bluuebunny/crossref_metadata_2025_split huggingface dataset:
PENGEMBANGAN MEDIA PEMBELAJARAN TERPADU BERBASIS APLIKASI FREEMIND DALAM MENINGKATKAN KUALITAS PEMBELAJARAN IPS DI JURUSAN PGMI FAKULTAS ILMU TARBIYAH DAN KEGURUAN UIN MAULANA MALIK IBRAHIM
Authors: Zahroh Nur Lailatus 
Published: November 2017

Penelitian ini dilatarbelakangi oleh ditemukannya permasalahan pada penelitian sebelumnya yaitu adanya model pembelajaran terpadu namun media yang digunakan masih terpisah. Oleh karena itu dibutuhkan sebuah media yang mampu memadukan semua materi IPS. Rumusan masalah difokuskan pada apakah media pembelajaran berbasis aplikasi <em>freemind </em>dapat meningkatkan kualitas pembelajaran IPS SD di SD di jurusan PGMI Fakultas Tarbiyah UIN Maulana Malik Ibrahim Malang. Metode yang digunakan dalam penelitian ini adalah <em>Research</em> <em>&amp; Development </em>Uji coba media dilakukan dengan metode eksperimen. Tiga hasil penelitian ini yaitu Media yang diproduksi adalah media pembelajaran dengan tema Indonesia klasik ini berupa media visual dari penggunaan aplikasi mindmap/freemind. Media pembelajaran berbasis aplikasi mindmap/freemind dapat meningkatkan kualitas pembelajaran IPS SD di jurusan PGMI UIN Maulana Malik Ibrahim Malang. Media pembelajaran berbasis aplikasi mindmap/freemind dapat meningkatkan pemahaman materi IPS Mahasiswa lebih tinggi dari pada media yang lain. Oleh karena itu media pembelajaran ini sebaiknya terus digunakan dalam pembelajaran IPS.
Einsatz digitaler Systeme zur Prozessüberwachung
Authors: Busse Alexander , Meudt Tobias , Metternich Joachim 
Published: November 2017

Kurzfassung
Maschinelles Lernen ermöglicht es, Gesetzmäßigkeiten automatisch aus Eingangsdaten und verknüpften Zielwerten zu „erlernen“ und Vorhersagen abzuleiten. Dies kann in der Produktion zur Prozessstabilisierung genutzt werden. Ein strukturierter Implementierungsansatz ist nötig, der datentechnische Anforderungen definiert und den Nutzen der digitalen zur analogen Problemlösungen abwägt. Am Institut PTW der TU Darmstadt wurde ein solcher Ansatz entwickelt. Erste Versuche zeigen, dass die Methode gezieltes maschinelles Lernen unterstützt und akkurate Vorhersagen zur Prozessstabilisierung ermöglicht.
Präzisionsbeschnitt von CFK-Metall-Verbunden
Authors: Rennau Axel , Dix Martin 
Published: November 2017

Kurzfassung
Besonders für Materialien mit stark differenten Eigenschaften stellt das Wasserabrasivstrahlschneiden eine Alternative zu konventionellen Trennverfahren dar. Dieser Beitrag stellt den Präzisionsbeschnitt von dreidimensionalen CFK-Aluminium-Verbunden mittels Feinstrahlschneiden vor. Der Fokus liegt auf der Untersuchung verschiedener Schneidstrategien und deren Einfluss auf die Eigenschaften des Verbundes. Es wird gezeigt, dass Düsenführung und Parameterwahl entscheidend für die Bauteilqualität sind.
Moderne Sicherheitskonzepte für Industrie 4.0
Authors: Smits Erwan 
Published: November 2017

Kurzfassung
Die zunehmende Vernetzung und die steigende Zahl an Datentransfers in modernen Fertigungsumgebungen ebnen nicht nur den Weg für gezieltere Kommunikation und individuelle Kundenansprache, sondern auch für neue Sicherheitsrisiken. Ein dreistufiger Sicherheitsansatz mit „Trust Brokern“, Sicherheitsanalysefähigkeiten und vertrauenswürdigen Komponenten schirmt Industrie-4.0-Plattformen gegen Angriffe von innen und außen ab.
Modellierung von elastischen Fügeverbindungen
Authors: Rudolph Holger , Ihlenfeldt Steffen 
Published: November 2017

KurzfassungIm Rahmen der Analyse und Bewertung des dynamischen Verformungsverhaltens von Werkzeugmaschinen kommt der modellgestützten Ermittlung des Eigenschwingungsverhaltens sowie der Nachgiebigkeitsfrequenzgänge eine zentrale Bedeutung zu. Hierzu erfordern die Modelle neben einer weitgehend gesicherten Parametrierung der Strukturbauteile auch geeignete Modellierungsansätze für die Fügeverbindungen zwischen den Bauteilen. Der vorliegende Beitrag stellt aktuelle Ergebnisse zur experimentellen Untersuchung realer Kontaktflächen und zur Analyse alternativer Modellierungsansätze innerhalb der Finite-Elemente-Methode vor.
Kompetenzorientierte Arbeitsplatzwechsel
Authors: Denkena Berend , Stobrawa Sebastian , Jenkner Ilka 
Published: November 2017

Kurzfassung
Industrieunternehmen wissen, dass in Zeiten des demografischen Wandels und der Digitalisierung die Kompetenzen der Belegschaft gesichert und ausgebaut werden müssen. Die Herausforderung besteht dabei in der Identifizierung von geeigneten Maßnahmen und deren Einbindung in den operativen Alltag. Der folgende Beitrag stellt einen Ansatz zur Jobrotation vor, der Übungsniveaus aufrechterhält sowie Kompetenzdefizite ermittelt und damit eine Entscheidungsunterstützung für die Personaleinsatzplanung bietet.
KMU 4.0: Arbeiten und Lernen mit digitalen Medien
Authors: Schuh Günther , Mühlbradt Thomas , Prote Jan-Philipp , Luckert Melanie , Ays Julian , Lensing Wilhelm 
Published: November 2017

Kurzfassung
Industrie 4.0 und die dafür benötigte digitale Transformation von Unternehmen stellen Betriebe und Beschäftigte vor eine große Herausforderung. In diesem Beitrag wird ein Qualifizierungskonzept für kleine und mittlere Unternehmen (KMU) vorgestellt, welches im Rahmen des Projekts „KMU 4.0“ entwickelt und erprobt wird. Am Beispiel der Einführung einer digitalen Lernlösung bei der Polierscheibenfabrik Spaeth werden die Herausforderungen und Vorteile digitaler Medien im Unternehmensalltag vorgestellt und diskutiert.
Das Projekt „PALM4.Q“
Authors: Ostermeier Manuela , Hesse Christina , Mühlbradt Thomas , Kuhlang Peter 
Published: November 2017

Kurzfassung
Die Firma Leopold Kostal GmbH & Co.KG steht, genau wie viele andere Unternehmen in Deutschland mit dem Schwerpunkt in der manuellen Montage, vor diversen Herausforderungen. Um die Mitarbeiter auf aktuelle und zukünftige Anforderungen vorzubereiten, führt das Unternehmen das Projekt PALM4.Q am Standort Lüdenscheid durch. Der Beitrag beschreibt die Vorgehensweise im Projekt und die bisherigen Ergebnisse.
Glaciological Observations on Some of the Outlet Glaciers of South-West Vatnajökull, Iceland, 1954: Part II: Ogives
Authors: King Cuchlaine A. M. , Ives J. D. 
Published: November 2017

AbstractObservations and measurements of ogives on Morsárjökull, Svinafellsjökull and Falljökull are given and discussed. The problems associated with the smaller ogives on Svínafellsjökull and the ridges below the ice falls are considered.
Electron Heating and Saturation of Self-regulating Magnetorotational Instability in Protoplanetary Disks
Authors: Mori Shoji , Muranushi Takayuki , Okuzumi Satoshi , Inutsuka Shu-ichiro 
Published: November 2017

Abstract
Magnetorotational instability (MRI) has the potential to generatevigorous turbulence in protoplanetary disks, although its turbulence strength and accretion stress remain debatable because of the uncertainty of MRI with a low ionization fraction. We focus on the heating of electrons by strong electric fields, which amplifies nonideal magnetohydrodynamic effects. The heated electrons frequently collide with and stick to dust grains, which in turn decreases the ionization fraction and is expected to weaken the turbulent motion driven by MRI. In order to quantitatively investigate the nonlinear evolution of MRI, including the electron heating, we perform magnetohydrodynamical simulation with the unstratified shearing box. We introduce a simple analytic resistivity model depending on the current density by mimicking the resistivity given by the calculation of ionization. Our simulation confirms that the electron heating suppresses magnetic turbulence when the electron heating occurs with low current density. We find a clear correlation between magnetic stress and current density, which means that the magnetic stress is proportional to the squared current density. When the turbulent motion is completely suppressed, laminar accretion flow is caused by an ordered magnetic field. We give an analytical description of the laminar stateusing a solution of linear perturbation equations with resistivity. We also propose a formula that successfully predicts the accretion stress in the presence of the electron heating.
A Detached Protostellar Disk around a ∼0.2 M⊙ Protostar in a Possible Site of a Multiple Star Formation in a Dynamical Environment in Taurus
Authors: Tokuda Kazuki , Onishi Toshikazu , Saigo Kazuya , Hosokawa Takashi , Matsumoto Tomoaki , Inutsuka Shu-ichiro , Machida Masahiro N. , Tomida Kengo , Kunitomo Masanobu , Kawamura Akiko , Fukui Yasuo , Tachihara Kengo 
Published: November 2017

Abstract
We report ALMA observations in 0.87 mm continuum and 12CO (J = 3–2) toward a very low-luminosity (<0.1 L
⊙) protostar, which is deeply embedded in one of the densest cores, MC27/L1521F, in Taurus with an indication of multiple star formation in a highly dynamical environment. The beam size corresponds to ∼20 au, and we have clearly detected blueshifted/redshifted gas in 12CO associated with the protostar. The spatial/velocity distributions of the gas show there is a rotating disk with a size scale of ∼10 au, a disk mass of ∼10−4
M
⊙, and a central stellar mass of ∼0.2 M
⊙. The observed disk seems to be detached from the surrounding dense gas, although it is still embedded at the center of the core whose density is ∼106 cm−3. The current low-outflow activity and the very low luminosity indicate that the mass accretion rate onto the protostar is extremely low in spite of a very early stage of star formation. We may be witnessing the final stage of the formation of ∼0.2 M
⊙ protostar. However, we cannot explain the observed low luminosity with the standard pre-main-sequence evolutionary track unless we assume cold accretion with an extremely small initial radius of the protostar (∼0.65

). These facts may challenge our current understanding of the low mass star formation, in particular the mass accretion process onto the protostar and the circumstellar disk.
VLBA Trigonometric Parallax Measurement of the Semi-regular Variable RT Vir
Authors: Zhang Bo , Zheng Xingwu , Reid Mark J. , Honma Mareki , Menten Karl M. , Brunthaler Andreas , Kim Jaeheon 
Published: November 2017

Abstract
We report a trigonometric parallax measurement of 22 GHz H2O masers toward the semi-regular variable RT Vir from multi-epoch Very Long Baseline Array observations. The parallax of 4.417 ± 0.134 mas, corresponding to a distance of 226 ± 7 pc, is significantly different from the Hipparcos parallax, but is consistent with a distance derived from the period–luminosity relation (PLR). This suggests that the Hipparcos parallax suffers from systematic bias, possibly owing to a variable photo-center for this giant star. As such, VLBI parallax measurements will serve as an important cross-check for Gaia. Combing our RT Vir parallax with other long period variable parallaxes, we find a Galactic PLR at an infrared K band of

, assuming that the slope of the Large Magellanic Cloud relation is the same to that of our Galaxy.
Clearing Residual Planetesimals by Sweeping Secular Resonances in Transitional Disks: A Lone-planet Scenario for the Wide Gaps in Debris Disks around Vega and Fomalhaut
Authors: Zheng 郑晓 Xiaochen 晨 , Lin 林 Douglas N. C. 潮 , Kouwenhoven 柯文 M. B. N. 采 , Mao 毛淑 Shude 德 , Zhang 张晓 Xiaojia 佳 
Published: November 2017

Abstract
Extended gaps in the debris disks of both Vega and Fomalhaut have been observed. These structures have been attributed to tidal perturbations by multiple super-Jupiter gas giant planets. Within the current observational limits, however, no such massive planets have been detected. Here we propose a less stringent “lone-planet” scenario to account for the observed structure with a single eccentric gas giant and suggest that clearing of these wide gaps is induced by its sweeping secular resonance. With a series of numerical simulations, we show that the gravitational potential of the natal disk induces the planet to precess. At the locations where its precession frequency matches the precession frequency the planet imposes on the residual planetesimals, their eccentricity is excited by its resonant perturbation. Due to the hydrodynamic drag by the residual disk gas, the planetesimals undergo orbital decay as their excited eccentricities are effectively damped. During the depletion of the disk gas, the planet’s secular resonance propagates inward and clears a wide gap over an extended region of the disk. Although some residual intermediate-size planetesimals may remain in the gap, their surface density is too low to either produce super-Earths or lead to sufficiently frequent disruptive collisions to generate any observable dusty signatures. The main advantage of this lone-planet sweeping-secular-resonance model over the previous multiple gas giant tidal truncation scenario is the relaxed requirement on the number of gas giants. The observationally inferred upper mass limit can also be satisfied provided the hypothetical planet has a significant eccentricity. A significant fraction of solar or more massive stars bear gas giant planets with significant eccentricities. If these planets acquired their present-day kinematic properties prior to the depletion of their natal disks, their sweeping secular resonance would effectively impede the retention of neighboring planets and planetesimals over a wide range of orbital semimajor axes.
Diverse Nuclear Star-forming Activities in the Heart of NGC 253 Resolved with 10-pc-scale ALMA Images
Authors: Ando Ryo , Nakanishi Kouichiro , Kohno Kotaro , Izumi Takuma , Martín Sergio , Harada Nanase , Takano Shuro , Kuno Nario , Nakai Naomasa , Sugai Hajime , Sorai Kazuo , Tosaki Tomoka , Matsubayashi Kazuya , Nakajima Taku , Nishimura Yuri , Tamura Yoichi 
Published: November 2017

Abstract
We present an 8 pc × 5 pc resolution view of the central ∼200 pc region of the nearby starburst galaxy NGC 253, based on ALMA Band 7 (

or

GHz) observations covering 11 GHz. We resolve the nuclear starburst of NGC 253 into eight dusty star-forming clumps, 10 pc in scale, for the first time. These clumps, each of which contains (4–10)

of dust (assuming that the dust temperature is 25 K) and up to

massive (O5V) stars, appear to be aligned in two parallel ridges, while they have been blended in previous studies. Despite the similarities in sizes and dust masses of these clumps, their line spectra vary drastically from clump to clump, although they are separated by only ∼10 pc. Specifically, one of the clumps, Clump 1, exhibits line-confusion-limited spectra with at least 36 emission lines from 19 molecules (including CH3OH, HNCO, H2CO, CH3CCH, H2CS, and H3O+) and a hydrogen recombination line (H26α), while far fewer kinds of molecular lines are detected in some other clumps where fragile species, such as complex organic molecules and HNCO, completely disappear from their spectra. We demonstrate the existence of hot molecular gas (

K) in the former clump, which suggests that the hot and chemically rich environments are localized within a 10-pc-scale star-forming clump.
Inflows, Outflows, and a Giant Donor in the Remarkable Recurrent Nova M31N 2008-12a?—Hubble Space Telescope Photometry of the 2015 Eruption
Authors: Darnley M. J. , Hounsell R. , Godon P. , Perley D. A. , Henze M. , Kuin N. P. M. , Williams B. F. , Williams S. C. , Bode M. F. , Harman D. J. , Hornoch K. , Link M. , Ness J.-U. , Ribeiro V. A. R. M. , Sion E. M. , Shafter A. W. , Shara M. M. 
Published: November 2017

Abstract
The recurrent nova M31N 2008-12a experiences annual eruptions, contains a near-Chandrasekhar-mass white dwarf, and has the largest mass accretion rate in any nova system. In this paper, we present Hubble Space Telescope (HST) WFC3/UVIS photometry of the late decline of the 2015 eruption. We couple these new data with archival HST observations of the quiescent system and Keck spectroscopy of the 2014 eruption. The late-time photometry reveals a rapid decline to a minimum luminosity state, before a possible recovery/rebrightening in the run up to the next eruption. Comparison with accretion disk models supports the survival of the accretion disk during the eruptions, and uncovers a quiescent disk mass accretion rate of the order of

10

−
6

M

⊙

yr

−
1

, which may rise beyond

10

−
5

M

⊙

yr

−
1

during the super-soft source phase—both of which could be problematic for a number of well-established nova eruption models. Such large accretion rates, close to the Eddington limit, might be expected to be accompanied by additional mass loss from the disk through a wind and even through collimated outflows. The archival HST observations, combined with the disk modeling, provide the first constraints on the mass donor:

L

donor

=

103

−
11

+
12

L

⊙

,

R

donor

=

14.14

−
0.47

+
0.46

R

⊙

, and

T

eff
,
donor

=
4890
±
110

K, which may be consistent with an irradiated M31 red-clump star. Such a donor would require a system orbital period

≳
5

days. Our updated analysis predicts that the M31N 2008-12a WD could reach the Chandrasekhar mass in

<
20

kyr.
Probing Subsurface Flows in NOAA Active Region 12192: Comparison with NOAA 10486
Authors: Jain Kiran , Tripathy S. C. , Hill F. 
Published: November 2017

Abstract
NOAA Active Region (AR) 12192 is the biggest AR observed in solar cycle 24 so far. This was a long-lived AR that survived for four Carrington rotations (CRs) and exhibited several unusual phenomena. We measure the horizontal subsurface flows in this AR in multiple rotations using the ring-diagram technique of local helioseismology and the Global Oscillation Network Group (GONG+) Dopplergrams, and we investigate how different was the plasma flow in AR 12192 from that in AR 10486. Both regions produced several high M- and X-class flares, but they had different coronal mass ejection (CME) productivity. Our analysis suggests that these ARs had unusually large horizontal flow amplitude with distinctly different directions. While meridional flow in AR 12192 was poleward that supports the flux transport to poles, it was equatorward in AR 10486. Furthermore, there was a sudden increase in the magnitude of estimated zonal flow in shallow layers in AR 12192 during the X3.1 flare; however, it reversed direction in AR 10486 with the X17.2 flare. These flow patterns produced strong twists in horizontal velocity with depth in AR 10486 that persisted throughout the disk passage, as opposed to AR 12192, which produced a twist only after the eruption of the X3.1 flare that disappeared soon after. Our study indicates that the sunspot rotation combined with the reorganization of magnetic field in AR 10486 was not sufficient to decrease the flow energy even after several large flares that might have triggered CMEs. Furthermore, in the absence of sunspot rotation in AR 12192, this reorganization of magnetic field contributed significantly to the substantial release of flow energy after the X3.1 flare.
Transport Properties of the Azimuthal Magnetorotational Instability
Authors: Guseva Anna , Willis Ashley P. , Hollerbach Rainer , Avila Marc 
Published: November 2017

Abstract
The magnetorotational instability (MRI) is thought to be a powerful source of turbulence in Keplerian accretion disks. Motivated by recent laboratory experiments, we study the MRI driven by an azimuthal magnetic field in an electrically conducting fluid sheared between two concentric rotating cylinders. By adjusting the rotation rates of the cylinders, we approximate angular velocity profiles

. We perform direct numerical simulations of a steep profile close to the Rayleigh line

and a quasi-Keplerian profile

and cover wide ranges of Reynolds (

) and magnetic Prandtl numbers (

). In the quasi-Keplerian case, the onset of instability depends on the magnetic Reynolds number, with

, and angular momentum transport scales as

in the turbulent regime. The ratio of Maxwell to Reynolds stresses is set by Rm. At the onset of instability both stresses have similar magnitude, whereas the Reynolds stress vanishes or becomes even negative as Rm increases. For the profile close to the Rayleigh line, the instability shares these properties as long as

but exhibits a markedly different character if

, where the onset of instability is governed by the Reynolds number, with

, and transport is via Reynolds stresses and scales as Re2. At intermediate Pm = 0.01 we observe a continuous transition from one regime to the other, with a crossover at

. Our results give a comprehensive picture of angular momentum transport of the MRI with an imposed azimuthal field.
Physical Properties of 15 Quasars at z ≳ 6.5
Authors: Mazzucchelli C. , Bañados E. , Venemans B. P. , Decarli R. , Farina E. P. , Walter F. , Eilers A.-C. , Rix H.-W. , Simcoe R. , Stern D. , Fan X. , Schlafly E. , Rosa G. De , Hennawi J. , Chambers K. C. , Greiner J. , Burgett W. , Draper P. W. , Kaiser N. , Kudritzki R.-P. , Magnier E. , Metcalfe N. , Waters C. , Wainscoat R. J. 
Published: November 2017

Abstract
Quasars are galaxies hosting accreting supermassive black holes; due to their brightness, they are unique probes of the early universe. To date, only a few quasars have been reported at

(<800 Myr after the big bang). In this work, we present six additional

quasars discovered using the Pan-STARRS1 survey. We use a sample of 15

quasars to perform a homogeneous and comprehensive analysis of this highest-redshift quasar population. We report four main results: (1) the majority of

quasars show large blueshifts of the broad C iv
λ1549 emission line compared to the systemic redshift of the quasars, with a median value ∼3× higher than a quasar sample at

; (2) we estimate the quasars’ black hole masses (

(0.3–5) × 109
M
⊙) via modeling of the Mg ii
λ2798 emission line and rest-frame UV continuum and find that quasars at high redshift accrete their material (with

) at a rate comparable to a luminosity-matched sample at lower redshift, albeit with significant scatter (0.4 dex); (3) we recover no evolution of the Fe ii/Mg ii abundance ratio with cosmic time; and (4) we derive near-zone sizes and, together with measurements for

quasars from recent work, confirm a shallow evolution of the decreasing quasar near-zone sizes with redshift. Finally, we present new millimeter observations of the [C ii] 158 μm emission line and underlying dust continuum from NOEMA for four quasars and provide new accurate redshifts and [C ii]/infrared luminosity estimates. The analysis presented here shows the large range of properties of the most distant quasars.
In silico identification of cytotoxic T lymphocyte epitopes encoded by RD5 region of Mycobacterium tuberculosis
Authors: Zhao Jun-Wei , Yan Min , Shi Guang , Zhang Shu-Lin , Ming Liang 
Published: November 2017

Introduction: While CD8+ T cells (cytotoxic T lymphocytes, CTLs) play important roles in immunity against Mycobacterium tuberculosis, only a small number of human leukocyte differentiation antigen (HLA) class I-restricted CTL epitopes for TB have been identified. The current study evaluates CTL epitopes of Rv3117 and Rv3120 proteins, two newly found M. tuberculosis region-diffference-5 (RD5)-encoded antigens, and their population coverage.
Methodology: The amino acid sequences of the two proteins were subjected to epitope analysis under HLA-A2, A3 and B7 supertype restriction using NetCTL, SYFPEITHI, BIMAS, NetCTLPan, IEDB, NetMHC and NetMHCPan prediction online servers.
Results: Eight RD5-encoded CTL epitopes were identified in the two proteins and the average population coverage of these epitopes was 87.2% among populations worldwide.
Conclusion: These CTL epitopes that were identified in silico and may have potential use for CD8+ T cell-mediated TB vaccine design.