bluuebunny/crossref_metadata_2025_split huggingface dataset:
Literatur interpretieren
Authors: Candel Bormann Daniel 
Published: November 2021

Analyse-Modelle für denkende Leser - mit Apps und Videos auf YouTube!
Das hier vorgestellte Analyse-Modell zur Interpretation von Literatur basiert auf semantischen Kategorien, ist praxisorientiert und einfach anwendbar.
Modelle sind nötig bei der Interpretation von Literatur, sie müssen aber zu Werkzeugen ausreifen, die beschreibbar und handhabbar sind.
Viele Beispiele aus verschiedenen Sprachen zeigen, wie die Interpretation von fiktionaler Prosa und Dichtung, von Filmen, Karikaturen und Bildern gelingen kann. Dabei werden bewährte kognitive und semantische Ansätze genutzt. Mit Aufgaben und Lösungsvorschlägen.
Mit diesem Analyse-Tool wird Interpretation endlich zu einer erlernbaren und nachvollziehbaren Technik.
Das Analyse-Tool erscheint 2013 auch in den renommierten Fachzeitschriften Semiotica und Poetics Today.
Ethisch reflektierter Geschichtsunterricht
Authors: Weber Karl-Christian 
Published: November 2021

Fragen an die Geschichte - ethisch fundiert
Ethische Fragestellungen durchdringen zunehmend den Geschichtsunterricht und halten Einzug in die Lehramtsausbildung.
Dieser Band zum modernen Geschichtsunterricht verknüpft erstmals ethische Fragen systematisch mit modernen geschichtsdidaktischen und -methodischen Ansätzen.
Ziel ist eine neue Form des Geschichtsunterrichts, die kompetenzorientiert und innovativ ist.
Der Geschichtsunterricht der Zukunft stellt sich ethischen Fragestellungen. Hier wird beschrieben, wie das gelingen kann.
Theatergeschichte
Authors: Kotte Andreas 
Published: November 2021

Von der antiken Tragödie bis zum "postdramatischen" Theater
In sieben klar strukturierten Kapiteln stellt Andreas Kotte die Geschichte des europäischen Theaters von der Antike bis zur Gegenwart vor.
Dabei geht er Impulsen, Neuerungen und Störfaktoren der Theaterentwicklung ebenso nach wie Veränderungen in den Rahmenbedingungen der Theaterkunst. Worin liegen die Ursprünge von Theater? Gab es ein Theatervakuum zwischen 530 und 930 und damit verbunden eine Wiederentdeckung von Theater im späten Mittelalter und in der Renaissance? Wie verhalten sich Theater und Medien zueinander?
Dieses grundlegende Studienbuch bietet einen chronologischen Durchgang durch die Epochen der europäischen Theatergeschichte und zielt dabei auf die Erschließung zentraler Frage- und Problemstellungen.
Medienethik
Authors: Schicha Christian 
Published: November 2021

Die Einführung in die Medienethik widmet sich normativen Grundlagen der Verantwortung, Öffentlichkeit, Inszenierung, Authentizität und Qualität. Es werden journalistische Medienskandale aufgezeigt und eingeordnet. Weiterhin werden bildethische Dimensionen erörtert. Daran anknüpfend werden Aspekte der PR-, Werbe- und Internetethik thematisiert. Darüber hinaus werden Unterhaltungsformate und sogenannte Fake News kritisch reflektiert. Des weiteren werden medienethische Initiativen vorgestellt, bevor eine kommentierte Auswahlbibliographie zur Medienethik den Band abgerundet.
PENGARUH MODEL PEMBELAJARAN PBL BERBANTUAN ALAT PERAGA DALAM PENINGKATAN KEMAMPUAN PENALARAN MATEMATIS
Authors: Aulya Richa , Purwaningrum Jayanti Putri 
Published: November 2021

Dalam pembelajaran matematika, kemampuan penalaran matematis siswa bersifat penting dikarenakan pembelajaran tersebut lebih ditekankan pada suatu aktivitas pemecahan masalah dan penalaran yang sangat erat serta berkaitan dengan pencapaian prestasi siswa. Namun, pada kondisi saat ini, penalaran matematis siswa dalam pembelajaran matematika masih dianggap kurang dan belum menekankan secara khusus. Penalaran matematis siswa yang masih rendah perlu diperbaiki dalam proses pembelajaran matematika. Ada beberapa cara untuk melatih siswa dalam bernalar yakni dengan menggunakan model pembelajaran dan alat peraga. Model pembelajaran yang dapat meningkatkan kemampuan penalaran matematis siswa agar menjadikan situasi belajar menyenangkan dan membuat siswa tidak merasa bosan yakni model pembelajaran problem based learning (PBL). Dengan menggabungkan model problem based learning dan alat peraga dapat meningkatkan kemampuan matematis siswa sehingga dapat tercapainya tujuan pembelajaran dan siswa tidak hanya sekedar menghafal melainkan juga memahami materi pelajaran.
Simultaneous Multiwavelength Flare Observations of EV Lacertae
Authors: Paudel Rishi R. , Barclay Thomas , Schlieder Joshua E. , Quintana Elisa V. , Gilbert Emily A. , Vega Laura D. , Youngblood Allison , L. Silverstein Michele , Osten Rachel A. , Tucker Michael A. , Huber Daniel , Do Aaron , Hamaguchi Kenji , Mullan D. J. , Gizis John E. , Monsue Teresa A. , Colón Knicole D. , Boyd Patricia T. , Davenport James R. A. , Walkowicz Lucianne 
Published: November 2021

Abstract
We present the first results of our ongoing project conducting simultaneous multiwavelength observations of flares on nearby active M dwarfs. We acquired data of the nearby dM3.5e star EV Lac using five different observatories: NASA’s Transiting Exoplanet Survey Satellite (TESS), NASA’s Neil Gehrels Swift Observatory (Swift), NASA’s Neutron Interior Composition Explorer (NICER), the University of Hawaii 2.2-meter telescope (UH88), and the Las Cumbres Observatory Global Telescope (LCOGT) Network. During the ∼25 days of TESS observations, we acquired three simultaneous UV/X-ray observations using Swift that total ∼18 ks, 21 simultaneous epochs totaling ∼98 ks of X-ray data using NICER, one observation (∼3 hr) with UH88, and one observation (∼3 hr) with LCOGT. We identified 56 flares in the TESS light curve with estimated energies in the range log E
T (erg) = (30.5–33.2), nine flares in the Swift UVM2 light curve with estimated energies in the range log E
UV (erg) = (29.3–31.1), 14 flares in the NICER light curve with estimated minimum energies in the range log E

N
(erg) = (30.5–32.3), and 1 flare in the LCOGT light curve with log E

L
(erg) = 31.6. We find that the flare frequency distributions (FFDs) of TESS and NICER flares have comparable slopes, β

T
= −0.67 ± 0.09 and β

N
= − 0.65 ± 0.19, and the FFD of UVOT flares has a shallower slope (β

U
= −0.38 ± 0.13). Furthermore, we do not find conclusive evidence for either the first ionization potential (FIP) or the inverse FIP effect during coronal flares on EV Lac.
Observational Evidence Points at AGB Stars as Possible Progenitors of CEMP-s and CEMP-r/s Stars*
Authors: Purandardas Meenakshi , Goswami Aruna 
Published: November 2021

Abstract
The origin of enhanced abundance of heavy elements observed in the surface chemical composition of carbon-enhanced metal-poor (CEMP) stars still remains poorly understood. Here, we present detailed abundance analysis of seven CEMP stars based on high-resolution (R ∼ 50,000) spectra that reveal enough evidence of asymptotic giant branch (AGB) stars being possible progenitors for these objects. For the objects HE 0110−0406, HE 1425−2052, and HE 1428−1950, we present for the first time a detailed abundance analysis. Our sample is found to consist of one metal-poor ([Fe/H] < −1.0) and six very metal-poor ([Fe/H] < −2.0) stars with enhanced carbon and neutron-capture elements. We have critically analyzed the observed abundance ratios of [O/Fe], [Sr/Ba], and [hs/ls] and examined the possibility of AGB stars being possible progenitors. The abundance of oxygen estimated in the program stars is characteristic of AGB progenitors except for HE 1429−0551 and HE 1447+0102. The estimated values of [Sr/Ba] and [hs/ls] ratios also support AGB stars as possible progenitors. The locations of the program stars in the absolute carbon abundance A(C) versus [Fe/H] diagram, along with the Group I objects, hint at the binary nature of the object. We have studied the chemical enrichment histories of the program stars based on abundance ratios [Mg/C], [Sc/Mn], and [C/Cr]. Using [C/N] and 12C/13C ratios, we have examined whether any internal mixing had modified their surface chemical compositions. Kinematic analysis shows that the objects HE 0110−0406 and HE 1447+0102 are thick-disk objects and the remaining five objects belong to the halo population of the Galaxy.
The IGRINS YSO Survey II: Veiling Spectra of Pre-main-sequence Stars in Taurus-Auriga
Authors: Kidder Benjamin , Mace Gregory , López-Valdivia Ricardo , Sokal Kimberly , Catlett Victoria E. , Gutiérrez Miguel , Tofflemire Benjamin M. , Jaffe Daniel 
Published: November 2021

Abstract
We present measurements of the H- and K-band veiling for 141 young stellar objects (YSOs) in the Taurus-Auriga star-forming region using high-resolution spectra from the Immersion Grating Near-Infrared Spectrometer. In addition to providing measurements of r

H
and r

K
, we produce low-resolution spectra of the excess emission across the H and K bands. We fit temperatures to the excess spectra of 46 members of our sample and measure near-infrared excess temperatures ranging from 1200–2200 K, with an average of 1575 ± 225 K. We compare the luminosity of the excess continuum emission in Class II and Class III YSOs and find that a number of Class III sources display a significant amount of excess flux in the near-infrared. We conclude that the mid-infrared SED slope, and therefore young stellar object classification, is a poor predictor of the amount of near-infrared veiling. If the veiling arises in thermal emission from dust, its presence implies a significant amount of remaining inner-disk (<1 au) material in these Class III sources. We also discuss the possibility that the veiling effects could result from massive photospheric spots, unresolved binary companions, or accretion emission. Six low-mass members of our sample contain a prominent feature in their H-band excess spectra that is consistent with veiling from cool photospheric spots.
Impact of Water-latent Heat on the Thermal Structure of Ultra-cool Objects: Brown Dwarfs and Free-floating Planets
Authors: Tang Shih-Yun , Robinson Tyler D. , Marley Mark S. , Batalha Natasha E. , Lupu Roxana , Prato L. 
Published: November 2021

Abstract
Brown dwarfs are essential targets for understanding planetary and sub-stellar atmospheres across a wide range of thermal and chemical conditions. As surveys continue to probe ever deeper and as observing capabilities continue to improve, the number of known Y dwarfs—the coldest class of sub-stellar objects, with effective temperatures below about 600 K—is rapidly growing. Critically, this class of ultra-cool objects has atmospheric conditions that overlap with solar-system worlds and, as a result, tools and ideas developed from studying Earth, Jupiter, Saturn, and other nearby worlds are well suited for application to sub-stellar atmospheres. To that end, we developed a one-dimensional (vertical) atmospheric structure model for ultra-cool objects that includes moist adiabatic convection, as this is an important process for many solar-system planets. Application of this model across a range of effective temperatures (350, 300, 250, 200 K), metallicities ([M/H] of 0.0, 0.5, 0.7, 1.5), and gravities (log g of 4.0, 4.5, 4.7, 5.0) demonstrates strong impact of water-latent heat release on simulated temperature-pressure profiles. At the highest metallicities, water-vapor mixing ratios reach an Earth-like 3% with associated major alterations to the thermal structure in the atmospheric regions where water condenses. Spectroscopic and photometric signatures of metallicity and moist convection should be readily detectable at near- and mid-infrared wavelengths, especially with James Webb Space Telescope observations, and can help indicate the formation history of an object.
Detached Shell Carbon Stars: Tracing Thermal Pulses on the Asymptotic Giant Branch
Authors: Kastner Joel H. , Wilson Emily 
Published: November 2021

Abstract
We consider whether the subset of carbon-rich asymptotic giant branch (AGB) stars that exhibit detached, expanding circumstellar shells may reveal the past histories of these stars as having undergone helium shell flashes (thermal pulses) on the AGB. We exploit newly available Gaia parallaxes and photometry, along with archival infrared photometry, to obtain refined estimates of the luminosities of all (12) known detached shell carbon stars. We examine the relationship between these luminosities and the estimated dynamical ages (ejection times) of the detached shells associated with the 12 stars, which range from ∼1000 to ∼30,000 yr. When arranged according to detached shell dynamical age, the (implied) luminosity evolution of the known detached shell carbon stars closely follows the predicted “light curves” of individual thermal pulses obtained from models of AGB stars. The comparison between data and models suggests that detached shell carbon stars are descended from ∼2.5 to 4.0 M
⊙ progenitors. We conclude that detached shell carbon stars may serve as effective tracers of the luminosity evolution of AGB thermal pulses.
Circumstellar Medium Constraints on the Environment of Two Nearby Type Ia Supernovae: SN 2017cbv and SN 2020nlb
Authors: Sand D. J. , Sarbadhicary S. K. , Pellegrino C. , Misra K. , Dastidar R. , Brown P. J. , Itagaki K. , Valenti S. , Swift Jonathan J. , Andrews J. E. , Bostroem K. A. , Burke J. , Chomiuk L. , Dong Y. , Galbany L. , Graham M. L. , Hiramatsu D. , Howell D. A. , Hsiao E. Y. , Janzen D. , Jencson J. E. , Lundquist M. J. , McCully C. , Reichart D. , Smith Nathan , Wang Lingzhi , Wyatt S. 
Published: November 2021

Abstract
We present deep Chandra X-ray observations of two nearby Type Ia supernovae, SN 2017cbv and SN 2020nlb, which reveal no X-ray emission down to a luminosity L
X ≲ 5.3 × 1037 and ≲ 5.4 × 1037 erg s−1 (0.3–10 keV), respectively, at ∼16–18 days after the explosion. With these limits, we constrain the pre-explosion mass-loss rate of the progenitor system to be

M

̇

< 7.2 × 10−9 and < 9.7 × 10−9
M
⊙ yr−1 for each (at a wind velocity v

w
= 100 km s−1 and a radius of R ≈ 1016 cm), assuming any X-ray emission would originate from inverse Compton emission from optical photons upscattered by the supernova shock. If the supernova environment was a constant-density medium, we would find a number density limit of n
CSM < 36 and < 65 cm−3, respectively. These X-ray limits rule out all plausible symbiotic progenitor systems, as well as large swathes of parameter space associated with the single degenerate scenario, such as mass loss at the outer Lagrange point and accretion winds. We also present late-time optical spectroscopy of SN 2020nlb, and set strong limits on any swept up hydrogen (L
Hα
< 2.7 × 1037 erg s−1) and helium (L
He,λ6678 < 2.7 × 1037 erg s−1) from a nondegenerate companion, corresponding to M

H
≲ 0.7–2 × 10−3
M
⊙ and M
He ≲ 4 × 10−3
M
⊙. Radio observations of SN 2020nlb at 14.6 days after explosion also yield a non-detection, ruling out most plausible symbiotic progenitor systems. While we have doubled the sample of normal Type Ia supernovae with deep X-ray limits, more observations are needed to sample the full range of luminosities and subtypes of these explosions, and set statistical constraints on their circumbinary environments.
Rapid Formation of Gas-giant Planets via Collisional Coagulation from Dust Grains to Planetary Cores
Authors: Kobayashi Hiroshi , Tanaka Hidekazu 
Published: November 2021

Abstract
Gas-giant planets, such as Jupiter, Saturn, and massive exoplanets, were formed via the gas accretion onto the solid cores, each with a mass of roughly 10 Earth masses. However, rapid radial migration due to disk–planet interaction prevents the formation of such massive cores via planetesimal accretion. Comparably rapid core growth via pebble accretion requires very massive protoplanetary disks because most pebbles fall into the central star. Although planetesimal formation, planetary migration, and gas-giant core formation have been studied with a lot of effort, the full evolution path from dust to planets is still uncertain. Here we report the result of full simulations for collisional evolution from dust to planets in a whole disk. Dust growth with realistic porosity allows the formation of icy planetesimals in the inner disk (≲10 au), while pebbles formed in the outer disk drift to the inner disk and there grow to planetesimals. The growth of those pebbles to planetesimals suppresses their radial drift and supplies small planetesimals sustainably in the vicinity of cores. This enables rapid formation of sufficiently massive planetary cores within 0.2–0.4 million years, prior to the planetary migration. Our models shows the first gas giants form at 2–7 au in rather common protoplanetary disks, in agreement with the exoplanet and solar systems.
Color Dependence of Planetary Transit Depths due to Large Starspots and Dust Clouds: Application to PTFO 8-8695
Authors: Grosson Theodore A. , Johns-Krull Christopher M. 
Published: November 2021

Abstract
Although thousands of exoplanets have now been discovered, there is still a significant lack of observations of young planets only a few Myr old. Thus there is little direct evidence available to differentiate between various models of planet formation. The detection of planets of this age would provide much-needed data that could help constrain the planet formation process. To explore what transit observations of such planets may look like, we model the effects of large starspots and dust clouds on the depths of exoplanet transits across multiple wavelengths. We apply this model to the candidate planet PTFO 8-8695b, whose depths vary significantly across optical and infrared wavelengths. Our model shows that, while large starspots can significantly increase the color dependence of planetary transits, a combination of starspots and a large cloud surrounding the planet is required to reproduce the observed transit depths across four wavelengths.
Analysis of Cohesion in Fast-spinning Small Bodies
Authors: Li Xiangyu , Scheeres Daniel J. 
Published: November 2021

Abstract
In this paper, the structural stability of a fast-spinning small body is investigated. In particular, a nonlinear yield condition in tensile stress is applied to estimate the required cohesion in a fast-spinning small body. The least upper bound of required cohesion is investigated for both ellipsoid and irregular shape models. The stress state of a fast-spinning ellipsoid is discussed analytically, and the effects of spin rates and size ratios are analyzed. For an irregularly shaped body, an element average stress method is developed to estimate the range of stress of any element in the body, where only self-gravity and centrifugal force are considered. The maximum tensile stress in the whole body is used to solve the required cohesion. Finally, the proposed methods are applied to different asteroid shape models. The result shows that the least upper bound of cohesion is mainly determined by the spin rate and length of the major axis, but an irregular shape will change the stress distribution and cause a stressed surface. The required cohesion of a fast-spinning small body varies between tens to 1000 Pa. The methods developed in this paper can rapidly provide a conservative lower bound on the cohesion in a fast-spinning body and qualitatively show the distribution of stress, which provides an effective way to study the structural stability of fast-spinning bodies of those bodies.
A Features Fusion Approach for Neonatal and Pediatrics Brain Tumor Image Analysis Using Genetic and Deep Learning Techniques
Authors: SJ Prashantha , Prakash H.N. 
Published: November 2021

Nowadays, Deep learning (DL) is the growing trend towards creating visual representations of human body organs for clinical analysis, medical interventions as well as to diagnose and treat diseases. This paper propose a method for neonatal and pediatric brain tumors image analysis and prerequisites a T2- weighted MR images only. The pipeline stages of the proposed work as follows: In the first stage, designed a set of specific feature vectors description for high-level classification task using Conventional and deep learning (DL) Feature Extraction methods. The second stage, select a deep features based on proposed convolutional neural network (CNN) method and conventional subset features are from Genetic Algorithm (GA). The third stage, merge the selected features by adapting fusion technique. Finally, predict the brain image is either normal or abnormal. The results demonstrated that the proposed method obtained accurate classification and revealed its robustness to difference in ages and acquisition protocols. The obtained results shows that based on combined deep learning features (DLF) and conventional features have been significantly improves the classification accuracy of the support vector machines (SVM) classifier up to 97.00%.
Archaeological Evidence for Population Rise and Collapse between ~2500 and ~500 cal. yr BP in Western Central Africa
Authors: Saulieu Geoffroy de , Garcin Yannick , Sebag David , Nlend Pascal R. Nlend , Zeitlyn David , Deschamps Pierre , Ménot Guillemette , Carlo Pierpaolo Di , Oslisly Richard 
Published: November 2021

Des études paléoenvironnementales antérieures ont montré que des changements majeurs de la végétation et de l’environnement se sont produits en Afrique centrale à partir de l’Holocène moyen (ex. Maley & Brenac 1998). Plusieurs d’entre elles mettent en évidence une origine humaine et supposent que les grandes migrations de population, les innovations techniques (par exemple, la technologie de la fonte du fer) et/ou de nouveaux choix dans les pratiques agricoles, conduisant à la déforestation et au défrichement, sont les moteurs de ces changements. Cependant, à ce stade, l’absence de reconstitution démographique ne permet pas de soutenir pleinement ces hypothèses. Notre étude utilise une base de données archéologiques géoréférencées pour déduire la dynamique des populations et l’évolution des pratiques culturelles en Afrique centrale occidentale au cours des 5000 dernières années. Cette base de données comprend 1139 dates calibrées au 14C provenant de 425 sites – localisés dans le sud du Cameroun, au Gabon, en République du Congo, en Guinée équatoriale et dans la partie occidentale de la République démocratique du Congo –, remontant à un maximum de 5000 ans cal. BP. La modélisation des données indique une possible croissance de la population entre ~2500 et ~1500 ans cal. BP, coïncidant avec l’apparition à l’échelle régionale de techniques et de pratiques spécifiques. L’augmentation concomitante des fosses dépotoirs, des vestiges d’utilisation de palmier à huile Elaeis guineesis, l’apparition de rares restes de millet Pennisetum glaucum et la montée en puissance des vestiges de métallurgie du fer ont eu lieu pendant la seconde moitié du Néolithique, à partir d’environ 2800 ans cal. BP. Dans les régions côtières, la croissance de la population concerne le Néolithique et le début de l’âge du fer (2500-2000 ans cal. BP et 2000-1500 ans cal. BP), tandis que dans l’Hinterland cette croissance semble légèrement plus tardive (2400 et 1300 ans cal. BP). Il n’est pas possible d’identifier un phénomène commun de diffusion à partir d’un seul centre. Les innovations techniques et les nouvelles pratiques semblent plutôt s’être répandues à travers un large réseau d’interactions culturelles qui a favorisé la formation des sociétés d’Afrique centrale occidentale au cours du troisième millénaire avant notre ère.