bluuebunny/crossref_metadata_2025_split huggingface dataset:
Результати реалізації підготовчого етапу дослідницького проєкту «Допрофільна позашкільна освіта учнів закладів загальної середньої освіти»
Authors: Первушевська Ірина , Давидюк Наталія 
Published: January 2025

У статті представлено результати підготовчого етапу дослідницького проєкту «Допрофільна позашкільна освіта учнів закладів загальної середньої освіти», що спільно реалізується Рівненським Палацом дітей та молоді й Рівненським ліцеєм № 1 Рівненської міської ради. Зміст проєкту розкривається на основі низки реалізованих завдань, що є одночасно й етапами його підготовчого періоду. Підґрунтям проєкту став багаторічний досвід інноваційної діяльності Рівненського Палацу дітей та молоді, результатом якого є розроблена й апробована багаторівнева система (модель) допрофесійної підготовки і початкової професійної освіти.
Освітній нетворкінг дозволив започаткувати освітнє партнерство між закладами загальної середньої та позашкільної освіти завдяки відповідній мережевій взаємодії. Формування напрямів допрофільної позашкільної освіти здійснювалося на основі діагностування здобувачів освіти, виявлення їхніх схильностей та задатків до того чи іншого виду професійної діяльності, запропонованого програмно-ресурсного забезпечення профільних шкіл і спеціалізованих центрів Рівненського Палацу дітей та молоді. Розроблений алгоритм взаємодії двох закладів освіти дозволив створити оптимальні умови для навчання учнів Рівненського ліцею № 1, які обрали еколого-біологічний, економічний, інформаційно-технічний та театральний профілі. Зворотний зв’язок, отриманий від учасників проєкту – педагогічних працівників, учнів та їхніх батьків – дозволяє зробити висновок щодо ефективності початкового етапу проєкту, а також змін, що відбулися в мотиваційній сфері учнів, їхньому ставленні до навчання, усвідомленості вибору профілю.
Telaah Terhadap Kitab Al-Luma’ Fī Asbāb Al-Wurūd Al-Hadīth Karya Imam Jalaluddin Al-Suyuthi
Authors: Hasyim Muhammad Sulaiman , Zainnurrofiq Muhammad , Faqih Muhammad Abdurrohman 
Published: January 2025

This article wants to examine in depth and examine the book Al-Luma’ fī Asbāb al-Wurūd al-Hadīth by a famous scholar named Al-Hafidz Imam Jalaluddin al-Suyuthi. In this paper, the author uses library research methods by referring to the main work of Imam Jalaluddin al-Suyuthi, namely the book Al-Luma’ fī Asbāb al-Wurūd al-Hadīth which is one of the books in the study of asbabul wurud hadith which is very phenomenal and is often used as a reference for looking for asbabul wurud from a hadith. The results of this research show that the book Al-Luma’ fī Asbāb al-Wurūd al-Hadīth is a book of asbabul wurud hadith which has its own method and system in collecting and mentioning each hadith and its asbabul wurud. The book Al-Luma’ fī Asbāb al-Wurūd al-Hadīth also refers to 35 reference sources and contains a lot of additional information regarding asbabul wurud hadith which is not found in other books. This makes the existence of this book by Imam Jalaluddin al-Suyuthi greatly contribute to hadith scholarship, especially the study of asbabul wurud hadith.
Analisis Implementasi Keputusan Direktur Jenderal Bimas Islam Nomor 379 Tahun 2018 Tentang Bimbingan Pranikah Di Kantor Urusan Agama Kecamatan Sangkapura
Authors: Halim Abdul , Zaki Zainul 
Published: January 2025

In the Decree of the Director General of Islamic Guidance Number 379 of 2018 concerning instructions for implementing pre-marital marriage guidance for prospective brides and grooms, it is emphasized that this guidance is a real seriousness from the government in creating a strong and harmonious family so as to produce happiness for the prospective bride and groom. This decision is also implemented simultaneously in all provinces of Indonesia, implemented by the district or city Ministry of Religion, District Religious Affairs Office (KUA) or other institutions. The discussion in this research is pre-marital guidance at the Sangkapura District Religious Affairs Office, broken down into 2 research focuses, namely: (1) How is the implementation of pre-marital guidance for prospective brides and grooms at the Sangkapura District KUA? 2) What are the obstacles in implementing the Decree of the Director General of Islamic Community Guidance Number 379 of 2018 in the KUA of Sangkapura District? The research objectives are (1) to determine the implementation of pre-marital guidance for prospective brides and grooms in the KUA of Sangkapura District. (2) mention what are the obstacles in implementing the Decree of the Director General of Islamic Community Guidance Number 379 of 2018 in the KUA of Sangkapura District. The research method uses an empirically based qualitative approach. Data collection uses interview, observation and documentation methods. Data is analyzed by organizing the data, arranging it into patterns, choosing what is important to examine, and making conclusions. Data validation uses observation extension, increased persistence, and triangulation. The results of this research show that: (1) Premarital guidance at the KUA Sangkapura District consists of two guidance models, namely (a) face-to-face guidance by bringing in speakers from the Gresik Ministry of Religion and (b) independent guidance carried out by the KUA. (2) Obstacles in implementing premarital guidance according to the Decree of the Director General of Islamic Guidance Number 379 of 2018 consist of two obstacle factors, namely: the organizer factor and the bride and groom factor.
The Age and Source of Be and U Mineralization from the Baiyanghe Deposit
Authors: Jacques Issac J. , Fayek Mostafa 
Published: January 2025

Abstract
Critical elements (e.g., Li, Be, U) are essential for energy, technology, and national defense applications. Therefore, it is important to develop effective exploration strategies, understand how these deposits form, and develop genetic models for these deposits. The Baiyanghe deposit, China, is the largest Be-U deposit in Asia. Despite several recent studies, the age and sources of mineralization remain controversial. Petrographic and geochemical analysis of host rocks indicate that the Yangzhuang rhyolite is underlain by an evolved alkali rhyolite tuff, rhyolitic to dacitic tuff, andesitic tuff, and basaltic tuff units. We used the Sm-Nd and Sr isotopic compositions of ore-bearing and barren fluorite and the U-Pb isotopic compositions of uranophane-beta to date the Be and U mineralization precisely. Our results indicate that two stages of Be mineralization occurred at 311 ± 12 and 261 ± 3 Ma. Whole rock geochemical data suggest the Yangzhuang rhyolite (YR) and the felsic tuff members of the underlying Tarbagatay Group are the sources of Be and U. The Sr and Nd isotope data suggest the first stage of Be mineralization formed from Yangzhuang rhyolite-derived fluids while mantle-derived fluids mobilized the second stage of Be mineralization. Our U-Pb geochronology indicates uranophane is associated with primary Be mineralization at 305.3 ± 1.3 Ma and reported uraninite mineralization at 246.1 ± 1.3 Ma due to supergene processes.
Kreiterite, CsLi2Fe+3(Si4O10)F2, a New Cesium Mica from the Darai-Pioz Alkaline Massif, Tajikistan
Authors: Agakhanov Atali A. , Pautov Leonid A. , Pekov Igor V. , Karpenko Vladimir Yu. , Siidra Oleg I. , Sokolova Elena , Hawthorne Frank C. , Faiziev Abdulkhak R. , Kasatkin Anatoly V. , Kulikova Inna M. , Muftakhov Vyacheslav A. 
Published: January 2025

Abstract
Kreiterite, CsLi2Fe+3(Si4O10)F2, a new cesium trioctahedral mica was discovered in the Darai-Pioz alkaline massif (Tajikistan). It is named after the Russian geologist, Prof. Vladimir Mikhailovich Kreiter (1897–1966). Kreiterite occurs as lamellar grains or flakes up to 0.2 mm across, irregular in shape and usually slightly deformed, in quartz-pectolite aggregates within so-called “quartz lumps”, the rocks consisting mainly of granular quartz. The mineral is colorless and transparent with vitreous luster. Mohs hardness is 2½, Dmeas. is 3.33(2) g/cm3, and Dcalc. is 3.342 g/cm3. The new mineral is optically biaxial (−) with α = 1.596(2), β = 1.605(2), γ = 1.607(2), 2V(calc) = −50°. It is monoclinic, space group C2/m, C2, or Cm (polytype 1M), a = 5.240(2) Å, b = 9.054(4) Å, c = 10.767(4) Å, β = 99.58(4)°, V = 503.4(6) Å3, and Z = 2. The strongest lines in the powder diffraction pattern are (d Å, I %, hkl): 4.49, 31, (1 1 0); 3.94, 31, (1 1 1); 3.70, 47, ( 1 2), ( 2); 3.45, 36, (0 2 2); 3.00, 34, ( 1 ), ( 3); 2.652, 17, (0 0 4); 2.610, 72, ( 0 1), (1 3 0), ( 3 0); 2.583, 100, (2 0 0), ( 3 1); 2.241, 38, (2 2 0); 2.190, 67, ( 3 3). Chemical analysis by electron microprobe and SIMS (for H2O and Li2O) gave SiO2 47.37, TiO2 0.99, Al2O3 0.29, MgO 0.40, Fe2O3 13.18, ZnO 0.12, K2O 0.02, Cs2O 27.37, Li2O 5.90, H2O 1.28, F 4.77, −O=F −2.01, total 99.68 wt.% The empirical formula, based on 12 (O+F), is Cs0.99Li2.01(Fe3+0.84Ti0.06Mg0.05Al0.03Zn0.01)Σ0.99Si4.01O10(F1.28OH0.72)Σ2. Kreiterite is a ferric-iron analogue of sokolovaite and gorbunovite and the lithium ferric-iron analogue of garmite.
Enfermedad de Moyamoya, como Causa Rara de un Evento Cerebrovascular Isquémico Pediátrico. Reporte de Caso
Authors: Mariscal García Raisa Stefanía , Guillermo Cornejo Andrea Priscila , Barahona Moreta Cristina Isabel , Cruz Barrera Aura Gabriela , García Ordóñez Galo Fabián 
Published: January 2025

Antecedentes La enfermedad de Moyamoya (EMm), es una arteriopatía estenooclusiva progresiva, que afecta la arteria carótida interna intracraneal distal y sus ramas principales, con formación de vasculatura colateral compensatoria y es responsable de hasta el 10% de los accidentes cerebrovasculares (ACV) y ataques isquémicos transitorios en la edad pediatríca. Metodología: Caso clínico: Masculino de 13 años, sin antecedentes clínico quirúrgicos de importancia, ingresa por presentar cuadro neurológico caracterizado por alteraciones en hemicuperpo derecho: mioclonias, hemiparesia y hemicorea, además de cefalea holocraneana y dislalia. Se realiza AngioRM Simple y Contrastada con evidencia de estenosis de los segmentos C6 y C7 del lado izquierdo, reducción significativa del calibre de arteria carótida izquierda y aumento en número de ramas lenticuloestriadas, compatibles con Enfermedad MoyaMoya y pequeñas imágenes sugestivas de Infarto en sustancia blanca frontal izquierda. Neurocirugía realiza una Panarteriografía con evidencia de oclusión total de arteria cerebral media izquierda y presencia de colateralidad a través de arteria cerebral anterior y posterior izquierda. Tratamiento: No quirúrgico y manejo multidisciplinario. Estancia hospitalaria 11 días, evolución favorable. Diagnóstico Final: Enfermedad de Moyamoya Grado II Suzuki más Hemicorea Derecha secundaria a Accidente Cerebro Vascular Isquémico. Tratamiento: enoxaparina y ácido valproico. Seguimiento por neurocirugía para valorar revascularización, con mejoría de cuadro neurológico. Conclusiones: La EMm, es una entidad rara en la población general y más rara en la población pediátrica, debe ser considerada como una causa primaria en ACV infantil, el tratamiento clínico puede mejorar los síntomas, el tratamiento final es la revascularización.
Alteraciones de la Funcionalidad Familiar de Pacientes con Secuelas de Evento Vascular Cerebral de una Unidad de Primer Nivel
Authors: Arrazola Cortes Andres , Reyes Pintor Arlette Juliette 
Published: January 2025

La enfermedad vascular cerebral (EVC) es una patología que se presenta aproximadamente en 230 casos y una mortalidad de 28.3 por cada 100.000 habitantes, en mayores de 65 años en hombres y 50 años en mujeres. Los supervivientes, presentan complicaciones en su desempeño físico, psicológico y social. Lo que deteriora el ambiente familiar en su función y dinámica hasta en un 55% de los casos. Objetivo: Determinar las alteraciones de la Funcionalidad Familiar de pacientes con secuelas de EVC de una Unidad de primer nivel. Material y métodos: Estudio transversal, observacional y analítico. Se incluyeron a pacientes con diagnóstico de EVC pertenecientes a la UMF 61 durante el periodo comprendido del 01 de enero del 2018 al 31 de diciembre del 2022. Se integró de un total de 54 familias, solo se logró entrevistar a 23 familias con la encuesta FF-SIL. El análisis estadístico se realizó con prueba de X2, estadísticamente significativas con valor de p ≤0.05. Resultados: Se identificó que más del 50% de los pacientes y de los familiares encuestados presentaron una familia funcional. También se identificó que de los demás factores demográficos la ocupación presento una P=0.31 mientras que en los familiares se encontró una P=0.50.
Eighteen Exoplanet Host Stars from the NPOI Data Archive
Authors: Baines Ellyn K. , Jones Jeremy , Clark James H. , Schmitt Henrique R. , Stone Jordan M. 
Published: January 2025

Abstract
During the course of publishing angular diameters from the Navy Precision Optical Interferometer data archive, we found we had data on 17 confirmed exoplanet host stars and 1 exoplanet candidate (HD 20902/α Per). Here, we update our previously published stellar radii with more precise Gaia parallaxes when available, and use our radius and effective temperature measurements to fit each star's mass and age using MIST models. The mass changed by more than 10% for 9 of the 18 stars. Combining our updated masses, radii, and temperatures, we present refined planetary masses as well as habitable zone calculations.
High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions
Authors: Kajikiya Yuto , Namekata Kosuke , Notsu Yuta , Maehara Hiroyuki , Sato Bunei , Nogami Daisaku 
Published: January 2025

Abstract
M dwarfs show frequent flares and associated coronal mass ejections (CMEs) may significantly impact close-in habitable planets. M dwarf flares sometimes show blue/red asymmetries in the Hα line profile, suggesting prominence eruptions as an early stage of CMEs. However, their high-time-cadence observations are limited. We conducted spectroscopic monitoring observations of the active M dwarf YZ Canis Minoris with an ∼1 minute time cadence using the Seimei telescope, simultaneously with the optical photometric observations by Transiting Exoplanet Survey Satellite. We detected 27 Hα flares with Hα energies ranging from 1.7 × 1029 to 3.8 × 1032 erg and durations from 8 to 319 minutes. Among them, we identified three blue asymmetry and five red asymmetry events based on criteria using the Bayesian information criterion. The maximum velocity of the blueshifted and redshifted components ranges from 200 to 450 km s−1 and 190 to 400 km s−1, respectively. The duration and time evolution show variety, and in particular, we discovered rapid, short-duration blue/red asymmetry events with the duration of 6–8 minutes. Among the eight blue/red asymmetry events, two blue and one red asymmetry events are interpreted as prominence eruptions because of their fast velocity and time evolution. Based on this interpretation, the lower limit of occurrence frequency of prominence eruptions can be estimated to be ∼1.1 events per day. Our discovery of short-duration events suggests that previous studies with low time cadence may have missed these events, potentially leading to an underestimation of the occurrence frequency of prominence eruptions/CMEs.
Evolution of Magnetic Reconnection in an Electron-scale Current Sheet
Authors: Guan Yundan , Lu Quanming , Lu San , Wang Rongsheng 
Published: January 2025

Abstract
Recently, a new type of magnetic reconnection, electron-only reconnection—where there is no obvious ion flow and heating—has been observed in various plasma environments. Previous kinetic simulations have shown that electron-only reconnection is a precursor of standard reconnection. In this paper, by performing a 2.5-dimensional particle-in-cell simulation, we investigate the evolution of electron-only magnetic reconnection to standard magnetic reconnection in a current sheet, whose initial width is of the electron inertial length. In the electron-only reconnection stage, electron outflow produces the electron-scale

B

z

pileup, and ions are slightly accelerated in the outflow direction by the Hall electric field force. As the reconnection electric field expands and

B

z

is piled up to the ion scale, ions start to be further accelerated inside the ion diffusion region and reflected by the

B

z

to the outflow direction. With

B

z

pileup as the bond, ions gradually transit from being accelerated by the Hall electric field to being coupled in reconnection by the Lorentz force.
Most Super-Earths Have Less Than 3% Water
Authors: Rogers James G. , Dorn Caroline , Aditya Raj Vivasvaan , Schlichting Hilke E. , Young Edward D. 
Published: January 2025

Abstract
Super-Earths are highly irradiated, small planets with bulk densities approximately consistent with Earth. We construct combined interior atmosphere models of super-Earths that trace the partitioning of water throughout a planet, including an iron-rich core, silicate-rich mantle, and steam atmosphere. We compare these models with exoplanet observations to infer a 1σ upper limit on the total water mass fraction of ≲3% at the population level. We consider end-member scenarios that may change this value, including the efficiency of mantle outgassing, escape of high mean molecular weight atmospheres, and increased iron core mass fractions. Although our constraints are agnostic as to the origin of water, we show that our upper limits are consistent with its production via chemical reactions of primordial hydrogen-dominated atmospheres with magma oceans. This mechanism has also been hypothesised to explain Earth's water content, possibly pointing to a unified channel for the origins of water on small terrestrial planets.
A Wideband Chemical Survey of Massive Star-forming Regions at Subarcsecond Resolution with the Submillimeter Array
Authors: Law Charles J. , Zhang Qizhou , Frommer Arielle C. , Öberg Karin I. , Galván-Madrid Roberto , Keto Eric , Liu Hauyu Baobab , Ho Paul T. P. , Izquierdo Andrés F. , Cleeves L. Ilsedore 
Published: January 2025

Abstract
Massive star-forming regions exhibit a rich chemistry with complex gas distributions, especially on small scales. While surveys have yielded constraints on typical gas conditions, they often have coarse spatial resolution and limited bandwidths. Thus, to establish an interpretative framework for these efforts, detailed observations that simultaneously provide high sensitivity, spatial resolution, and large bandwidths for a subset of diverse sources are needed. Here, we present wide-band (≈32 GHz) Submillimeter Array (SMA) observations of four high-mass star-forming regions (G28.20-0.05, G20.08-0.14 N, G35.58-0.03, and W33 Main) at subarcsecond resolution, where we detect and spatially resolve hundreds of lines from over 60 molecules, including many complex organic molecules (COMs). The chemical richness of our sample is consistent with an evolutionary sequence from the line-rich hot cores and hypercompact H ii regions of G28.20-0.05 and G20.08-0.14 N to the more chemically modest ultracompact H ii regions in G35.58-0.03, followed by the molecule-poor H ii region W33 Main. We detect lines across a range of excitation conditions (E
u ≈ 20 to ≳800 K) and from numerous isotopologues, which enables robust estimates of gas properties. We derive nearly constant COM column density ratios that agree with literature values in other low- and high-mass protostellar cores, supporting the idea that COM abundances are set during the pre-stellar phase. In all regions, we identify spatial offsets among different molecular families, due to a combination of source physical structure and chemistry. In particular, we find potential evidence of carbon grain sublimation in G28.20-0.05 and identify an elemental oxygen gradient and rich sulfur chemistry in G35.58-0.03. Overall, these results demonstrate that the SMA's wide bandwidth is a powerful tool to untangle the complex molecular gas structures associated with massive star formation.
A Multiple-detection-heads Machine Learning Algorithm for Detecting White Dwarfs
Authors: Zhang Jiangchuan , Bu Yude , Zhang Mengmeng , Xie Duo , Yi Zhenping 
Published: January 2025

Abstract
White dwarfs (WDs) are the ultimate stage for approximately 97% of stars in the Milky Way and are crucial for studying stellar evolution and galaxy structure. Due to their small size and low luminosity, WDs are not easily observable. Traditional search methods mostly rely on analyzing photometric parameters, which need high-quality data. In recent years, machine learning has played a significant role in astronomical data mining, due to its speed, real time, and precision. However, we have identified two common issues. On the one hand, many studies are based on high-quality spectral data, while a large amount of image data remain underutilized. On the other hand, existing astronomical algorithms are essentially classification algorithms, with sample incompleteness being a critical weakness. In our study, we propose the WD Network (WDNet) algorithm, which is a new object detection algorithm that integrates multiple advanced technologies and can directly locate WDs in images. WDNet overcomes the degradation issue of WDs and detected 31,065 candidates in 80,448 images. The candidates exhibit a wide range of types, including DA, DB, DC, DQ, and DZ, with surface gravity within 7.8 dex ∼ 8.4 dex, effective temperatures within 10,000 K ∼ 56,000 K, colors within −1 < u − g < 1 and −0.8 < g − r < 0.4, and reduced proper motion within 20∼35 mag. In the future, WDNet will conduct large-scale searches using the Chinese Space Station Telescope and Sloan Digital Sky Survey V.
Stellar Contamination Correction Using Back-to-back Transits of TRAPPIST-1 b and c
Authors: Rathcke Alexander D. , Buchhave Lars A. , de Wit Julien , Rackham Benjamin V. , August Prune C. , Diamond-Lowe Hannah , MendonÇa João M. , Bello-Arufe Aaron , López-Morales Mercedes , Kitzmann Daniel , Heng Kevin 
Published: January 2025

Abstract
Stellar surface heterogeneities, such as spots and faculae, often contaminate exoplanet transit spectra, hindering precise atmospheric characterization. We demonstrate a novel, epoch-based, model-independent method to mitigate stellar contamination, applicable to multiplanet systems with at least one airless planet. We apply this method using quasi-simultaneous transits of TRAPPIST-1 b and TRAPPIST-1 c observed on 2024 July 9, with JWST/NIRSpec PRISM. These two planets, with nearly identical radii and impact parameters, are likely to either be bare rocks or possess thin, low-pressure atmospheres, making them ideal candidates for this technique, as variations in their transit spectra would be primarily attributed to stellar activity. Our observations reveal their transit spectra exhibit consistent features, indicating similar levels of stellar contamination. We use TRAPPIST-1 b to correct the transit spectrum of TRAPPIST-1 c, achieving a 2.5 × reduction in stellar contamination at shorter wavelengths. At longer wavelengths, lower signal-to-noise ratio prevents clear detection of contamination or full assessment of mitigation. Still, out-of-transit analysis reveals variations across the spectrum, suggesting contamination extends into the longer wavelengths. Based on the success of the correction at shorter wavelengths, we argue that contamination is also reduced at longer wavelengths to a similar extent. This shifts the challenge of detecting atmospheric features to a predominantly white noise issue, which can be addressed by stacking observations. This method enables epoch-specific stellar contamination corrections, allowing coaddition of planetary spectra for reliable searches of secondary atmospheres with signals of 60–250 ppm. Additionally, we identify small-scale cold (∼2000 K) and warm (∼2600 K) regions almost uniformly distributed on TRAPPIST-1, with overall covering fractions varying by ∼0.1% per hour.