagittarius 2, Triangulum 2, and Tucana 2, derived from high-precision Hubble Space Telescope photometry. We find that the SFH of each galaxy is consistent with them having created at least 80% of the stellar mass by z ∼ 6. For all galaxies, we find quenching times older than 11.5 Gyr ago, compatible with the scenario in which reionization suppresses the star formation of small dark matter halos. However, our analysis also reveals some differences in the SFHs of candidate Magellanic Cloud satellites, i.e., galaxies that are likely satellites of the Large Magellanic Cloud and that entered the Milky Way potential only recently. Indeed, Magellanic satellites show quenching times about 600 Myr more recent with respect to those of other Milky Way satellites, on average, even though the respective timings are still compatible within the errors. This finding is consistent with theoretical models that suggest that satellites’ SFHs may depend on their host environment at early times, although we caution that within the error bars all galaxies in our sample are consistent with being quenched at a single epoch.
Integrative taxonomic review of the genus Peschetius (Coleoptera, Dytiscidae, Hydroporinae) from India with description of two new species
Authors: Sheth Sayali D. , Ghate Hemant V. , Dahanukar Neelesh , Hájek Jiří 
Published: October 2021

AbstractThe diving beetle genusPeschetiusGuignot, 1942 (Coleoptera: Dytiscidae) in India is reviewed. Integrative taxonomic approach using morphology, multivariate morphometry and genetic analysis of cytochrome oxidase subunit 1 revealed the presence of four species, two of which are described here as new:Peschetius bistroemisp. nov.from southern Western Ghats (Kerala) differs from all known congeners with distinctly broadened male antennomeres IV and V, shape of the prosternal process and the male genitalia;P. nilssonisp. nov.from northern Western Ghats, Rajasthan and Madhya Pradesh is similar to the widespread IndianP. toxophorusGuignot, 1942, from which it differs in habitus, elytral colour pattern and the shape of the male genitalia. New records are presented for the remaining Indian species, namelyP. quadricostatus(Aubé, 1838) andP. toxophorus. All species are diagnosed, illustrated and a key to their identification is provided.
Le paternalisme comme système de contrôle dans la durée : une approche historique du « Système Michelin »
Authors: Cohanier Bruno , Baker Charles Richard 
Published: October 2021

Le Groupe Michelin a été fondé en 1889 à Clermont-Ferrand par deux frères André et Édouard Michelin. Depuis sa création, cette société a déployé un système de contrôle paternaliste offrant différents « privilèges » à ses employés. En retour, les fondateurs et directeurs généraux successifs espéraient de la « loyauté » et un travail « diligent ». Fondé sur une méthode historique l’article propose d’éclairer le système de contrôle sous un angle culturel, puis dans sa relation avec le paternalisme. Il expose les étapes de l'évolution du système de contrôle chez Michelin en proposant une discussion à cet égard.