bluuebunny/crossref_metadata_2025_split huggingface dataset:
Compound word as an element of a word-formation system Russian and Chinese languages: comparative analysis
Authors: Ян Тяньжуй 
Published: November 2023

Статья посвящена сопоставительному анализу сложных слов в словообразовательной системе русского и китайского языков. В статье рассматриваются сходства и различия сложных слов в обоих языках. Сравнивая сложные слова двух языков, мы обнаруживаем, что, несмотря на то что русский и китайский языки являются разнотипными, существуют определенные сходства и различия в морфемном статусе, способах образования сложных слов и словосочетаний. Китайские ученые считают, что сложные слова, как правило, образуются от словосочетаний.
This article is devoted to the comparative analysis of complex words in the word formation systems of Russian and Chinese languages. This article discusses the similarities and differences of compound words in both languages. Comparing the complex words of the two languages, we find that although Russian and Chinese belong to two heterogeneous languages, there are certain similarities in terms of morpheme status, the way compound words are formed, and their relationship to phrases. Chinese scholars generally believe that compound words come from phrases.
THE CONCEPT OF A «COMMUNICATIVE SITUATION» ON THE EXAMPLE OF A REQUEST SITUATION
Authors: Амир Кушеш Закариа 
Published: November 2023

В данной статье рассматривается понятие коммуникативной ситуации на примере коммуникативной ситуации просьбы. Анализируется значение побудительного речевого акта, его семантические классификации, способы формальных реализаций акта просьбы в русском языке. Коммуникативная ситуация речевого акта просьбы включает в себя единицы, маркирующие данный речевой акт: вводные слова и ответные реплики.
This article discusses the concept of a communicative situation on the example of a communicative situation of a request. The meaning of the motivating speech act, its semantic classifications, ways of formal realizations of the act of request in the Russian language are analyzed. The communicative situation of the speech act of request includes units that mark the data of the speech act: introductory words and response remarks.
The Relevance of the Lexical Approach Implementation in Teaching Russian as a Foreign Language to the Korean Students of a Linguistic University (The example of Russian Conversation Elementary Level Classes)
Authors: Шагаева С.А. 
Published: November 2023

В статье речь идет об актуальности применения лексического подхода на уроках РКИ. Этот подход может положительно повлиять на устранение проблем, вызванных экстралингвистическими факторами и влияющих на развитие навыков речевого общения у студентов корейских вузов. Единицей обучения в рамках подхода признаются частотные лексические блоки – чанки (англ. chunks), запоминание и автоматизация воспроизведения которых повышает беглость и правильность речи. Кроме того, на уроках большое внимание уделяется аудированию, коммуникативным стратегиям, функционированию языка в разных ситуациях общения. Развитие автономности и осознанности у студентов, принцип подачи материала в рамках композиции «обзор – гипотеза – эксперимент», а также смещение роли преподавателя с позиции ментора на позицию модератора учебного процесса полностью отвечают современным образовательным требованиям.
The article is devoted to the relevance of the lexical approach implementation in teaching Russian as a foreign language to the Korean students. The approach can be useful in solving problems caused by extralinguistic factors and affect the development of the Korean students’ communicative skills. Memorizing and automatization of the chunks (multiword units) have a positive effect to the fluency and accuracy. In addition, during the lessons attention to listening, communication strategies, and functional language are given. The development of autonomy and awareness among students, the framework «observe – hypothesize – experiment», changing the teacher’s mindset from a mentor into a moderator of educational processes represents modern educational trends.
Study of Russian adjectival prefixes по-, после- and пост-, and ways of their expression in Persian Language
Authors: Хосейн Голами , Немат Салман-Асл 
Published: November 2023

В статье рассматриваются приставки по-, после- и пост-, образующие русские имена прилагательные и выражающие значение «совершившийся после того, что названо словом, которым мотивировано суффиксальное мотивирующее прилагательное». Упомянутые приставки были выбраны в качестве предмета изучения, так как они обладают синонимичными значениями, но при этом могут придавать прилагательному различные смысловые оттенки. Различение их значений и смысловых оттенков играет важную роль в понимании устной и письменной речи, а также в переводе с одного языка на другой для студентов, изучающих русский язык как иностранный. В данной работе в центре нашего внимания находится дифференциация данных приставок, определение их сходств и различий при переводе. Для этого мы приводим примеры русских приставочных прилагательных в сочетании с данными приставками, осуществляем перевод каждого примера, а потом определяем значение каждой приставки в соответствии с разрядами частей речи в персидском языке.
In this article we study prefixes по-, после- and пост-, that form Russian adjectives and denote «accomplishing or accomplished after motivating words». Mentioned prefixes were chosen as subject of study, because they possess synonymous meanings, but at the same time they can give adjective various shades of meaning. Distinguishing between their meanings and shades of their meanings plays an important role in understanding oral and written speech, and also in translating/interpreting from one language to another, for students studying Russian as a foreign language. In this paper we are focused on differentiating between these prefixes, determining their similarities and differences, during translation/interpretation. For this purpose, we will bring examples of Russian prefixal adjectives in conjunction with these prefixes, translate every example, and then determine meaning of every prefix according to parts of speech in Persian language.
Selection of educational texts in Russian for Slavic audience
Authors: Юхименко Н.В. 
Published: November 2023

В статье рассматриваются принципы отбора учебных текстов для студентов-филологов из славянских стран, изучающих русский язык. Актуальность поднимаемой проблемы связана с трудностью формирования такой компетенции, как создание оригинальных связных текстов на русском языке, и необходимостью особого подхода к учащимся с родственным русскому родным языком. Анализируются критерии отбора текстов с учетом насыщенности общеславянской лексикой (межъязыковыми полисемантами).
The article discusses the principles of selecting educational texts for students of philology from Slavic countries who study the Russian language. The relevance of the problem raised is connected with the difficulty of forming such competence as the creation of original coherent texts in Russian and the need for a special approach to students with a native Slavic language. Approaches to the selection of texts are analyzed, taking into account the saturation with common Slavic vocabulary (cross-language polysemantics).
Exploring Climate with Obliquity in a Variable-eccentricity Earth-like World
Authors: Way M. J. , Georgakarakos Nikolaos , Clune Thomas L. 
Published: November 2023

Abstract
Exploring planetary systems similar to our solar system can provide a means to explore a large range of possibly temperate climates on Earth-like worlds. Rather than run hundreds of simulations with different eccentricities at fixed obliquities, our variable-eccentricity approach provides a means to cover an incredibly large parameter space. Herein Jupiter’s orbital radius is moved substantially inward in two different scenarios, causing a forcing on Earth’s eccentricity. In one case, the eccentricity of Earth varies from 0 to 0.27 over ∼7000 yr for three different fixed obliquities (0°, 23°, and 45°). In another case, the eccentricity varies from 0 to 0.53 over ∼9400 yr in a single case with zero obliquity. In all cases, we find that the climate remains stable, but regional habitability changes through time in unique ways. At the same time, the moist greenhouse state is approached but only when at the highest eccentricities.
Tracing the Total Stellar Mass and Star Formation of High-redshift Protoclusters
Authors: Popescu Roxana , Pope Alexandra , Lee Kyoung-Soo , Alberts Stacey , Chiang Yi-Kuan , Lee Sowon , Brodwin Mark , McKinney Jed , Ramakrishnan Vandana 
Published: November 2023

Abstract
As the progenitors of present-day galaxy clusters, protoclusters are excellent laboratories to study galaxy evolution. Since existing observations of protoclusters are limited to the detected constituent galaxies at UV and/or infrared wavelengths, the details of how typical galaxies grow in these young, pre-virialized structures remain uncertain. We measure the total stellar mass and star formation within protoclusters, including the contribution from faint undetected members by performing a stacking analysis of 211 z = 2–4 protoclusters selected as Planck cold sources. We stack Wide-field Infrared Survey Explorer and Herschel/SPIRE images to measure the angular size and the spectral energy distribution of the integrated light from the protoclusters. The fluxes of protoclusters selected as Planck cold sources can be contaminated by line-of-sight interlopers. Using the WebSky simulation, we estimate that a single protocluster contributes 33% ± 15% of the flux of a Planck cold source on average. After this correction, we obtain a total star formation rate of 7.3 ± 3.2 × 103
M
⊙yr−1 and a total stellar mass of 4.9 ± 2.2 × 1012
M
⊙. Our results indicate that protoclusters have, on average, 2× more star formation and 4× more stellar mass than the total contribution from individually detected galaxies in spectroscopically confirmed protoclusters. This suggests that much of the total flux within z = 2–4 protoclusters comes from galaxies with luminosities lower than the detection limit of SPIRE (L
IR < 3 × 1012
L
⊙). Lastly, we find that protoclusters subtend a half-light radius of 2.′8 (4.2–5.8 cMpc), which is consistent with simulations.
Generation of Subion Scale Magnetic Holes from Electron Shear Flow Instabilities in Plasma Turbulence
Authors: Arrò Giuseppe , Pucci Francesco , Califano Francesco , Innocenti Maria Elena , Lapenta Giovanni 
Published: November 2023

Abstract
Magnetic holes (MHs) are coherent structures associated with strong magnetic field depressions in magnetized plasmas. They are observed in many astrophysical environments at a wide range of scales, but their origin is still under debate. In this work, we investigate the formation of subion scale MHs using a fully kinetic 2D simulation of plasma turbulence initialized with parameters typical of the Earth’s magnetosheath. Our analysis shows that the turbulence is capable of generating subion scale MHs from large scale fluctuations via the following mechanism: first, the nonlinear large scale dynamics spontaneously leads to the development of thin and elongated electron velocity shears; these structures then become unstable to the electron Kelvin–Helmholtz instability and break up into small scale electron vortices; the electric current carried by these vortices locally reduces the magnetic field, inducing the formation of subion scale MHs. The MHs thus produced exhibit features consistent with satellite observations and with previous numerical studies. We finally discuss the kinetic properties of the observed subion scale MHs, showing that they are characterized by complex non-Maxwellian electron velocity distributions exhibiting anisotropic and agyrotropic features.
Understanding the Duration of Solar and Stellar Flares at Various Wavelengths
Authors: Reep Jeffrey W. , Airapetian Vladimir S. 
Published: November 2023

Abstract
Recent irradiance measurements from numerous heliophysics and astrophysics missions including Solar Dynamics Observatory (SDO), GOES, Kepler, TESS, Chandra, the X-ray Multi-Mirror Mission, and NICER have provided critical input into understanding the physics of the most powerful transient events on the Sun and magnetically active stars:solar and stellar flares. The light curves of flare events from the Sun and stars show remarkably similar shapes, typically with a sharp rise and protracted decay phase. The duration of solar and stellar flares has been found to be correlated with the intensity of the event in some wavelengths, such as white light, but not in other wavelengths, such as soft X-rays, but it is not evident why this is the case. In this study, we use a radiative hydrodynamics code to examine factors affecting the duration of flare emission at various wavelengths. The duration of a light curve depends on the temperature of the plasma, the height in the atmosphere at which the emission forms, and the relative importance of cooling due to radiation, thermal conduction, and enthalpy flux. We find that there is a clear distinction between emission that forms low in the atmosphere and responds directly to heating, and emission that forms in the corona, indirectly responding to heating-induced chromospheric evaporation, a facet of the Neupert effect. We discuss the implications of our results for a wide range of flare energies.
Mass Ratio Distribution of Hierarchical Triple Systems from the LAMOST-MRS Survey
Authors: He Tongyu , Li Jiangdan , Chen Xuefei , Yang Rong-jia , Xiao Lin , Han Zhanwen 
Published: November 2023

Abstract
Hierarchical triple-star systems consists of three components organized into an inner binary (M
1, M
2) and a more distant outer tertiary (M
3) star. The LAMOST Medium-Resolution Spectroscopic Survey has offered a great sample for the study of triple-system populations. We used the peak amplitude ratio method to obtain the mass ratio (q
in, q
out) of a triple system from its normalized spectrum. By calculating the cross-correlation function, we determined the correlation between the mass ratio q
out (M
3/(M
1 + M
2)) and the amplitude ratio (A
3/(A
1 + A
2)). We derived a q
in of 0.5–1.0 and a q
out between 0.2 and 0.8. By fitting a power-law function of the corrected q
in distribution, γ
in is estimated to be −0.654 ± 2.915, 4.304 ± 1.125, and 11.371 ± 1.309 for A-, F-, and G-type stars. The derived γ
in values increase as the mass decreases, indicating that less massive stars are more likely to have companion stars with similar masses. By fitting a power-law function of the corrected q
out distribution, γ
out is estimated to be −2.016 ± 0.172, −1.962 ± 0.853, and −1.238 ± 0.141 for G-, F-, and A-type stars, respectively. The γ
out values show a trend of growth toward lower primary star masses.
Numerical Simulation on the Leading Edge of Coronal Mass Ejection in the Near-Sun Region
Authors: Mei Zhixing , Ye Jing , Li Yan , Xu Shanshan , Chen Yuhao , Hu Jialiang 
Published: November 2023

Abstract
The coronal mass ejections (CMEs) observed by white-light coronagraphs, such as the Large Angle and Spectrometric Coronagraph (LASCO) C2/C3, commonly exhibit the three-part structure, with the bright leading edge as the outermost part. In this work, we extend previous work on the leading edge by performing a large-scale 3D magnetohydrodynamic numerical simulation on the evolution of an eruptive magnetic flux rope (MFR) in a near-Sun region based on a radially stretched calculation grid in spherical coordination and the incorporation of solar wind. In the early stage, the new simulation almost repeats the previous results, i.e., the expanding eruptive MFR and associated CME bubble interact with the ambient magnetic field, which leads to the appearance of the helical current ribbon/boundary (HCB) wrapping around the MFR. The HCB can be interpreted as a possible mechanism of the CME leading edge. Later, the CME bubble propagates self-consistently to a larger region beyond a few solar radii from the solar center, similar to the early stage of evolution. The continuous growth and propagation of the CME bubbles leading to the HCB can be traced across the entire near-Sun region. Furthermore, we can observe the HCB in the white-light synthetic images as a bright front feature in the large field of view of LASCO C2 and C3.
A Dragon Out of Breath? Monitoring High-velocity Outflows from the High-mass Gamma-Ray Binary LS 2883/PSR B1259–63 During the 2017–2021 Binary Cycle
Authors: Hare Jeremy , Pavlov George G. , Garmire Gordon P. , Kargaltsev Oleg 
Published: November 2023

Abstract
Observations of the high-mass gamma-ray binary LS 2883/PSR B1259–63 with the Chandra X-ray Observatory during the 2011–2014 and 2014–2017 binary cycles have shown X-ray-emitting clumps, presumably ejected from the binary during periastron passages. These clumps traveled at projected velocities of ∼0.1c and have shown evidence of being accelerated. The clumps also evolved in shape, size, and flux. We monitored this binary with Chandra during the 2017–2021 binary cycle to search for additional X-ray-emitting ejections. While we find evidence of extended emission in two of the six observations, it is unlike the clumps observed in the previous three binary cycles. More specifically, the extended emission is not well localized, and no bright clump is observed moving away from the binary. It is still unclear what caused the lack of X-ray-emitting clump in this orbital cycle, but it may be due to changes in the decretion disk of the Be star.
The Maximum Energy of Shock-accelerated Cosmic Rays
Authors: Diesing Rebecca 
Published: November 2023

Abstract
Identifying the accelerators of Galactic cosmic ray (CR) protons with energies up to a few PeV (1015 eV) remains a theoretical and observational challenge. Supernova remnants (SNRs) represent strong candidates because they provide sufficient energetics to reproduce the CR flux observed at Earth. However, it remains unclear whether they can accelerate particles to PeV energies, particularly after the very early stages of their evolution. This uncertainty has prompted searches for other source classes and necessitates comprehensive theoretical modeling of the maximum proton energy,

E

max

, accelerated by an arbitrary shock. While analytic estimates of

E

max

have been put forward in the literature, they do not fully account for the complex interplay between particle acceleration, magnetic field amplification, and shock evolution. This paper uses a multizone, semianalytic model of particle acceleration based on kinetic simulations to place constraints on

E

max

for a wide range of astrophysical shocks. In particular, we develop relationships between

E

max

, shock velocity, size, and ambient medium. We find that SNRs can only accelerate PeV particles under a select set of circumstances, namely, if the shock velocity exceeds ∼104 km s−1 and escaping particles drive magnetic field amplification. However, older and slower SNRs may still produce observational signatures of PeV particles due to populations accelerated when the shock was younger. Our results serve as a reference for modelers seeking to quickly produce a self-consistent estimate of the maximum energy accelerated by an arbitrary astrophysical shock.
1

1

Presented as a thesis to the Department of Astronomy and Astrophysics, The University of Chicago, in partial fulfillment of the requirements for a Ph.D. degree.
Rankine–Hugoniot Relations and Magnetic Field Enhancement in Turbulent Shocks
Authors: Gedalin Michael 
Published: November 2023

Abstract
In fast collisionless shocks, the density and magnetic field increase and the plasma is heated. The compression and heating are ultimately determined by the Rankine–Hugoniot relations connecting the upstream and downstream parameters. The standard Rankine–Hugoniot relations take into account only mean upstream and downstream parameters. Observations at the Earth's bow shock show that the downstream magnetic field does not always relax to a uniform state, but large amplitude magnetic oscillations persist. Here, these Rankine–Hugoniot relations are extended to such turbulent shocks where the mean downstream magnetic field is accompanied by magnetic fluctuations. It is shown that the turbulent magnetic field pressure may substantially exceed the pressure of the mean field, while the density compression and heating may be only weakly affected. Thus, strong amplification of the rms magnetic field can be achieved at the expense of a modest reduction of plasma heating.
Evolutionary Relationship between Sunspot Groups and Soft X-Ray Flares over Solar Cycles 21–25
Authors: Lin 林 Jiaqi 家琪 , Wang 王 Feng 锋 , Deng 邓 Linhua 林华 , Deng 邓 Hui 辉 , Mei 梅 Ying 盈 , Zhang 张 Xiaojuan 小娟 
Published: November 2023

Abstract
Studying the interaction between solar flares and sunspot groups (SGs) is crucial for understanding and predicting solar activity. We examined the distribution, correlation, and flaring rates in the northern and southern hemispheres to reveal the relationship between different classes of soft X-ray (SXR) flares and different magnetic classifications of SGs. We discovered a significant north–south asymmetry in SXR flares and SG distribution over Solar Cycles (SC) 21–25. In the rising phase of SC24, the northern hemisphere’s activity is significantly excessive. In the declining phase of SC24, the southern hemisphere’s activity becomes significantly excessive. The total numbers of various SXR flares and SGs vary between the northern and southern hemispheres over the solar cycle. B-class flares are negatively correlated with all SGs at maximum but positively correlated at minimum. C-class flares correlate best with α and β SGs. M-class flares correlate best with β
γ
δ and β SGs. X-class flares correlate highest with β
γ
δ SGs. The flaring rate of each flare class is lowest for α SGs and highest for β
γ
δ SGs. The flaring rates are higher in the southern hemisphere than in the northern hemisphere. Our results demonstrate that solar flares originate from different sources of solar active regions; the high-energy flares tend to be caused by more complex magnetic fields.
Radar Perspective of the Aristarchus Pyroclastic Deposit and Implications for Future Missions
Authors: Morgan G. A. , Jawin E. R. , Campbell B. A. , Patterson G. W. , Bramson A. M. , Nypaver C. A. , Stopar J. D. , Jozwiak L. M. , Stickle A. M. , Bhiravarasu S. S. 
Published: November 2023

Abstract
The Aristarchus plateau represents one of the most complex volcanic provinces on the lunar surface and is host to the largest pyroclastic deposit on the Moon. Lunar pyroclastic deposits offer a window into the Moon’s interior and represent a valuable resource to support a sustained human presence. We present a new analysis of the Aristarchus pyroclastic deposit using Mini-RF bistatic radar data at wavelengths of 4.2 and 12.6 cm. Building on previous Earth-based Arecibo Observatory radar studies at 12.6 and 70 cm, we place further constraints on the spatial extent of the pyroclastic deposit and investigate the clast size distribution and provenance of foreign material distributed within the formation. Concentrations of blocky material >0.5 cm in diameter and suspended within the upper decimeters of the pyroclastic deposit are associated with potential buried mare flows along the rim of Vallis Schröteri and discrete pockets of primary material ejected by the Aristarchus impact. Unraveling the deposit from nonpyroclastic materials and the surrounding landscape creates new constraints with which to reconstruct the volcanic history of the region. From a future mission perspective, the identification of primary Aristarchus material distributed across the plateau offers an opportunity to sample diverse volcanic lithologies within an area that could be sampled by a single Commercial Lunar Payload Services mission. In terms of lunar resource in situ utilization, such ejected material also represents a contaminant; thus, radar data provide an invaluable tool to identify pristine pyroclastic material for mission planners.