bluuebunny/crossref_metadata_2025_split huggingface dataset:
Assessing the Role of Recreational Activities in Physical Education Participation of College Students in One State University in Laguna Philippines
Authors: Aquino John Michael D. 
Published: June 2023

Physical education (PE) is a crucial component of a well-rounded education because it equips the holistic aspects of the students required to live a healthy and active lifestyle. The objective of this study is to assess the role of recreational activities on physical education participation. This study explores the students’ profile, role of recreational activities in physical education participation and its relationship among 2nd year college students in one state university in Laguna, Philippines. This research employs descriptive design and random sampling method in determining the respondents. The researcher analyzed the gathered data from the administered validated self-made questionnaire. The results showed that the respondents relished the recreational activities immensely and actively participated which demonstrate that the recreational activities enabled physical activity, intellectual and emotional stimulation, and interaction with others. The high levels of participation illustrates that the students enjoyed the games and that they benefited to their overall enjoyment of physical education courses. Consequently, the results emphasize the respondents' favorable feelings toward physical education classes along with their strong drive to get involved and prosper in their classes. Their desire to learn and pursue new physical activities is indicative of their proactive approach to PE. The significance of nurturing a supportive and active physical education environment that encourages the holistic development and well-being of students is highlighted. It is recommended to utilize the designed process handbook to prioritize the incorporation of recreational activities into their curricula and provide an atmosphere of encouragement to have an active engagement and enjoyment.
Phrasal Prominence Location is Influenced by IP Boundary Location in the Absence of Stress Clash
Authors: Azzabou - Kacem Soundess , Turk Alice 
Published: June 2023

Several factors can influence early prominence in double-stressed words (e.g., Maltese), namely the presence of foot-level stress clash with a following word, and their adjacency to domain-initial boundaries. We test whether initial accent can occur in such words even when the words are spoken in isolation. Fourteen targets and 26 tri-syllabic filler-items were produced in isolation and in a frame sentence, e.g., [Say Maltese again], by 12 English speakers. In isolation, ‘Early’ prominence on, e.g., Mal- is more likely because the target is utterance- and phrase-initial. In the Embedded condition, phrasal prominence should be less likely on the initial syllable because there is a weaker boundary preceding the target. Three linguists coded prominence location. Early prominence rates, and Early scores (sum of ‘Early’ judgements/token) were calculated. While 96% of the Embedded tokens were perceived with ‘Late’ prominence, this pattern appeared in only 48% of the Isolated targets. The Early scores were also significantly higher in the Isolated condition. Overall, results suggest that doubly-stressed words show stress shifting to demarcate the left IP-edge. Because this study uses contexts free of stress clash with a following word, its results provide evidence that other factors, namely domain-onset-marking, can influence prominence location.
Трихобезоар тонкого кишечника у пациентки в сроке 33 недель беременности: клинический случай
Authors: Иралина Р.В. , Аутенов Б.Б. , Филатова Н.А. 
Published: June 2023

Актуальность: Трихобезоары, представляющие собой безоары, состоящие из волос, возникают при трихотилломании, навязчивом выдергивании волос, и трихофагии, поедании волос. Они локализуются преимущественно в желудке. В редких случаях волосы полностью проходят через желудок и образуют трихобезоар в тонкой кишке. Данная патология является очень редким заболеванием. Больные с инородными телами желудка типа трихобезоара наблюдаются в клинической практике чрезвычайно редко.
Цель исследования – показать и проанализировать динамику клинического течения острой кишечной непроходимости вследствие трихобезоара в тонком кишечнике у беременной на примере клинического случая.
Материалы и методы: В исследовании использован метод наблюдения за изменением клинического состояния в случае редко встречающегося трихобезоара в тонком кишечнике у беременной.
Результаты: В данной статье представлен редкий клинический случай трихобезоара тонкого кишечника у пациентки в сроке 33 недель беременности с неизвестной историей трихофагии и с предварительным диагнозом острого аппендицита. Следующий пример является первым случаем оперативного лечения подобного заболевания в родильном отделении №2 Костанайской областной больницы. У пациентки 25 лет, которая находилась в отделении патологии беременных, на 4-й день нахождения в стационаре, появилась клиническая картина кишечной непроходимости. Представлены результаты лабораторных и инструментальных методов исследования. После проведения мультидисциплинарного консилиума врачей было принято решение о проведении операции с учетом развития острой кишечной непроходимости. Пациентке выполнено хирургическое вмешательство в объеме: Нижнесрединная лапаротомия. Кесарево сечение в нижнем маточном сегменте. Устранение кишечной непроходимости. Санация и дренирование брюшной полости. После операции состояние больной улучшилось. Пациентка была выписана домой на 10 сутки с рекомендациями.
Заключение: Представленный клинический случай показывает, что формирование трихобезоара требует продолжительного времени. Пагубная привычка к проглатыванию волос является главным фактором формирования трихобезоара. Представленный нами клинический случай интересен для врачей в качестве напоминания о редко встречающихся патологиях желудочно-кишечного тракта.
BCH-based Compactors with Data Compression for Test Responses
Authors: Reungpeerakul Taweesak , Qian Xiaoshu , Mourad Samiha 
Published: June 2023

This paper presents a novel approach to compacting a test response for a multiple scan chains design. The compactor design is based on an extended ( + 1; k) BCH code, where k is the number of information bits and + 1 is the number of bits in the block. It can detect any odd number of single bit errors or up to 2t single-bit errors, where t is a positive integer, - k mt, and + 1 = 2m. Also we use a controllable mask to handle any number of unknown logic values (Xs) on test responses. We show how extra control data can be reduced by proposed compression technique. Compared to augmenting previous space compaction techniques with additional circuitry to mask any number of Xs, our approach can detect more single-bit errors with minimum number of compactor outputs. This leads to fewer tester channels, shorter test application time, and smaller test data volumes regardless of the Circuit Under Test (CUT) and fault models.
Wave probabilistic functions, entanglement and quasi-non-ergodic models
Authors: Svitek Miroslav 
Published: June 2023

The paper presents the theory of wave probabilistic models together with their important features like inclusion-exclusion rule, product rule and entanglement. These features are athematically described and the illustrative example is shown to demonstrate the possible applications of the theory. The presented theory can be also applied for modeling of quasi-non-ergodic probabilistic systems. First of all we show the new methodology on binary non-ergodic time series. The theory is extended into M-dimensional non-ergodic n-valued systems with linear ergodicity evolution that are called quasi-on-ergodic probabilistic systems.
Leakage Current and Pollutant Properties of Porcelain Insulators from the Geothermal Area
Authors: Waluyo Waluyo , Sinisuka Ngapuli Irmea , Suwarno Suwarno , Djauhari Maman Abdurahman 
Published: June 2023

This manuscript presents the experimental results of a new-clean and seven geothermal naturally polluted outdoor porcelain insulators. These insulators were tested in a hermetically sealed chamber, where their leakage currents and applied voltages were measured with a storage digital oscilloscope. The measured data could be recorded oscilloscope and transferred to a computer, saved in softcopy forms. FFT was used to analyze the leakage current waveforms, and correlation coe±cient matrix and principal component analysis (PCA) were used to analyze the relation among parameters. It was also carried out EDAX tests of insulator adhered pollutant. The results indicated that the power factors and leakage current amplitudes closed to humidity, the phase angle closed to THD, and temperature opposited the humidity. The ratios of insulator impedance on the high and low humidity were ranged from 0.8696 until 0.1343. The small insulator impedance ratios were rearched on the ¯rst and seventh withdrawals, i.e. 0.1363 and 0.1343 respectively. On these insulators, THD ratios on the same conditions were 0.3739 and 0.4598 respectively. These phenomena were caused by dry season, which amount of pollutant stuck on the insulator surfaces signi¯cantly. On the high humidity, the minimum phase angles ranged between 66.8 and 25.7 degrees. Sulfur chemical element was found in medium composition on the pollutant.
Scaling K2. VI. Reduced Small-planet Occurrence in High-galactic-amplitude Stars
Authors: Zink Jon K. , Hardegree-Ullman Kevin K. , Christiansen Jessie L. , Petigura Erik A. , Boley Kiersten M. , Bhure Sakhee , Rice Malena , Yee Samuel W. , Isaacson Howard , Fernandes Rachel B. , Howard Andrew W. , Blunt Sarah , Lubin Jack , Chontos Ashley , Pidhorodetska Daria , MacDougall Mason G. 
Published: June 2023

Abstract
In this study, we performed a homogeneous analysis of the planets around FGK dwarf stars observed by the Kepler and K2 missions, providing spectroscopic parameters for 310 K2 targets —including 239 Scaling K2 hosts—observed with Keck/HIRES. For orbital periods less than 40 days, we found that the distribution of planets as a function of orbital period, stellar effective temperature, and metallicity was consistent between K2 and Kepler, reflecting consistent planet formation efficiency across numerous ∼1 kpc sight-lines in the local Milky Way. Additionally, we detected a 3× excess of sub-Saturns relative to warm Jupiters beyond 10 days, suggesting a closer association between sub-Saturn and sub-Neptune formation than between sub-Saturn and Jovian formation. Performing a joint analysis of Kepler and K2 demographics, we observed diminishing super-Earth, sub-Neptune, and sub-Saturn populations at higher stellar effective temperatures, implying an inverse relationship between formation and disk mass. In contrast, no apparent host-star spectral-type dependence was identified for our population of Jupiters, which indicates gas-giant formation saturates within the FGK mass regimes. We present support for stellar metallicity trends reported by previous Kepler analyses. Using Gaia DR3 proper motion and radial velocity measurements, we discovered a galactic location trend; stars that make large vertical excursions from the plane of the Milky Way host fewer super-Earths and sub-Neptunes. While oscillation amplitude is associated with metallicity, metallicity alone cannot explain the observed trend, demonstrating that galactic influences are imprinted on the planet population. Overall, our results provide new insights into the distribution of planets around FGK dwarf stars and the factors that influence their formation and evolution.
Searching in H i for Massive Low Surface Brightness Galaxies: Samples from HyperLeda and the UGC
Authors: O’Neil K. , Schneider Stephen E. , van Driel W. , Liu G. , Joseph T. , Schwortz A. C. , Butcher Z. 
Published: June 2023

Abstract
A search has been made for 21 cm H i line emission in a total of 350 unique galaxies from two samples whose optical properties indicate they may be massive. The first consists of 241 low surface brightness (LSB) galaxies of morphological type Sb and later selected from the HyperLeda database and the second consists of 119 LSB galaxies from the UGC with morphological types Sd-m and later. Of the 350 unique galaxies, 239 were observed at the Nançay Radio Telescope, 161 at the Green Bank Telescope, and 66 at the Arecibo telescope. A total of 295 (84.3%) were detected, of which 253 (72.3%) appear to be uncontaminated by any other galaxies within the telescope beam. Finally, of the total detected, uncontaminated galaxies, at least 31 appear to be massive LSB galaxies, with a total H i mass ≥ 1010
M
⊙, for H
0 = 70 kms−1 Mpc−1. If we expand the definition to also include galaxies with significant total (rather than just gas) mass, i.e., those with an inclination-corrected H i line width W
50,cor > 500 km s−1, this brings the total number of massive LSB galaxies to 41. There are no obvious trends between the various measured global galaxy properties, particularly between mean surface brightness and galaxy mass.
ELVES. III. Environmental Quenching by Milky Way–mass Hosts
Authors: Greene Jenny E. , Danieli Shany , Carlsten Scott , Beaton Rachael , Jiang Fangzhou , Li Jiaxuan 
Published: June 2023

Abstract
Isolated dwarf galaxies usually exhibit robust star formation but satellite dwarf galaxies are often devoid of young stars, even in Milky Way–mass groups. Dwarf galaxies thus offer an important laboratory of the environmental processes that cease star formation. We explore the balance of quiescent and star-forming galaxies (quenched fractions) for a sample of ∼400 satellite galaxies around 30 Local Volume hosts from the Exploration of Local VolumE Satellites (ELVES) Survey. We present quenched fractions as a function of satellite stellar mass, projected radius, and host halo mass, to conclude that overall, the quenched fractions are similar to the Milky Way, dropping below 50% at satellite M
* ≈ 108
M
⊙. We may see hints that quenching is less efficient at larger radii. Through comparison with the semianalytic modeling code SatGen, we are also able to infer average quenching times as a function of satellite mass in host halo-mass bins. There is a gradual increase in quenching time with satellite stellar mass rather than the abrupt change from rapid to slow quenching that has been inferred for the Milky Way. We also generally infer longer average quenching times than recent hydrodynamical simulations. Our results are consistent with models that suggest a wide range of quenching times are possible via ram pressure stripping, depending on the clumpiness of the circumgalactic medium, the orbits of the satellites, and the degree of earlier preprocessing.
Strong Dark Matter Self-interactions Diversify Halo Populations within and surrounding the Milky Way
Authors: Yang Daneng , Nadler Ethan O. , Yu Hai-Bo 
Published: June 2023

Abstract
We perform a high-resolution cosmological zoom-in simulation of a Milky Way (MW)–like system, which includes a realistic Large Magellanic Cloud analog, using a large differential elastic dark matter self-interaction cross section that reaches ≈100 cm2 g−1 at relative velocities of ≈10 km s−1, motivated by the diverse and orbitally dependent central densities of dwarf galaxies within and surrounding the MW. We explore the effects of dark matter self-interactions on satellite, splashback, and isolated halos through their abundance, central densities, maximum circular velocities, orbital parameters, and correlations between these variables. We use an effective constant cross section model to analytically predict the stages of our simulated halos’ gravothermal evolution, demonstrating that deviations from the collisionless

R

max

–

V

max

relation can be used to select deeply core-collapsed halos, where

V

max

is a halo’s maximum circular velocity, and

R

max

is the radius at which it occurs. We predict that a sizable fraction (≈20%) of subhalos with masses down to ≈108
M
⊙ is deeply core collapsed in our SIDM model. Core-collapsed systems form ≈10% of the isolated halo population down to the same mass; these isolated, core-collapsed halos would host faint dwarf field galaxies with extremely steep central density profiles. Finally, most halos with masses above ≈109
M
⊙ are core-forming in our simulation. Our study thus demonstrates how self-interactions diversify halo populations in an environmentally dependent fashion within and surrounding MW-mass hosts, providing a compelling avenue to address the diverse dark matter distributions of observed dwarf galaxies.
The Hateful Eight: Connecting Massive Substructures in Galaxy Clusters like A2744 to Their Dynamical Assembly State Using the Magneticum Simulations
Authors: Kimmig Lucas C. , Remus Rhea-Silvia , Dolag Klaus , Biffi Veronica 
Published: June 2023

Abstract
Substructures are known to be good tracers for the dynamical states and recent accretion histories of the most massive collapsed structures in the universe, galaxy clusters. Observations find extremely massive substructures in some clusters, especially Abell 2744 (A2744), which are potentially in tension with the ΛCDM paradigm because they are not found in simulations directly. However, the methods to measure substructure masses strongly differ between observations and simulations. Using the fully hydrodynamical cosmological simulation suite Magneticum Pathfinder, we develop a method to measure substructure masses in projection from simulations, similarly to the observational approach. We identify a simulated A2744 counterpart that not only has eight substructures of similar mass fractions but also exhibits similar features in the hot gas component. This cluster formed only recently through a major merger together with at least six massive minor merger events since z = 1, where previously the most massive component had a mass of less than 1 × 1014
M
⊙. We show that the mass fraction of all substructures and of the eighth substructure separately are excellent tracers for the dynamical state and assembly history for all galaxy cluster mass ranges, with high fractions indicating merger events within the last 2 Gyr. Finally, we demonstrate that the differences between subhalo masses measured directly from simulations as bound and those measured in projection are due to methodology, with the latter generally 2–3 times larger than the former. We provide a predictor function to estimate projected substructure masses from SubFind masses for future comparison studies between simulations and observations.
Grain Alignment and Rotational Disruption by Radiative Torques in Exoplanet Atmospheres
Authors: Hoang Thiem , Lazarian Alex 
Published: June 2023

Abstract
Dust clouds are ubiquitous in the atmospheres of hot Jupiters and affect their observable properties. The alignment of dust grains in the clouds and resulting dust polarization provide a promising way to study the magnetic fields of exoplanets. Moreover, the grain size distribution plays an important role in the physical and chemical processes in the atmospheres, which are rather uncertain. In this paper, we first study the grain alignment of dust grains in the atmospheres of hot Jupiters by radiative torques (RATs). We find that silicate grains can be aligned by RATs with the magnetic fields (B − RAT) due to the strong magnetic fields of hot Jupiters, but carbonaceous grains of diamagnetic material tend to be aligned with the radiation direction (k − RAT). At a low altitude of r < 2R
p, where R
p is the planet radius, only large grains can be aligned, but tiny grains of a ∼ 0.01 μm can be aligned at a high altitude of r > 3R
p. We then study the rotational disruption of dust grains by the RAT disruption (RAT-D) mechanism. We find that large grains can be disrupted by RAT-D into smaller sizes. Grains of high tensile strength are disrupted at an altitude of r > 3R
p, but grains of low tensile strength can be disrupted at a lower altitude. We suggest that the disruption of large grains into smaller ones can facilitate dust clouds escaping to high altitudes due to lower gravity and may explain the presence of high-altitude clouds in hot Jupiters, as well as superpuff atmospheres.
Hanle Effect with Angle-dependent Partial Frequency Redistribution in Three-dimensional Media
Authors: Anusha L. S. 
Published: June 2023

Abstract
There has been a constant improvement in the observational measurement of linear polarization in chromospheric spectral lines in the last three decades. However, modeling polarized profiles of these lines still remains incomplete, due to the lack of inclusion of fundamental physics in modeling efforts. To model the observed solar spectrum and its linear polarization, we need a solution to the polarized radiative transfer equation. The polarization in strong resonance lines originates from the scattering mechanism known as the partial frequency redistribution (PFR) of an anisotropic radiation field. The understanding of the linear polarization in spatially resolved structures needs radiative transfer solutions in multidimensional geometries. In this paper, we explore the effects of angle-dependent PFR on scattering polarization profiles formed in three-dimensional (3D) media. We find that the 3D geometry combined with angle-dependent PFR produces more scattering polarization than an angle-averaged one.
JWST NIRSpec Observations of Supernova 1987A—From the Inner Ejecta to the Reverse Shock
Authors: Larsson J. , Fransson C. , Sargent B. , Jones O. C. , Barlow M. J. , Bouchet P. , Meixner M. , Blommaert J. A. D. L. , Coulais A. , Fox O. D. , Gastaud R. , Glasse A. , Habel N. , Hirschauer A. S. , Hjorth J. , Jaspers J. , Kavanagh P. J. , Krause O. , Lau R. M. , Lenkić L. , Nayak O. , Rest A. , Temim T. , Tikkanen T. , Wesson R. , Wright G. S. 
Published: June 2023

Abstract
We present initial results from JWST NIRSpec integral field unit observations of the nearby supernova SN 1987A. The observations provide the first spatially resolved spectroscopy of the ejecta and equatorial ring (ER) over the 1–5 μm range. We construct 3D emissivity maps of the [Fe i] 1.443 μm line from the inner ejecta and the He i 1.083 μm line from the reverse shock (RS), where the former probes the explosion geometry and the latter traces the structure of the circumstellar medium. We also present a model for the integrated spectrum of the ejecta. The [Fe i] 3D map reveals a highly asymmetric morphology resembling a broken dipole, dominated by two large clumps with velocities of ∼2300 km s−1. We also find evidence that the Fe-rich inner ejecta have started to interact with the RS. The RS surface traced by the He i line extends from just inside the ER to higher latitudes on both sides of the ER with a half-opening angle ∼45°, forming a bubble-like structure. The spectral model for the ejecta allows us to identify the many emission lines, including numerous H2 lines. We find that the H2 is most likely excited by far-UV emission, while the metal-line ratios are consistent with a combination of collisional excitation and recombination in the low-temperature ejecta. We also find several high-ionization coronal lines from the ER, requiring a temperature ≳2 × 106 K.