bluuebunny/crossref_metadata_2025_split huggingface dataset:
The Hungarian Nippon Society
Authors: Farkas Ildikó Mária 
Published: November 2022

The Hungarian Nippon Society was founded in 1924, with the aim of building and developing Hungarian–Japanese relations, popularising Japan and Japanese culture in Hungary, and encouraging research on Japan. The society organised public lectures on Japan and Japanese culture and art exhibitions and social events connected to Japanese culture, and through these activities the society was the most important organiser and promoter of Japanese culture and art in Hungary between the two world wars. This society was the first (and for a long time, until the foundation of the Hungarian Japanese Friendship Society in 1987, the only) association in Hungary to focus solely on Japan and Japanese culture. This study summarises the most important issues related to the Nippon Society, with the aim of placing its history and activity in the broader historic and ideological context of its time. Examining the history of the Hungarian Nippon Society can provide us a more nuanced picture about how and why Japan’s image changed during the first half of the 20th century in a Central European country that had different images and concepts about the East and thus a different approach than Western European societies had. Moreover, this case of a primarily cultural association in a politically difficult era can show how different cultural and intellectual thoughts and theories can be affected by identity issues and by contemporary politics, political thinking, and international situations.
A Tale of Two Potalakas: Intercultural Relations Between China and Korea Examined Through Maritime Buddhism
Authors: Vörös Erika Erzsébet 
Published: November 2022

Several places around the world have been identified as Potalaka, which was originally thought to be located in South India. The most well-known among these places are Mount Putuo in China and Naksan Temple in Korea. Geographically speaking, Korea is connected to China by sea, which acted as a source of cultural and material resources for a long time. For this reason, throughout history the sea became the stage of cultural exchanges between these two regions. The sea was the channel through which faith in Avalokiteśvara entered Korea from China, and where the traditions of Buddhism merged with beliefs in indigenous sea gods. The present paper focuses on the cultural exchanges between Korea and China, with special emphasis on the role that the sea played in this process examined through the faith in Potalaka.
The Early Solar System Abundance of Iron-60: New Constraints from Chondritic Silicates
Authors: Kodolányi János , Hoppe Peter , Vollmer Christian , Berndt Jasper , Müller Maren 
Published: November 2022

Abstract
The abundance of iron-60 in the early solar system is important for planetary evolution models, and has been hotly debated. To put further constraints on the initial 60Fe/56Fe ratio of the solar system, here we present new iron-nickel isotope data, measured in situ by NanoSIMS, for 14 silicate chondrules from three carbonaceous and three unequilibrated ordinary chondrites. NanoSIMS measurements were performed at high spatial resolution (200–300 nm primary beam diameter), to avoid inclusion of unwanted phases in the analysis volume. The average initial 60Fe/56Fe ratios that can be estimated from our pooled chondrule data are 2.1 (±1.3) × 10−7 and 0.8 (±1.0) × 10−7 for carbonaceous and ordinary chondrites, respectively (1σ uncertainties). The estimated average initial 60Fe/56Fe ratio of all analyzed chondrules is 1.0 (±0.7) × 10−7. These results are inconsistent with initial 60Fe/56Fe ratios >2.4 × 10−7 (2σ upper limit of our entire data set) reported in the literature for some chondrule silicates based on in situ isotope data, and agree better with our previously published in situ data on chondritic troilites (0.10 ± 0.15 × 10−7), as well as with 60Fe/56Fe ratios estimated from isotope data of bulk meteorites and chondrules (0.10–0.75 × 10−7). Our isotope data hint at a possible difference between the initial 60Fe/56Fe ratios of the early solar system’s two major isotope reservoirs, with the carbonaceous chondritic reservoir having higher iron-60 abundance than the non-carbonaceous reservoir. Nevertheless, in light of similar hints in the literature, this possibility deserves further investigation.
High-energy Photon Opacity in the Twisted Magnetospheres of Magnetars
Authors: Hu Kun , Baring Matthew G. , Harding Alice K. , Wadiasingh Zorawar 
Published: November 2022

Abstract
Magnetars are neutron stars characterized by strong surface magnetic fields generally exceeding the quantum critical value of 44.1 TG. High-energy photons propagating in their magnetospheres can be attenuated by QED processes like photon splitting and magnetic pair creation. In this paper, we compute the opacities due to photon splitting and pair creation by photons emitted anywhere in the magnetosphere of a magnetar. Axisymmetric, twisted dipole field configurations embedded in the Schwarzschild metric are treated. The paper computes the maximum energies for photon transparency that permit propagation to infinity in curved spacetime. Special emphasis is given to cases where photons are generated along magnetic field loops and/or in polar regions; these cases directly relate to resonant inverse Compton scattering models for the hard X-ray emission from magnetars and Comptonized soft gamma-ray emission from giant flares. We find that increases in magnetospheric twists raise or lower photon opacities, depending on both the emission locale and the competition between field-line straightening and field strength enhancement. Consequently, given the implicit spectral transparency of hard X-ray bursts and persistent “tail” emission of magnetars, photon splitting considerations constrain their emission region locales and the twist angle of the magnetosphere; these constraints can be probed by future soft gamma-ray telescopes such as COSI and AMEGO. The inclusion of twists generally increases the opaque volume of pair creation by photons above its threshold, except when photons are emitted in polar regions and approximately parallel to the field.
A Multiscale Picture of the Magnetic Field and Gravity from a Large-scale Filamentary Envelope to Core-accreting Dust Lanes in the High-mass Star-forming Region W51
Authors: Koch Patrick M. , Tang Ya-Wen , Ho Paul T. P. , Hsieh Pei-Ying , Wang Jia-Wei , Yen Hsi-Wei , Duarte-Cabral Ana , Peretto Nicolas , Su Yu-Nung 
Published: November 2022

Abstract
We present 230 GHz continuum polarization observations with the Atacama Large Millimeter/Submillimeter Array at a resolution of 0.″1 (∼540 au) in the high-mass star-forming regions W51 e2 and e8. These observations resolve a network of core-connecting dust lanes, marking a departure from earlier coarser, more spherical continuum structures. At the same time, the cores do not appear to fragment further. Polarized dust emission is clearly detected. The inferred magnetic field orientations are prevailingly parallel to dust lanes. This key structural feature is analyzed together with the local gravitational vector field. The direction of local gravity is found to typically align with dust lanes. With these findings, we derive a stability criterion that defines a maximum magnetic field strength that can be overcome by an observed magnetic field–gravity configuration. Equivalently, this defines a minimum field strength that can stabilize dust lanes against a radial collapse. We find that the detected dust lanes in W51 e2 and e8 are stable, hence possibly making them a fundamental component in the accretion onto central sources, providing support for massive star formation models without the need of large accretion disks. When comparing to coarser resolutions, covering the scales of envelope, global, and local collapse, we find recurring similarities in the magnetic field structures and their corresponding gravitational vector fields. These self-similar structures point at a multiscale collapse-within-collapse scenario until finally the scale of core-accreting dust lanes is reached where gravity is entraining the magnetic field and aligning it with the dust lanes.
Orbital Decay of Double White Dwarfs: Beyond Gravitational-wave Radiation Effects
Authors: Carvalho G. A. , Anjos R. C. dos , Coelho J. G. , Lobato R. V. , Malheiro M. , Marinho R. M. , Rodriguez J. F. , Rueda J. A. , Ruffini R. 
Published: November 2022

Abstract
The traditional description of the orbital evolution of compact-object binaries, like double white dwarfs (DWDs), assumes that the system is driven only by gravitational-wave (GW) radiation. However, the high magnetic fields with intensities of up to gigagausses measured in WDs alert a potential role of the electromagnetic (EM) emission in the evolution of DWDs. We evaluate the orbital dynamics of DWDs under the effects of GW radiation, tidal synchronization, and EM emission by a unipolar inductor generated by the magnetic primary and the relative motion of the nonmagnetic secondary. We show that the EM emission can affect the orbital dynamics for magnetic fields larger than megagausses. We applied the model to two known DWDs, SDSS J0651+2844 and ZTF J1539+5027, for which the GW radiation alone does not fully account for the measured orbital decay rate. We obtain upper limits to the primary’s magnetic field strength, over which the EM emission causes an orbital decay faster than observed. The contribution of tidal locking and the EM emission is comparable, and together they can contribute up to 20% to the measured orbital decay rate. We show that the gravitational waveform for a DWD modeled as purely driven by GWs and including tidal interactions and EM emission can have large relative dephasing detectable in the mHz regime of frequencies relevant for space-based detectors like LISA. Therefore, including physics besides GW radiation in the waveform templates is essential to calibrate the GW detectors using known sources, e.g., ZTF J1539+5027, and to infer binary parameters.
Dynamical Masses of the Primary Be Star and Secondary sdB Star in the Single-lined Binary κ Dra (B6 IIIe)
Authors: Klement Robert , Baade Dietrich , Rivinius Thomas , Gies Douglas R. , Wang Luqian , Labadie-Bartz Jonathan , dos Santos Pedro Ticiani , Monnier John D. , Carciofi Alex C. , Mérand Antoine , Anugu Narsireddy , Schaefer Gail H. , Bouquin Jean-Baptiste Le , Davies Claire L. , Ennis Jacob , Gardner Tyler , Kraus Stefan , Setterholm Benjamin R. , Labdon Aaron 
Published: November 2022

Abstract
Because many classical Be stars may owe their nature to mass and angular-momentum transfer in a close binary, the present masses, temperatures, and radii of their components are of high interest for comparison to stellar evolution models. Object κ Dra is a 61.5 day single-lined binary with a B6 IIIe primary. With the CHARA Array instruments MIRC/MIRC-X and MYSTIC, we detected the secondary at (approximately photospheric) flux ratios of 1.49% ± 0.10% and 1.63% ± 0.09% in the H and K band, respectively. From a large and diverse optical spectroscopic database, only the radial velocity curve of the Be star could be extracted. However, employing the parallaxes from Hipparcos and Gaia, which agree within their nominal 1σ errors, we could derive the total mass and found component masses of 3.65 ± 0.48 and 0.426 ± 0.043 M
⊙ for the Be star and the companion, respectively. Previous cross-correlation of the observed FUV spectrum with O-type subdwarf (sdO) spectral model templates had not detected a companion belonging to the hot sdO population known from ∼20 earlier-type Be stars. Guided by our full 3D orbital solution, we found a strong cross-correlation signal for a stripped subdwarf B-type companion (FUV flux ratio of 2.3% ± 0.5%), enabling the first firm characterization of such a star and making κ Dra the first mid- to late-type Be star with a directly observed subdwarf companion.
Inconspicuous Solar Polar Coronal X-Ray Jets as the Source of Conspicuous Hinode/EUV Imaging Spectrometer Doppler Outflows
Authors: Sterling Alphonse C. , Schwanitz Conrad , Harra Louise K. , Raouafi Nour E. , Panesar Navdeep K. , Moore Ronald L. 
Published: November 2022

Abstract
We examine in greater detail five events previously identified as being sources of strong transient coronal outflows in a solar polar region in Hinode/Extreme Ultraviolet (EUV) Imaging Spectrometer (EIS) Doppler data. Although relatively compact or faint and inconspicuous in Hinode/X-ray Telescope (XRT) soft-X-ray (SXR) images and in Solar Dynamics Observatory (SDO)/Atmospheric Imaging Assembly (AIA) EUV images, we find that all of these events are consistent with being faint coronal X-ray jets. The evidence for this is that the events result from eruption of minifilaments of projected sizes spanning 5000–14,000 km and with erupting velocities spanning 19–46 km s−1, which are in the range of values observed in cases of confirmed X-ray polar coronal hole jets. In SXR images, and in some EUV images, all five events show base brightenings, and faint indications of a jet spire that (in four of five cases where determinable) moves away from the brightest base brightening; these properties are common to more obvious X-ray jets. For a comparatively low-latitude event, the minifilament erupts from near (≲few arcsec) a location of near-eruption-time opposite-polarity magnetic-flux-patch convergence, which again is consistent with many observed coronal jets. Thus, although too faint to be identified as jets a priori, otherwise all five events are identical to typical coronal jets. This suggests that jets may be more numerous than recognized in previous studies, and might contribute substantially to solar wind outflow, and to the population of magnetic switchbacks observed in Parker Solar Probe (PSP) data.
Topological Modes in Stellar Oscillations
Authors: Leclerc Armand , Laibe Guillaume , Delplace Pierre , Venaille Antoine , Perez Nicolas 
Published: November 2022

Abstract
Stellar oscillations can be of topological origin. We reveal this deep and so far hidden property of stars by establishing a novel parallel between stars and topological insulators. We construct an Hermitian problem to derive the expression of the stellar acoustic–buoyant frequency S of nonradial adiabatic pulsations. A topological analysis then connects the changes of sign of the acoustic–buoyant frequency to the existence of Lamb-like waves within the star. These topological modes cross the frequency gap and behave as gravity modes at low harmonic degree ℓ and as pressure modes at high ℓ. S is found to change sign at least once in the bulk of most stellar objects, making topological modes ubiquitous across the Hertzsprung–Russell diagram. Some topological modes are also expected to be trapped in regions where the internal structure varies strongly locally.
The Nonpotentiality of Steady-state Coronal Magnetic Field Derived with Time-relaxation Magnetohydrodynamics Simulations Using Helioseismic and Magnetic Imager Three-component Magnetic Field Data
Authors: Hayashi Keiji , Wu Chin-Chun , Liou Kan 
Published: November 2022

Abstract
The steady states of the coronal magnetic field obtained with the magnetohydrodynamic (MHD) time-relaxation simulation model are examined. Our electric-field-driven model can introduce the three components of the solar surface magnetic field data maps as the boundary values of an MHD simulation, without violating the divergence-free condition of the magnetic field. The magnetic field in the simulated steady-state solar corona exhibits substantial nonpotentiality in the closed-field streamers. A few choices are allowed in our model, such as the criteria for determining whether or not the horizontal components at the weak-field region are included. The initial magnetic field configuration can be arbitrarily determined. In this work, we examined the differences between the steady states obtained with the information on the horizontal components and with several choices of the simulation setting, and compared the new steady states with those obtained without using the horizontal magnetic field components. We found that nonpotential magnetic structures in the derived steady states well correspond to the observed solar filament structures during a selected period of Carrington Rotation 2106. The difference in the steady state with different boundary treatments is found to be large. The difference caused by the initial magnetic configuration is found to be small.
The Thermonuclear X-Ray Bursts of 4U 1730–22
Authors: Bult Peter , Mancuso Giulio C. , Strohmayer Tod E. , Albayati Arianna C. , Altamirano Diego , Buisson Douglas J. K. , Chenevez Jérôme , Guillot Sebastien , Güver Tolga , Iwakiri Wataru , Jaisawal Gaurava K. , Ng Mason , Sanna Andrea , Swank Jean H. 
Published: November 2022

Abstract
We present observations of the historic transient 4U 1730–22 as observed with the Neutron Star Interior Composition Explorer (NICER). After remaining in quiescence since its 1972 discovery, this X-ray binary showed renewed outburst activity in 2021 and 2022. We observed 4U 173–22 extensively with NICER, detecting a total of 17 thermonuclear X-ray bursts. From a spectroscopic analysis, we find that these X-ray bursts can be divided into a group of bright and weak bursts. All bright bursts showed 1–2 s rise times and a photospheric radius expansion phase, while the weak bursts showed a slower ∼5 s rise with a tendency for concave shapes. From the photospheric radius expansion flux, we estimate the source distance at 6.9 ± 0.2 kpc. We consider various interpretations for our observations and suggest that they may be explained if accreted material is burning stably at the stellar equator and unstable ignition occurs at a range of higher latitudes.
Une médecine mutualiste de transformation sociale au service du mouvement ouvrier à l’épreuve du tournant « lucratif » de la mutualité
Authors: Carini-Belloni Benoît 
Published: November 2022

L’article traite de la transformation de la « médecine mutualiste » exercée dans les centres de santé d’une union mutualiste départementale des Bouches-du-Rhône sous l’effet croisé, dans la tourmente de la libéralisation, de l’injonction à la rentabilité et de la séparation des missions assurantielles et sociales des mutuelles de santé. D’inspiration cégétiste et communiste, cette mutualité ouvrière a créé, dès la fin des années 1950, un réseau de centres de santé dans tout le département à l’initiative de médecins d’orientation marxiste, engagés dans le combat social à la recherche de nouveaux modes d’exercice médical, et de militants syndicaux cgt , alliés à des représentants mutualistes et à des municipalités de gauche souhaitant investir le terrain du droit à la santé et à sa protection. À partir des années 1980, face au recul de la Sécurité sociale et sous l’effet de la réglementation européenne de la concurrence, les impératifs gestionnaires et l’alignement sur la rhétorique entrepreneuriale de la mutualité ont progressivement modifié l’éthique solidaire, la vocation sociale et l’orientation préventive des centres de santé. Cette évolution profonde a poussé la mutualité, fragilisée par une baisse de ses adhérents consécutive à la montée du chômage et de la précarité, à adopter un mode de gouvernance plus opaque et moins démocratique débouchant sur une crise interne en 2012, dont l’élément catalyseur a été le passage à la rémunération à l’acte des médecins des centres.
Bonnets rouges contre chapeaux noirs : les enjeux vestimentaires de la révolte de 1675 dans le Cap Caval
Authors: André Christophe 
Published: November 2022

En juillet 1675, dans l’actuel pays Bigouden, une assemblée de participants à la révolte dite des Bonnets Rouges décide d’envoyer des représentants devant les États de Bretagne pour y expliquer les raisons de la sédition. Les activistes prévoient de vêtir ces délégués selon un costume défini et fixé dans un écrit, le Règlement. Ce dernier existe en trois exemplaires, avec des divergences concernant la codification vestimentaire. Si les exemplaires issus des archives bretonnes évoquent un bonnet et camisole rouges et un haut-de-chausse bleu, celui qui a été retrouvé dans les archives de Colbert évoque aussi un bonnet et une camisole rouges mais prévoit des haut-de-chausses verts. L’étude des inventaires après décès et des signalements émanant des autorités judiciaires montre que le diocèse de Cornouaille s’est singularisé par une identité vestimentaire masculine composée d’un bonnet rouge, d’une camisole rouge et de hauts-de-chausses bleus-violets. Ces derniers commencent toutefois à être concurrencés par des vêtements à connotation citadine. La mise à l’écart de ces effets d’un genre nouveau d’une part et la remise à l’honneur du costume diocésain d’autre part permettent de comprendre la motivation des insurgés : celle d’un retour utopique à un idéal communautaire.
Les réseaux aristocratiques de la Bretagne septentrionale au prisme des enquêtes royales de 1235
Authors: Launay Vincent 
Published: November 2022

Entre 1231 et 1234, une guerre entrecoupée de deux trêves oppose une large partie de l’aristocratie bretonne ralliée au roi de France, au duc Pierre de Dreux soutenu par le roi d’Angleterre Henri III. Abandonné par ce dernier, ce n’est qu’en novembre 1234 qu’il se soumet au roi Louis IX. L’année suivante, celui-ci octroie à ses soutiens de Bretagne septentrionale une série de neuf enquêtes contentieuses dans lesquelles les dommages qu’ils ont subis sont recensés. Les procès-verbaux établis par les enquêteurs permettent d’analyser avec précision les réseaux où gravitent ces nobles et ces établissements ecclésiastiques. Appuyés par d’autres sources diplomatiques, ils révèlent un paysage aristocratique exclusivement masculin et scindé entre Bretagne occidentale et Bretagne orientale. Très hiérarchisé, il est caractérisé par trois types de liens qui, parfois, s’entremêlent : des liens de parenté, des liens féodaux-vassaliques et des liens d’amicitia spirituelle.