bluuebunny/crossref_metadata_2025_split huggingface dataset:
IMPLEMENTASI BOTTOM AIR DECK DAN EXPAND PATTERN SECARA TERINTEGRASI DALAM RANGKA OPTIMALISASI PENGGUNAAN BAHAN PELEDAK DI PIT SOUTH PINANG PT. KALTIM PRIMA COAL
Authors: Sadiq Masda Rohal 
Published: July 2021

Untuk menghadapi harga jual batubara yang terus melemah dan mempertahankan kinerja perusahaan, manajemen PT. Kaltim Prima Coal terus melakukan strategi manajemen biaya dengan menekan berbagai komponen pengeluaran, diantaranya adalah dengan melakukan upaya efisiensi penggunaan bahan peledak yang di gunakan. Seiring dengan perkembangan waktu dan teknologi, terdapat beberapa metode yang di gunakan untuk mengefisiensi penggunaan bahan peledak tanpa mengorbankan kualitas hasil peledakan. Adapun metode yang telah di lakukan untuk mencapai hal tersebut adalah dengan cara sebagai berikut :1.Implementasi Bottom Air Deck pada Lubang LedakBottom Air Deck merupakan istilah rongga udara yang terdapat di bagian bawah kolom bahan peledak yang berfungsi untuk membuat perangkap energi dan mengurangi energi terbuang secara vertikal. Rongga udara yang ada akan menyebabkan energi hasil peledakan lebih merata ke sekitar lubang ledak dan menciptakan fragmentasi peledakan yang lebih seragam. Implementasi Bottom Air Deck di terapkan pada kedalaman lubang mulai dari 7.5 m – 11 m (berdasarkan analisa Air Deck Factor &#38; Rock Mass Rating), dimana penggunaan bahan peledak dapat di efisiensi sebesar 15% - 17% per lubang (setara dengan penghematan 20 kg – 25 kg bahan peledak) 2.Trial Expand Pattern menggunakan Analisa Kuz-Ram dan Scale Depth Of Burrial (S.D.O.B)Analisa Kuz-ram dan Scale Depth Of Burial digunakan sebagai pendekatan matematis untuk memprediksi dan mengontrol fragmentasi batuan hasil peledakan, Flying Rock dan Air Blast. Dengan melakukan percobaan Expand Pattern dari 8x8 m dan 8x8.5 m menjadi 8x9 m (dimana distribusi fragmentasi aktual P-30 ≥ 80% dan rasio S.D.O.B = 0.92 – 1.40) masing-masing dapat mengoptimalkan Powder Factor sebesar 5 % – 11 % dari budget yang sudah di tetapkanSetelah melakukan 2 metode di atas selama bulan Januari - September 2020, penggunaan bahan peledak telah berhasil di efisiensi sebesar 8.6 % dari budget yang telah di tetapkan (aktual Powder Factor = 0.201 kg/ bcm terhadap Budget = 0.220 kg/ bcm). Penghematan bahan peledak tersebut setara dengan penghematan biaya operasional sebesar $84,888 (Rp.1.2 Milyar) selama bulan January – September 2020. Di sisi lain, aktual produktifitas alat gali-muat Libherr S420 dan Hitachi S321 selama bulan Januari – September 2020 yang beroperasi di Pit South Pinang, masing- masing masih produktif di angka 5.3% dan 4.7% dari budget yang telah di tetapkan (Aktual Prodt’y S420 = 2,106 bcm/ hr terhadap budget = 2,000 bcm/ hr dan Aktual Prodt’y S321 = 1,314 bcm/ hr terhadap budget = 1,255 bcm/ hr)
Budaya Komunikasi Virtual Pada Masa Pandemi Covid-19 (Studi Kasus Pembelajaran Daring di UIN Walisongo Semarang)
Authors: Putri Fitri Ariana 
Published: July 2021

<em>Budaya komunikasi virtual sebagai suatu kebiasaan baru yang dillakukan pada masa pandemic covid-19 secara virtual atau tidak langsung dengan melalui media sosial. Dalam dunia virtual CMC (Computer Mediatied Communication) seseorang dapat saling berinteraksi meskipun tidak dalam lokasi yang sama, namun ekspresi, emosi seseorang tidak terwakilkan seluruhnya karena proses komunikasi hanya melalui layar (face-to screen). Adanya pandemi Covid-19 dinilai mengubah pola komunikasi masyarakat. Dimana komunikasi yang biasanya dapat dilakukan secara tatap muka, kini harus dilakukan secara virtual karena adanya kebijakan social distancing dari pemerintah. cara berkomunikasi tidak hanya bisa dilakukan dengan face to face saja. Akan tetapi dapat dilakukan secara virtual untuk memudahkan dan memanfaatkan adanya media sosial yang ada. Dalam penelitian ini menggunakan penelitian kualitatif deskriptif dengan pendekatan library research. Tujuan dari penelitian ini untuk mengetahui budaya komunikasi virtual pada masa pandemi Covid-19. Dan hasil dari temuan ini media komunikasi virtual yang sering digunakan dalam agenda rapat ataupun pembelajaran pada masa pandemi Covid-19 seperti zoom, skype for business dan gotomeetings.</em>
Komunikasi Propaganda Islam Politik Di Indonesia
Authors: Islamy Imam El 
Published: July 2021

<em>Latar belakang penulis mengangkat judul ini dikarenakan ilmu komunikasi khususnya tentang propaganda disalahgunakan untuk mencapai keinginan suatu kelompok atau perorangan terutama propaganda Islam politik. Permasalahan yang akan dibahas di dalam Jurnal ini yaitu bagaimana propaganda menjadi senjata untuk mencapai tujuan suatu kelompok atau perorangan. Penelitian ini menggunakan pendekatan kualitatif dengan metode studi literatur dan dokumentasi. Menurut hasil penelitian penulis menunjukkan bahwa propaganda yang dilakukan sebagian kelompok di Indonesia telah menjadikan kelompok islam menjadi terpojok terkhusus permasalahan politik di Indonesia. Keadaan ini memaksa kondisi politik Indonesia menjadi tidak sehat dan tidak stabil sebab ada kecenderungan menekan kelompok islam politik yang ada di Indonesia. </em>
FOR TEACHING RUSSIAN LANGUAGE AD PERSONAM
Authors: Параккини Л. 
Published: July 2021

Настоящая статья посвящена важности инновационных форм обучения в современном образовательном процессе. В контексте требований студентоцентричности рассматриваются изменения условий учебного процесса, в частности изменения мотивации студентов. Применительно к преподаванию РКИ анализируется методический потенциал дидактической платформы для обучения иностранным языкам «Ревита», которая основана на принципах искусственного интеллекта. Выявляются точки соприкосновения функциональности и философии платформы «Ревита» с основными принципами теории образования взрослых (андрагогики).
This article analyzes the importance of innovative teaching forms in the contemporary educational process. It considers the changes in the conditions of such process, in particular the changes of students’ motivation, in a context requiring a student-oriented approach. With reference to the teaching of Russian as foreign language, the work analyzes the methodological potential of the teaching platform for foreign language “Revita”, which is based on the principles of artificial intelligence. The contact points between functionality and philosophy of the platform “Revita” and the basic principles of the theory of adult education (andragogy) are identified.
DEVELOPMENT OF NEW SCIENTIFIC AND PRACTICAL APPROACHES TO THE ORGANIZATION OF VOLUNTARY ACTIVITIES IN THE FIELD OF FIRE SAFETY
Authors: Ратникова Ольга Дмитриевна , Перегудова Наталья Васильевна , Кононко Павел Павлович , Илларионова Надежда Михайловна 
Published: July 2021

В статье проведен анализ нормативных правовых документов в области организации добровольческой деятельности. Анализ законодательства и организационно-методических документов, которые обеспечивают унифицированный подход к организации деятельности добровольческих организаций, позволяет МЧС России наиболее эффективно реализовывать полномочия по координации и планированию добровольческой деятельности в сфере ответственности Министерства.
The article analyzes the normative legal documents in the field of organizing voluntary activities. The analysis of legislation and organizational and methodological documents, which provide a unified approach to the organization of the activities of voluntary organizations, allows the Russian Emergencies Ministry to coordinate and plan voluntary activities most effectively.
Outer Solar System Perihelion Gap Formation through Interactions with a Hypothetical Distant Giant Planet
Authors: Oldroyd William J. , Trujillo Chadwick A. 
Published: July 2021

Abstract
Among the outer solar system minor planet orbits there is an observed gap in perihelion between roughly 50 and 65 au at eccentricities
e
≳ 0.65. Through a suite of observational simulations, we show that the gap arises from two separate populations, the Extreme Trans-Neptunian Objects (ETNOs; perihelia q ≳ 40 au and semimajor axes a ≳ 150 au) and the Inner Oort Cloud objects (IOCs; q ≳ 65 au and a ≳ 250 au), and is very unlikely to result from a realistic single, continuous distribution of objects. We also explore the connection between the perihelion gap and a hypothetical distant giant planet, often referred to as Planet 9 or Planet X, using dynamical simulations. Some simulations containing Planet X produce the ETNOs, the IOCs, and the perihelion gap from a simple Kuiper-Belt-like initial particle distribution over the age of the solar system. The gap forms as particles scattered to high eccentricity by Neptune are captured into secular resonances with Planet X where they cross the gap and oscillate in perihelion and eccentricity over hundreds of kiloyears. Many of these objects reach a minimum perihelia in their oscillation cycle within the IOC region increasing the mean residence time of the IOC region by a factor of approximately five over the gap region. Our findings imply that, in the presence of a massive external perturber, objects within the perihelion gap will be discovered, but that they will be only ∼20% as numerous as the nearby IOC population (65 au ≲ q ≲ 100 au).
New Observational Constraints on the Winds of M dwarf Stars*
Authors: Wood Brian E. , Müller Hans-Reinhard , Redfield Seth , Konow Fallon , Vannier Hunter , Linsky Jeffrey L. , Youngblood Allison , Vidotto Aline A. , Jardine Moira , Alvarado-Gómez Julián D. , Drake Jeremy J. 
Published: July 2021

Abstract
High-resolution UV spectra of stellar H i Lyα lines from the Hubble Space Telescope (HST) provide observational constraints on the winds of coronal main-sequence stars, thanks to an astrospheric absorption signature created by the interaction between the stellar winds and the interstellar medium. We report the results of a new HST survey of M dwarf stars, yielding six new detections of astrospheric absorption. We estimate mass-loss rates for these detections and upper limits for nondetections. These new constraints allow us to characterize the nature of M dwarf winds and their dependence on coronal activity for the first time. For a clear majority of the M dwarfs, we find winds that are weaker than or comparable in strength to that of the Sun, i.e.,

M

̇

≤
1

M

̇

⊙

. However, two of the M dwarfs have much stronger winds: YZ CMi (M4 Ve;

M

̇

=
30

M

̇

⊙

) and GJ 15AB (M2 V+M3.5 V;

M

̇

=
10

M

̇

⊙

). Even these winds are much weaker than expectations if the solar relation between flare energy and coronal mass ejection (CME) mass extended to M dwarfs. Thus, the solar flare/CME relation does not appear to apply to M dwarfs, with important ramifications for the habitability of exoplanets around M dwarfs. There is evidence for some increase in

M

̇

with coronal activity as quantified by X-ray flux, but with much scatter. One or more other factors must be involved in determining wind strength besides spectral type and coronal activity, with magnetic topology being one clear possibility.
Identifying Acoustic Wave Sources on the Sun. I. Two-dimensional Waves in a Simulated Photosphere
Authors: Bahauddin Shah Mohammad , Rast Mark Peter 
Published: July 2021

Abstract
The solar acoustic oscillations are likely stochastically excited by convective dynamics in the solar photosphere, though few direct observations of individual source events have been made and their detailed characteristics are still unknown. Wave source identification requires measurements that can reliably discriminate the local wave signal from the background convective motions and resonant modal power. This is quite challenging as these noise contributions have amplitudes several orders of magnitude greater than the sources and the propagating wave fields they induce. In this paper, we employ a high-temporal-frequency filter to identify sites of acoustic emission in a radiative magnetohydrodynamic simulation. The properties of the filter were determined from a convolutional neural network trained to identify the two-dimensional acoustic Green’s function response of the atmosphere, but once defined, it can be directly applied to an image time series to extract the signal of local wave excitation, bypassing the need for the original neural network. Using the filter developed, we have uncovered previously unknown properties of the acoustic emission process. In the simulation, acoustic events are found to be clustered at mesogranular scales, with peak emission quite deep, about 500 km below the photosphere, and sites of very strong emission can result from the interaction of two supersonic downflows that merge at that depth. We suggest that the method developed, when applied to high-resolution high-cadence observations, such as those forthcoming with the Daniel K. Inouye Solar Telescope, will have important applications in chromospheric wave studies and may lead to new investigations in high-resolution local helioseismology.
SDSS-IV MaNGA: Refining Strong Line Diagnostic Classifications Using Spatially Resolved Gas Dynamics
Authors: Law David R. , Ji Xihan , Belfiore Francesco , Bershady Matthew A. , Cappellari Michele , Westfall Kyle B. , Yan Renbin , Bizyaev Dmitry , Brownstein Joel R. , Drory Niv , Andrews Brett H. 
Published: July 2021

Abstract
We use the statistical power of the MaNGA integral-field spectroscopic galaxy survey to improve the definition of strong line diagnostic boundaries used to classify gas ionization properties in galaxies. We detect line emission from 3.6 million spaxels distributed across 7400 individual galaxies spanning a wide range of stellar masses, star formation rates, and morphological types, and find that the gas-phase velocity dispersion σ
Hα
correlates strongly with traditional optical emission-line ratios such as [S ii]/Hα, [N ii]/Hα, [O i]/Hα, and [O iii]/Hβ. Spaxels whose line ratios are most consistent with ionization by galactic H ii regions exhibit a narrow range of dynamically cold line-of-sight velocity distributions (LOSVDs) peaked around 25 km s−1 corresponding to a galactic thin disk, while those consistent with ionization by active galactic nuclei (AGNs) and low-ionization emission-line regions (LI(N)ERs) have significantly broader LOSVDs extending to 200 km s−1. Star-forming, AGN, and LI(N)ER regions are additionally well separated from each other in terms of their stellar velocity dispersion, stellar population age, Hα equivalent width, and typical radius within a given galaxy. We use our observations to revise the traditional emission-line diagnostic classifications so that they reliably identify distinct dynamical samples both in two-dimensional representations of the diagnostic line ratio space and in a multidimensional space that accounts for the complex folding of the star-forming model surface. By comparing the MaNGA observations to the SDSS single-fiber galaxy sample, we note that the latter is systematically biased against young, low-metallicity star-forming regions that lie outside of the 3″ fiber footprint.
The Carnegie Chicago Hubble Program X: Tip of the Red Giant Branch Distances to NGC 5643 and NGC 1404
Authors: Hoyt Taylor J. , Beaton Rachael L. , Freedman Wendy L. , Jang In Sung , Lee Myung Gyoon , Madore Barry F. , Monson Andrew J. , Neeley Jillian R. , Rich Jeffrey A. , Seibert Mark 
Published: July 2021

Abstract
The primary goal of the Carnegie Chicago Hubble Program (CCHP) is to calibrate the zero-point of the Type Ia supernova (SN Ia) Hubble Diagram through the use of Population II standard candles. So far, the CCHP has measured direct distances to 11 SNe Ia, and here we increase that number to 15 with two new Tip of the Red Giant Branch (TRGB) distances measured to NGC 5643 and NGC 1404. We present resolved, point-source photometry from new Hubble Space Telescope imaging of these two galaxies in the F814W and F606W bandpasses. From each galaxy’s stellar halo, we construct an F814W-band luminosity function in which we detect an unambiguous edge feature identified as the TRGB. For NGC 5643, we find μ
0 = 30.48 ± 0.03(stat) ± 0.07(sys) mag, and for NGC 1404 we find μ
0 = 31.36 ± 0.04(stat) ± 0.05(sys) mag. From a preliminary consideration of the SNe Ia in these galaxies, we find increased confidence in the results presented in Paper VIII. The high precision of our TRGB distances enables a significant measurement of the 3D displacement between the Fornax cluster galaxies NGC 1404 and NGC 1316 (Fornax A) equal to

1.50

−
0.39

+
0.25

Mpc, which we show is in agreement with independent constraints found in the literature.
The First Dynamical Mass Measurement in the HR 8799 System
Authors: Brandt G. Mirek , Brandt Timothy D. , Dupuy Trent J. , Michalik Daniel , Marleau Gabriel-Dominique 
Published: July 2021

Abstract
HR 8799 hosts four directly imaged giant planets, but none has a mass measured from first principles. We present the first dynamical mass measurement in this planetary system, finding that the innermost planet HR 8799 e has a mass of

9.6

−
1.8

+
1.9

M

Jup

. This mass results from combining the well-characterized orbits of all four planets with a new astrometric acceleration detection (5σ) from the Gaia EDR3 version of the Hipparcos-Gaia Catalog of Accelerations. We find with 95% confidence that HR 8799 e is below 13 M
Jup, the deuterium-fusing mass limit. We derive a hot-start cooling age of

42

−
16

+
24

Myr for HR 8799 e that agrees well with its hypothesized membership in the Columba association but is also consistent with an alternative suggested membership in the β Pictoris moving group. We exclude the presence of any additional ≳5 − M
Jup planets interior to HR 8799 e with semimajor axes between ≈3–16 au. We provide proper motion anomalies and a matrix equation to solve for the mass of any of the planets of HR 8799 using only mass ratios between the planets.
Time-lag Between Disk and Corona Radiation Leads to Hysteresis Effect Observed in Black hole X-Ray Binary MAXI J1348-630
Authors: Weng Shan-Shan , Cai Zhen-Yi , Zhang Shuang-Nan , Zhang Wei , Chen Yu-Peng , Huang Yue , Tao Lian 
Published: July 2021

Abstract
Accretion is an essential physical process in black hole X-ray binaries (BHXRBs) and active galactic nuclei. The properties of accretion flows and their radiation were originally considered to be uniquely determined by the mass accretion rate of the disk; however, the “hysteresis effect” observed during outbursts of nearly all BHXRBs seriously challenges this paradigm. The hysteresis effect referred to is that the hard-to-soft state transition in the fast-rise stage occurs at much higher luminosity than the soft-to-hard state transition in the slow-decay stage. That is, the same source can show different spectral/temporal properties at the same luminosity. Phenomenologically, this effect is also represented as the so-called “q”-shaped hardness-intensity diagram, which has been proposed as a unified scene for BHXRBs. However, there is still a lack of quantitative theoretical interpretation and observational understanding of the “q”-diagram. Here, we present a detailed time-lag analysis of a recently found BHXRB, MAXI J1348-630, intensively monitored by Insight-HXMT over a broad energy band (1–150 keV). We find the first observational evidence that the observed time-lag between radiations of the accretion disk and the corona leads naturally to the hysteresis effect and the “q”-diagram. Moreover, complemented by the quasi-simultaneous Swift data, we achieve a panorama of the accretion flow: the hard X-ray outburst from the corona heats and subsequently induces the optical brightening in the outer disk with nearly no lag; thereafter, the enhanced accretion in the outer disk propagates inward, generating the delayed soft X-ray outburst at the viscous timescale of ∼8–12 days.
The Outermost Edges of the Milky Way Halo from Galaxy Kinematics
Authors: Li Zhao-Zhou , Han Jiaxin 
Published: July 2021

Abstract
We measure for the first time the outermost edges of the Milky Way (MW) halo in terms of the depletion and turnaround radii. The inner depletion radius, r
id, identified at the location of maximum infall velocity, separates a growing halo from the draining environment, while the turnaround radius, r
ta, marks the outermost edge of infalling material toward the halo, both of which are located well outside the virial radius. Using the motions of nearby dwarf galaxies within 3 Mpc, we obtain a marginal detection of the infall zone around the MW with a maximum velocity of

v

inf
,
max

=
−

46

−
39

+
24

km

s

−
1

. This enables us to measure r
id = 559 ± 107 kpc and r
ta = 839 ± 121 kpc. The measured depletion radius is about 1.5 times the MW virial radius (R
200m) measured from internal dynamics. Compared with halos in the cosmological simulation Illustris TNG100, the factor 1.5 is consistent with that of halos with similar masses and dynamical environments to the MW but slightly smaller than typical values of Local Group analogs, potentially indicating the unique evolution history of the MW. These measurements of halo edges directly quantify the ongoing evolution of the MW outer halo and provide constraints on the current dynamical state of the MW that are independent from internal dynamics.
Les marchands ruraux et la commercialisation des campagnes dans l’Europe du XVIII e siècle
Authors: Villain Julien 
Published: July 2021

L’objet de cette recherche est d’estimer l’ampleur de la participation des habitants des campagnes de l’Europe du xviii e siècle aux relations de marché, en prenant la présence de marchands dans les villages comme indicateur du degré de « commercialisation » des économies. Le travail s’appuie sur le cas de la Lorraine centrale et méridionale, région relativement riche et développée à la veille de la Révolution. Le nombre de commerçants ruraux (exportateurs de productions locales ou d’importateurs de biens diffusés localement) y était élevé. Loin d’être seulement des colporteurs, ces marchands tenaient souvent boutique, quitte à coupler leurs activités avec d’autres – principalement l’agriculture, mais assez fréquemment l’artisanat. La vigueur de l’économie d’échanges rurale en Lorraine était réelle, sans toutefois atteindre celle des zones économiquement les plus dynamiques du continent comme les Provinces-Unies ou l’Angleterre méridionale.
Modélisation d’un nouveau procédé d’enquête. « La temporalité de la réception » : l’itinéraire d’un déplacement noétique
Authors: Mouchtouris Antigone 
Published: July 2021

Dans cet article est développée une nouvelle façon d’enquêter sur le terrain ; il s’agit d’un modèle d’enquête qui se présente comme un procédé afin de comprendre les interactions produites entre l’individu social et son environnement. À travers le cas paradigmatique entre un visiteur et une exposition dans un musée a été proposé un axe de recherche original. En considérant tout d’abord que cette expérience s’inscrit dans un itinéraire, qu’à travers cette dimension physique et mentale, les apports d’une visite muséale sont reconsidérés. Grâce à cette approche, nous avons pu observer la construction de la temporalité de la réception. Ce modèle d’enquête peut être appliqué pour d’autres situations et événements marquants ; d’autant plus s’il est à même de provoquer, au niveau mental, un déplacement noétique