bluuebunny/crossref_metadata_2025_split huggingface dataset:
MARTIN LUTHER’S IDEAS ON THE GAME IN LEARNING
Authors: Толстова Е.В. , Иванов В.А. 
Published: June 2023

В статье рассматривается использование игровых приемов в обучении в эпоху Реформации, анализируются высказывания М. Лютера об игре. В Средние века данные формы обучения не вызывали интереса и не одобрялись церковью, но с наступлением Нового времени педагоги вновь начали считать игру действенным фактором развития ребенка. В переходное время, очевидно, произошло переосмысление игры, в том числе благодаря стараниям Лютера в деле просвещения народа. Многообразие игровых технологий сегодня, с одной стороны, дает огромные возможности для их применения в образовании, с другой стороны, обедняет ассортимент актуальных игр, дети разучиваются играть без гаджетов. Материалом для исследования послужили труды М. Лютера, а также работы на немецком и русском языках о педагогической деятельности реформатора. Исследование позволяет выявить специфику обращения Лютера к игре, применяемые и рекомендуемые им игровые формы. Одной из заслуг реформатора является внимание к ребенку и проявление уважения к детству как важному этапу в жизни. Педагогика Лютера исходит из его теологии, он стремился научить людей жить в соответствии со Священным Писанием. Реформатор призывал обучать детей с радостью и игрой, считал, что учитель должен стать ребенком и создавать положительную атмосферу на занятиях, чему способствует в том числе и музыка. На основании проведенного исследования делается вывод, что Лютер на исходе Средневековья выступал за гуманизацию обучения через игру как отвечающую детским потребностям деятельность, выявил ее педагогический потенциал, внес ценный вклад в дидактику.
The article discusses the use of game techniques in learning in the era of the Reformation, analyzes M. Luther’s statements about the game. In the Middle Ages, game forms of education did not arouse interest and were not approved by the church, but with the New Age, teachers consider the game to be an effective factor in the development of a child. In a transitional time, obviously, there is a rethinking of the game thanks to M. Luther’s efforts to educate people. The variety of game technologies today, on the one hand, provides great opportunities for their use in education, on the other hand, impoverishes the range of games, children cannot play without gadgets. The material for the study is the works of M. Luther, as well as the works in German and Russian on the pedagogical activity of the reformer. M. Luther’s pedagogy comes from his theology, he sought to teach people to live in accordance with the Holy Scriptures. The reformer called for teaching children with joy and play, the teacher should become a child and create a positive atmosphere in the classroom, which is achieved among other things by music. Based on the study, it is concluded that at the end of the Middle Ages M. Luther advocated the humanization of learning through play as an activity that meets children’s needs, he revealed its pedagogical potential and made a valuable contribution to didactics.
New Chondritic Bodies Identified in Eight Oxygen-bearing White Dwarfs
Authors: Doyle Alexandra E. , Klein Beth L. , Dufour Patrick , Melis Carl , Zuckerman B. , Xu Siyi , Weinberger Alycia J. , Trierweiler Isabella L. , Monson Nathaniel N. , Jura Michael A. , Young Edward D. 
Published: June 2023

Abstract
We present observations and analyses of eight white dwarf stars (WDs) that have accreted rocky material from their surrounding planetary systems. The spectra of these helium-atmosphere WDs contain detectable optical lines of all four major rock-forming elements (O, Mg, Si, and Fe). This work increases the sample of oxygen-bearing WDs with parent body composition analyses by roughly 33%. To first order, the parent bodies that have been accreted by the eight WDs are similar to those of chondritic meteorites in relative elemental abundances and oxidation states. Seventy-five percent of the WDs in this study have observed oxygen excesses implying volatiles in the parent bodies with abundances similar to those of chondritic meteorites. Three WDs have oxidation states that imply more reduced material than found in CI chondrites, indicating the possible detection of Mercury-like parent bodies, but are less constrained. These results contribute to the recurring conclusion that extrasolar rocky bodies closely resemble those in our solar system, and do not, as a whole, yield unusual or unique compositions.
Simulated Observations of Star Formation Regions: Infrared Evolution of Globally Collapsing Clouds
Authors: Jáquez-Domínguez Jesús M. , Galván-Madrid Roberto , Fritz Jacopo , Zamora-Avilés Manuel , Camps Peter , Bruzual Gustavo , Baes Maarten , Lin Yuxin , Vázquez-Semadeni Enrique 
Published: June 2023

Abstract
A direct comparison between hydrodynamical simulations and observations is needed to improve the physics included in the former and to test biases in the latter. Post-processing radiative transfer and synthetic observations are now the standard way to do this. We report on the first application of the SKIRT radiative-transfer code to simulations of a star-forming cloud. The synthetic observations are then analyzed following traditional observational workflows. We find that in the early stages of the simulation, stellar radiation is inefficient in heating dust to the temperatures that are observed in Galactic clouds, thus the addition of an interstellar radiation field is necessary. The spectral energy distribution of the cloud settles rather quickly after ∼3 Myr of evolution from the onset of star formation, but its morphology continues to evolve for ∼8 Myr due to the expansion of H ii regions and the respective creation of cavities, filaments, and ridges. Modeling synthetic Herschel fluxes with one- or two-component modified blackbodies underestimates total dust masses by a factor of ∼2. However, spatially resolved fitting recovers up to about 70% of the intrinsic value. This “missing mass” is located in a very cold dust component with temperatures below 10 K, which does not contribute appreciably to the far-infrared flux. This effect could bias real observations if this dust exists in large amounts. Finally, we tested observational calibrations of the SFR based on infrared fluxes and concluded that they are in agreement when compared to the intrinsic SFR of the simulation averaged over ∼100 Myr.
One Relation for All Wavelengths: The Far-ultraviolet to Mid-infrared Milky Way Spectroscopic R(V)-dependent Dust Extinction Relationship
Authors: Gordon Karl D. , Clayton Geoffrey C. , Decleir Marjorie , Fitzpatrick E. L. , Massa Derck , Misselt Karl A. , Tollerud Erik J. 
Published: June 2023

Abstract
Dust extinction is one of the fundamental measurements of dust grain sizes, compositions, and shapes. Most of the wavelength-dependent variations seen in Milky Way extinction are strongly correlated with the single parameter R(V) = A(V)/E(B − V). Existing R(V)-dependent extinction relationships use a mixture of spectroscopic and photometry observations, and hence do not fully capture all the important dust features or continuum variations. Using four existing samples of spectroscopically measured dust extinction curves, we consistently measure the R(V)-dependent extinction relationship spectroscopically from the far-ultraviolet (FUV) to mid-infrared for the first time. Linear fits of A(λ)/A(V) dependent on R(V) are done using a method that fully accounts for their significant and correlated uncertainties. These linear parameters are fit with analytic wavelength-dependent functions to determine the smooth R(V) (2.3–5.6) and wavelength (912 Å–32 μm) dependent extinction relationship. This relationship shows that the FUV rise, 2175 Å bump, and the three broad optical features are dependent on R(V), but the 10 and 20 μm features are not. Existing literature relationships show significant deviations compared to this relationship especially in the FUV and infrared (IR). Extinction curves that clearly deviate from this relationship illustrate that this relationship only describes the average behavior versus R(V). We find tentative evidence that the relationship may not be linear with R(V)−1 especially in the ultraviolet (UV). For the first time, this relationship provides measurements of dust extinction that spectroscopically resolve the continuum and features in the UV, optical, and IR as a function of R(V), enabling detailed studies of dust grain properties and full spectroscopic accounting for the effects of dust extinction on astrophysical objects.
Star Formation in the Dwarf Seyfert Galaxy NGC 4395: Evidence for Both AGN and SN Feedback?
Authors: Nandi Payel , Stalin C. S. , Saikia D. J. , Muneer S. , Mountrichas George , Wylezalek Dominika , Sagar R. , Kissler-Patig Markus 
Published: June 2023

Abstract
We present a detailed multiwavelength study of star formation in the dwarf galaxy NGC 4395, which hosts an active galactic nucleus (AGN). From our observations with the Ultra-Violet Imaging Telescope, we have compiled a catalog of 284 star-forming (SF) regions, out of which we could detect 120 SF regions in Hα observations. Across the entire galaxy, we found the extinction-corrected star formation rate (SFR) in the far ultraviolet (UV) to range from 2.0 × 10−5
M
⊙ yr−1 to 1.5 × 10−2
M
⊙ yr−1 with a median of 3.0 × 10−4
M
⊙ yr−1, and the age to lie in the range of ∼1 to 98 Myr with a median of 14 Myr. In Hα we found the SFR to range from 7.2 × 10−6
M
⊙ yr−1 to 2.7 × 10−2
M
⊙ yr−1 with a median of 1.7 × 10−4
M
⊙ yr−1, and the age to lie between 3 to 6 Myr with a median of 5 Myr. The stellar ages derived from Hα show a gradual decline with galactocentric distance. We found three SF regions close to the center of NGC 4395 with high SFRs both from Hα and UV, which could be attributed to feedback effects from the AGN. We also found six other SF regions in one of the spiral arms having higher SFRs. These are very close to supernova remnants, which could have enhanced the SFR locally. We obtained a specific SFR (SFR per unit mass) for the whole galaxy of 4.64 × 10−10 yr−1.
The Properties of Small Magnetic Flux Ropes inside the Solar Wind Come from Coronal Holes, Active Regions, and Quiet Sun
Authors: Zhai Changhao , Fu Hui , Si Jiachen , Huang Zhenghua , Xia Lidong 
Published: June 2023

Abstract
The origination and generation mechanisms of small magnetic flux ropes (SMFRs), which are important structures in solar wind, are not clearly known. In the present study, 1993 SMFRs immersed in coronal holes, active regions, and quiet-Sun solar wind are analyzed and compared. We find that the properties of SMFRs immersed in three types of solar wind are significantly different. The SMFRs are further classified into hot-SMFRs, cold-SMFRs, and normal-SMFRs, according to whether the O7+/O6+ is 30% elevated or dropped inside SMFRs as compared with background solar wind. Our studies show that the parameters of normal-SMFRs are similar to background in all three types of solar wind. The properties of hot-SMFRs and cold-SMFRs seem to be lying in two extremes. Statistically, the hot-SMFRs (cold-SMFRs) are associated with longer (shorter) duration, lower (higher) speeds and proton temperatures, higher (lower) charge states, helium abundance, and first ionization potential bias as compared with normal-SMFRs and background solar wind. The anticorrelations between speed and O7+/O6+ inside hot-SMFRs (normal-SMFRs) are different from (similar to) those in background solar wind. Most hot-SMFRs and cold-SMFRs should come from the Sun. Hot-SMFRs may come from streamers associated with plasma blobs and/or small-scale activities on the Sun. Cold-SMFRs may be accompanied by small-scale eruptions with lower-temperature materials. Both hot-SMFRs and cold-SMFRs could also be formed by magnetic erosions of interplanetary coronal mass ejections that do not contain or do contain cold-filament materials. The characteristics of normal-SMFRs can be explained reasonably by the two originations, both from the Sun and generated in the heliosphere.
Magnetar Giant Flare Origin for GRB 210410A?
Authors: Li Guo-Yu , Lin Da-Bin , Li Guo-Peng , Chen Zhi-Lin , Zhang Hai-Ming , Wang Xiang-Gao , Liang En-Wei 
Published: June 2023

Abstract
In general, giant flares (GFs) produced by magnetars have a very short-hard initial spike that is followed by a weak oscillatory phase. GFs from a nearby galaxy would appear as cosmic short-hard gamma-ray bursts (GRBs), such as GRB 200415A. In this paper, we search for GF-originated bursts in the Fermi GRB category and report GRB 210410A, which is presented with a very short-hard spike followed by an extended tail emission. In the E
p,z
− E
iso plane, GRB 210410A with a duration of T
90 ∼ 48 s differs from long GRBs, might be classified as a short GRB with a redshift of z ∼ 0.28, and could be regarded as a GF with a distance of ∼2.7 Mpc. Here, E
p,z
, E
iso, and L
iso denote the rest-frame peak photon energy, the isotropic energy, and the isotropic luminosity of the burst, respectively. The radiation spectrum of GRB 210410A, similar to that of GRB 200415A, can be well fitted with a non-dissipative photospheric emission. However, GRB 210410A in the E
p,z
− L
iso plane is beyond the death line of cosmic GRBs for non-dissipated photospheric emission with a general initial size of the fireball. Since the E
p,z
− L
iso relation of GFs is far beyond the death line of cosmic GRBs, GRB 210410A may have originated from the same channel that produces GFs. We also perform the analysis and discuss both the highest photon energy event (4.2 GeV) and the extended tail emission in this burst.
Nonparametric Representation of Neutron Star Equation of State Using Variational Autoencoder
Authors: Han Ming-Zhe , Tang Shao-Peng , Fan Yi-Zhong 
Published: June 2023

Abstract
We introduce a new nonparametric representation of the neutron star (NS) equation of state (EOS) by using the variational autoencoder (VAE). As a deep neural network, the VAE is frequently used for dimensionality reduction since it can compress input data to a low-dimensional latent space using the encoder component and then reconstruct the data using the decoder component. Once a VAE is trained, one can take the decoder of the VAE as a generator. We employ 100,000 EOSs that are generated using the nonparametric representation method based on Han et al. as the training set and try different settings of the neural network, then we get an EOS generator (the trained VAE’s decoder) with four parameters. We use the mass–tidal-deformability data of binary NS merger event GW170817, the mass–radius data of PSR J0030+0451, PSR J0740+6620, PSR J0437-4715, and 4U 1702-429, and the nuclear constraints to perform the Bayesian inference. The overall results of the analysis that includes all the observations are

R

1.4

=

12.59

−
0.42

+
0.36

km

,

Λ

1.4

=

489

−
110

+
114

, and

M

max

=

2.20

−
0.19

+
0.37

M

⊙

(90% credible levels), where R
1.4/Λ1.4 are the radius/tidal deformability of a canonical 1.4 M
⊙ NS, and

M

max

is the maximum mass of a nonrotating NS. The results indicate that the implementation of these VAE techniques can obtain reasonable results, while accelerating calculation by a factor of ∼3–10 or more, compared with the original method.
X-Ray Polarimetry of the Accreting Pulsar 1A 0535+262 in the Supercritical State with PolarLight
Authors: Long Xiangyun , Feng Hua , Li Hong , Kong Ling-Da , Heyl Jeremy , Ji Long , Tao Lian , Muleri Fabio , Wu Qiong , Zhu Jiahuan , Huang Jiahui , Minuti Massimo , Jiang Weichun , Citraro Saverio , Nasimi Hikmat , Yu Jiandong , Jin Ge , Zeng Ming , An Peng , Baldini Luca , Bellazzini Ronaldo , Brez Alessandro , Latronico Luca , Sgrò Carmelo , Spandre Gloria , Pinchera Michele , Soffitta Paolo , Costa Enrico 
Published: June 2023

Abstract
The X-ray pulsar 1A 0535+262 exhibited a giant outburst in 2020, offering us a unique opportunity for X-ray polarimetry of an accreting pulsar in the supercritical state. Measurement with PolarLight yielded a nondetection in 3–8 keV; the 99% upper limit of the polarization fraction (PF) is found to be 0.34 averaged over spin phases, or 0.51 based on the rotating vector model. No useful constraint can be placed with phase-resolved polarimetry. These upper limits are lower than a previous theoretical prediction of 0.6–0.8, but consistent with those found in other accreting pulsars, like Her X-1, Cen X-3, 4U 1626−67, and GRO J1008−57, which were in the subcritical state, or at least not confidently in the supercritical state, during the polarization measurements. Our results suggest that the relatively low PF seen in accreting pulsars cannot be attributed to the source not being in the supercritical state, but could be a general feature.
Lightning: An X-Ray to Submillimeter Galaxy SED-fitting Code with Physically Motivated Stellar, Dust, and AGN Models
Authors: Doore Keith , Monson Erik B. , Eufrasio Rafael T. , Lehmer Bret D. , Garofali Kristen , Basu-Zych Antara 
Published: June 2023

Abstract
We present an updated version of Lightning, a galaxy spectral energy distribution (SED) fitting code that can model X-ray to submillimeter observations. The models in Lightning include the options to contain contributions from stellar populations, dust attenuation and emission, and active galactic nuclei (AGNs). X-ray emission, when utilized, can be modeled as originating from stellar compact binary populations with the option to include emission from AGNs. We have also included a variety of algorithms to fit the models to observations and sample parameter posteriors; these include adaptive Markov Chain Monte Carlo (MCMC), affine-invariant MCMC, and Levenberg–Marquardt gradient-descent (MPFIT) algorithms. To demonstrate some of the capabilities of Lightning, we present several examples using a variety of observational data. These examples include (1) deriving the spatially resolved stellar properties of the nearby galaxy M81, (2) demonstrating how X-ray emission can provide constraints on the properties of the supermassive black hole of a distant AGN, (3) exploring how to rectify the attenuation effects of inclination on the derived the star formation rate of the edge-on galaxy NGC 4631, (4) comparing the performance of Lightning to similar Bayesian SED-fitting codes when deriving physical properties of the star-forming galaxy NGC 628, and (5) comparing the derived X-ray and UV-to-IR AGN properties from Lightning and CIGALE for a distant AGN. Lightning is an open-source application developed in IDL and is available at https://github.com/rafaeleufrasio/lightning.
Formation of an Ultra Diffuse Satellite Galaxy
Authors: Reed Courtney , Samuel Jenna , Kong Hyunsu , Boylan-Kolchin Michael 
Published: June 2023

Abstract
The formation of ultra diffuse satellite galaxies (UDSGs) within Λ CDM cosmology is a key area of study in theoretical galaxy formation because current models struggle to produce low-mass galaxies with a wide variety of morphologies. We identified 16 UDSGs around 8 Milky Way-mass hosts in the FIRE-2 simulations based on their large sizes in comparison to typical satellites. We selected an analogue of the observed Milky Way UDSG Antlia II in the stellar mass range 106−6.5 M
⊙ for further study. The analogue likely underwent a tidal shock near its first pericenter passage as it came within <10 kpc of its host. The analogue galaxy subsequently experienced significant tidal stripping of its dark matter and puffing up of its stellar distribution, causing it to transform into an UDSG.
Simulating Secondary Electron and Ion Emission from the Cassini Spacecraft in Saturn’s Ionosphere
Authors: Zhang Z. , Desai R. T. , Shebanits O. , Johansson F. L. , Miyake Y. , Usui H. 
Published: June 2023

Abstract
The Cassini spacecraft’s Grand Finale flybys through Saturn’s ionosphere provided unprecedented insight into the composition and dynamics of the gas giant’s upper atmosphere and a novel and complex spacecraft–plasma interaction. In this article, we further study Cassini’s interaction with Saturn’s ionosphere using three-dimensional particle-in-cell simulations. We focus on how electrons and ions, emitted from spacecraft surfaces due to the high-velocity impact of atmospheric water molecules, could have affected the spacecraft potential and low-energy plasma measurements. The simulations show emitted electrons extend upstream along the magnetic field, and for sufficiently high emission rates, charge the spacecraft to positive potentials. The lack of accurate emission rates and characteristics, however, makes differentiation between the prominence of secondary electron emission and ionospheric charged dust populations, which induce similar charging effects, difficult for Cassini. These results provide further context for Cassini’s final measurements and highlight the need for future laboratory studies to support high-velocity flyby missions through planetary and cometary ionospheres.
Biodiversity atlas of the special area of conservation Montesinho/Nogueira, Portugal
Authors: Garcia Nuno , Campos João , Silva Daniel , Alírio João , Duarte Lia , Arenas-Castro Salvador , Pôças Isabel , Loureiro Armando , Teodoro Ana , Sillero Neftalí 
Published: June 2023

The special area of conservation Montesinho/Nogueira (PTCON0002) is a key area for conserving biodiversity in the Iberian Peninsula. Covering an area of approximately 1081 km² in the northeast of Portugal mainland, the PTCON0002 is home to a wide range of biodiversity, including several endemic and endangered species, and priority habitats. Despite its ecological significance and importance for conservation, there is a lack of publicly available biodiversity data, which urges the need to create a comprehensive and up-to-date biodiversity dataset for the PTCON0002.
To bridge the knowledge gap on biodiversity in PTCON0002, we undertook a thorough data collection process, such as species occurrence records and conservation status information at regional (Portugal) and European levels, from multiple sources. We collected and compiled this information for PTCON0002 resulting in a total of 31 871 records with 1 312 documented species. In addition, we developed an easy-to-navigate web-based geographic information system (Web GIS). In this article, we present an in-depth report on the process of compiling and preparing data, as well as the development and design of our Web GIS to increase awareness and enhance understanding of the importance of preserving biodiversity in PTCON0002.
La protection des enfants par la Cour européenne des droits de l’homme
Authors: Gouttenoire Adeline 
Published: June 2023

La jurisprudence de la Cour européenne des droits de l’homme qui concerne les enfants, au sens de personnes mineures, est particulièrement riche et fournie. La Cour se fonde sur leur vulnérabilité et leurs besoins spécifiques leur assurer une protection renforcée et spécifique à partir du texte de la Convention interprétée à la lumière de la Convention internationale des droits de l’enfant. Cette protection, grâce aux outils mis en œuvre par la Cour, se caractérise par un contenu substantiel qui fait de la Convention européenne une garantie particulièrement efficace des droits de l’enfant. La richesse de la protection des enfants s’explique sur le plan procédural, par un accès facilité des mineurs à la Cour européenne et sur le plan substantiel par la mise en œuvre au profit des enfants du dynamisme interprétatif de cette dernière. Sont en effet mobilisés au profit des enfants, l’effet horizontal de la Convention et son interprétation évolutive ; la Cour impose également aux États des obligations positives particulières à leur profit. Pour ce qui est du contenu de la protection des enfants, celle-ci se fonde largement sur le principe de primauté de l’intérêt des enfants que la Cour européenne a intégré à sa jurisprudence. La juge de Strasbourg a en outre consacré un certain nombre de droits spécifiques au bénéfice de l’enfant tels que le droit d’être protégé contre les violences intra-familiales, le droit à la reconnaissance juridique de sa filiation – élément essentiel de l’identité –, le droit d’être entendu dans les procédures le concernant ou encore le droit du mineur délinquant à une juridiction spécialisée.