bluuebunny/crossref_metadata_2025_split huggingface dataset:
PENGARUH MEDIA PAPAN PECAHAN TERHADAP HASIL BELAJAR SISWA KELAS III MATERI PECAHAN SEDERHANA PEMBELAJARAN MATEMATIKA SD
Authors: Ulandari Jeni , Surmilasari Nora , Jayanti  
Published: August 2023

ABSTRAC
This study aims to find out how the influence of the fraction board media on the learning outcomes of class III students on simple fractions in elementary mathematics learning. The samples for this study were 2 classes selected by random sampling, namely class IIIA students and class IIIB students at SD Negeri 09 Pedamaran. This study used an experimental research method. The method of collecting student data is through observation and documentation, while the data on learning outcomes is collected using a multiple choice test in the form of learning outcomes. With a posttest-only control design. Methods of data analysis researchers used quantitative analysis using independent t test known sig. (2-tailed) of 0.000 <0.05 or it can also be seen from t_count = 7.025 > t_table = 2.064. So it can be concluded that there is a significant difference between the average learning outcomes of the experimental class and the control class. Thus it can be concluded that there is an influence of fraction board media on the learning outcomes of class III students on simple fractions in elementary mathematics learning.
Keywords: Fraction Board, Learning Outcomes, Simple Fractions
ABSTRAK

Penelitian ini bertujuan untuk mengetahui adakah pengaruh media papan pecahan terhadap hasil belajar siswa kelas III materi pecahan sederhana pembelajaran matematika SD. Sempel penelitian ini adalah 2 kelas dipilih secara ranbom sampling yaitu, siswa kelas IIIA dan siswa kelas IIIB di SD Negeri 09 Pedamaran. Penelitian ini menggunakan metode penelitian jenis eksperimen. Metode pengumpulan data siswa melalui observasi dan dokumentasi, sedangkan data hasil belajar dikumpulkan menggunakan tes berbentuk pilihan ganda hasil belajar. Dengan desain posttest-only control design. Metode analisis data peneliti menggunakan analisis kuantitatif menggunakan uji independent t test diketahui nilai sig. (2-tailed) sebesar 0,000 0,05 atau dapat juga dilihat dari = 7,025 = 2,064. Maka dapat disimpulkan bahwa ada perbedaan yang signifikan antara rata-rata hasil belajar kelas esksperimen dan kelas kontrol. Dengan demikian dapat disimpulkan bahwa terdapat pengaruh media papan pecahan terhadap hasil belajar siswa kelas III materi pecahan sederhana pembelajaran matematika SD.
Outcomes of Patients with FLT3 Positive Acute Myeloid Leukemia; an Experience from a Tertiary Care Hospital in Karachi, Pakistan
Authors: Zulfiqar Maria , Ali Natasha , Shaikh Usman , Jehanzeb Hamzah , Arif Salman , Fasih Khan Zurrya , Saeed Nabiha , Ansar Zeeshan 
Published: August 2023

Introduction: Molecular genetic abnormalities in AML are essential for disease diagnosis and determining prognosis and clinical course. Mutations in FLT3 and NPM genes are the most frequent genetic abnormalities, which are also known to impact disease outcomes. FLT3 mutations have been identified in approximately 30% of denovo AML patients and are associated with poor prognoses. This study aimed to determine the response to induction chemotherapy, overall survival, and relapse rate in patients with FLT3-positive acute myeloid leukaemia. Materials and Methods: In this study, a retrospective analysis was performed of 75 newly diagnosed patients with AML registered between January 2015 and July 2022. Patient demographics and clinical-haematological parameters were noted, and molecular analysis for FLT3 ITD/TKD and NPM mutations was performed. All the patients received standard induction chemotherapy, and their response to treatment, overall survival, and relapse rate were assessed. Results: A total of 75 cases of AML were analysed. The mean age of the sample was 34.9 years, of which 65.3% were males and 34.7% were females. The patients were stratified into two groups: those who were positive for FLT3 while negative for NPM (FLT3+/NPM-), representing 17.3%, and those who were negative for both FLT3 and NPM (FLT3-/NPM-), representing 82.7% of cases. On day 28 post-induction, the complete remission rate was 69.2% in the FLT3 positive group and 77.4% in the FLT3 negative group. In the FLT3+/NPM- group, 55.6% of cases who were in remission at day 28 subsequently relapsed, compared to 50.0% of FLT3-/NPM- cases. The overall median survival time for the cohort and FLT3+ group was 1467 days, while that of the FLT3-group could not be estimated due to the very high survival rate. Conclusion: No significant differences in outcomes were observed in patients who were FLT3 positive compared to those who were FLT3 negative.
Estimating lighting direction in scenes with multiple objects
Authors: Peterson Lindsay M. , Kersten Daniel J. , Mannion Damien J. 
Published: August 2023

AbstractTo recover the reflectance and shape of an object in a scene, the human visual system must account for the properties of the light illuminating the object. Here, we examine the extent to which multiple objects within a scene are utilised to estimate the direction of lighting in a scene. In Experiment 1, we presented participants with rendered scenes that contained 1, 9, or 25 unfamiliar blob-like objects and measured their capacity to discriminate whether a directional light source was left or right of the participants’ vantage point. Trends reported for ensemble perception suggest that the number of utilised objects—and, consequently, discrimination sensitivity—would increase with set size. However, we find little indication that increasing the number of objects in a scene increased discrimination sensitivity. In Experiment 2, an equivalent noise analysis was used to measure participants’ internal noise and the number of objects used to judge the average light source direction in a scene, finding that participants relied on 1 or 2 objects to make their judgement regardless of whether 9 or 25 objects were present. In Experiment 3, participants completed a shape identification task that required an implicit judgement of light source direction, rather than an explicit judgement as in Experiments 1 and 2. We find that sensitivity for identifying surface shape was comparable for scenes containing 1, 9, and 25 objects. Our results suggest that the visual system relied on a small number of objects to estimate the direction of lighting in our rendered scenes.
Social prioritisation in scene viewing and the effects of a spatial memory load
Authors: Martinez-Cedillo A. P. , Dent Kevin , Foulsham Tom 
Published: August 2023

AbstractWhen free-viewing scenes, participants tend to preferentially fixate social elements (e.g., people). In the present study, we tested whether this bias would be disrupted by increasing the demands of a secondary dual-task: holding a set of (one or six) spatial locations in memory, presented either simultaneously or sequentially. Following a retention interval, participants judged whether a test location was present in the to-be-remembered stimuli. During the retention interval participants free-viewed scenes containing a social element (a person) and a non-social element (an object) that served as regions of interest. In order to assess the impact of physical salience, the non-social element was presented in both an unaltered baseline version, and in a version where its salience was artificially increased. The results showed that the preference to look at social elements decreased when the demands of the spatial memory task were increased from one to six locations, regardless of presentation mode (simultaneous or sequential). The high-load condition also resulted in more central fixations and reduced exploration of the scene. The results indicate that the social prioritisation effect, and scene viewing more generally, can be affected by a concurrent memory load.
Investigación de un sistema fotovoltaico y la factibilidad financiera de su implementación para la generación de demanda de energía eléctrica en las instalaciones de una empresa que se dedica a la venta de vehículos, Costa Rica, 2021
Authors: campos Aráuz Mariela , Cordero Céspedes Alexander 
Published: August 2023

La presente investigación tiene como objetivo desarrollar un proyecto teórico que permita determinar la conveniencia de la utilización de energías no convencionales para satisfacer la demanda de consumo de energía eléctrica, utilizando paneles fotovoltaicos en las instalaciones de una empresa que se dedica a la venta de Vehículos, en el año 2021. Bajo este contexto es donde aplica la creación, generación y conocimiento de nuevas alternativas que se ajusten a las necesidades actuales de la sociedad, tomando como herramienta la investigación y tecnología disponibles. En este proyecto se investigará específicamente la tecnología que implica el panel fotovoltaico como generador de recurso de forma sostenible para consumo de las instalaciones, cuáles son las medidas a considerar para la implementación, las estimaciones financieras que determinaran la rentabilidad que puede generar el proyecto como tal, adicional, como estos resultados pueden influir en los flujos de caja de la empresa y los objetivos ambientales planteados en su estrategia de negocio.
KMT-2022-BLG-2397: Brown Dwarf at the Upper Shore of the Einstein Desert
Authors: Gould Andrew , Ryu Yoon-Hyun , Yee Jennifer C. , Albrow Michael D. , Chung Sun-Ju , Han Cheongho , Hwang Kyu-Ha , Jung Youn Kil , Shin In-Gu , Shvartzvald Yossi , Yang Hongjing , Zang Weicheng , Cha Sang-Mok , Kim Dong-Jin , Kim Seung-Lee , Lee Chung-Uk , Lee Dong-Joo , Lee Yongseok , Park Byeong-Gon , Pogge Richard W. ,   The KMTNet Collaboration
Published: August 2023

Abstract
We measure the Einstein radius of the single-lens microlensing event KMT-2022-BLG-2397 to be θ
E = 24.8 ± 3.6 μas, placing it at the upper shore of the Einstein Desert, 9 ≲ θ
E/μas ≲ 25, between free-floating planets (FFPs) and bulge brown dwarfs (BDs). In contrast to the six BD (25 ≲ θ
E ≲ 50) events presented by Gould et al. (2022), which all had giant-star source stars, KMT-2022-BLG-2397 has a dwarf-star source, with angular radius θ
ast ∼ 0.9 μas. This prompts us to study the relative utility of dwarf and giant sources for characterizing FFPs and BDs from finite-source point-lens (FSPL) microlensing events. We find “dwarfs” (including main-sequence stars and subgiants) are likely to yield twice as many θ
E measurements for BDs and a comparable (but more difficult to quantify) improvement for FFPs. We show that neither current nor planned experiments will yield complete mass measurements of isolated bulge BDs, nor will any other planned experiment yield as many θ
E measurements for these objects as the Korea Microlensing Telescope (KMT). Thus, the currently anticipated 10 yr KMT survey will remain the best way to study bulge BDs for several decades to come.
Rapid Quenching of Galaxies at Cosmic Noon
Authors: Park Minjung , Belli Sirio , Conroy Charlie , Tacchella Sandro , Leja Joel , Cutler Sam E. , Johnson Benjamin D. , Nelson Erica J. , Emami Razieh 
Published: August 2023

Abstract
The existence of massive quiescent galaxies at high redshift seems to require rapid quenching, but it is unclear whether all quiescent galaxies have gone through this phase and what physical mechanisms are involved. To study rapid quenching, we use rest-frame colors to select 12 young quiescent galaxies at z ∼ 1.5. From spectral energy distribution fitting, we find that they all experienced intense starbursts prior to rapid quenching. We confirm this with deep Magellan/FIRE spectroscopic observations for a subset of seven galaxies. Broad emission lines are detected for two galaxies, and are most likely caused by active galactic nucleus (AGN) activity. The other five galaxies do not show any emission features, suggesting that gas has already been removed or depleted. Most of the rapidly quenched galaxies are more compact than normal quiescent galaxies, providing evidence for a central starburst in the recent past. We estimate an average transition time of 300 Myr for the rapid quenching phase. Approximately 4% of quiescent galaxies at z = 1.5 have gone through rapid quenching; this fraction increases to 23% at z = 2.2. We identify analogs in the TNG100 simulation and find that rapid quenching for these galaxies is driven by AGNs, and for half of the cases, gas-rich major mergers seem to trigger the starburst. We conclude that these young massive quiescent galaxies are not just rapidly quenched, but also rapidly formed through a major starburst. We speculate that mergers drive gas inflow toward the central regions and grow supermassive black holes, leading to rapid quenching by AGN feedback.
Differences between the Pierre Auger Observatory and Telescope Array Spectra: Systematic Effects or Indication of a Local Source of Ultra-high-energy Cosmic Rays?
Authors: Plotko Pavlo , van Vliet Arjen , Rodrigues Xavier , Winter Walter 
Published: August 2023

Abstract
The Pierre Auger Observatory (PAO) and Telescope Array (TA) collaborations report significant differences in the observed energy spectra of ultra-high-energy cosmic rays (UHECRs) above 30 EeV. In this work we present a joint fit of TA and PAO data using the rigidity-dependent maximum energy model, including a full marginalization over all relevant parameters. We test two possible scenarios to explain these differences. One is that they are due to complex energy-dependent experimental systematics; the other is the presence of a local astrophysical source in the Northern Hemisphere, which is only visible by the TA experiment. We show that the astrophysical and systematic scenarios improve the explanation of the data equally well, compared to the scenario where both experiments observe the same UHECR flux from a cosmological source distribution and have energy-independent systematics. We test different mass compositions emitted from the local source and conclude that the data are best described by a source lying at a distance below 26 Mpc that emits cosmic rays dominated by the silicon mass group. We also discuss possible source candidates and the possible role of the putative local UHECR source in the observed TA anisotropy and in the differences in TA spectral data from different decl. bands.
The Magnetic Fields of Starburst Galaxies. I. Identification and Characterization of the Thermal Polarization in the Galactic Disk and Outflow
Authors: Lopez-Rodriguez Enrique 
Published: August 2023

Abstract
Far-infrared polarized emission by means of magnetically aligned dust grains is an excellent tracer of the magnetic fields (B-fields) in the cold phase of the galactic outflows of starburst galaxies. We present a comprehensive study of the B-fields in three nearby (3.5–17.2 Mpc) starbursts (M82, NGC 253, and NGC 2146) at 5 pc–1.5 kpc resolutions using publicly available 53–890 μm imaging polarimetric observations with Stratospheric Observatory for Infrared Astronomy/HAWC+, James Clerk Maxwell Telescope/POL-2, and ALMA. We find that the polarized spectral energy distributions (SEDs) of the full galaxies are dominated by the polarized SEDs of the outflows with dust temperatures of

T

d
,
outflow

PI

∼
45

K and an emissive index of

β

outflow

PI

∼
2.3

. The disks are characterized by low

T

d
,
disk

PI

=
[
24
,
31
]

K and

β

disk

PI

∼
1

. We show that disk- and outflow-dominated galaxies can be better distinguished by using polarized SEDs instead of total SEDs. We compute the 53–850 μm polarization spectrum of the disk and outflow, and find that dust models of the diffuse ISM can reproduce the fairly constant polarization spectrum of the disk, 〈 P
disk〉 = 1.2% ± 0.5%. The dust models of heterogenous clouds and two-temperature components are required to explain the polarization spectrum of the outflow (2%–4% at 53 μm, ∼1% at 850 μm, and a minimum within 89–154 μm). We conclude that the polarized dust grains in the outflow arise from a dust population with higher dust temperature and emissivities than those from the total flux. The B-fields of the outflows have maximum extensions within 89–214 μm reaching heights of ∼4 kpc, and have flatter polarized fluxes than total fluxes. The extension of the B-field permeating the circumgalactic medium increases as the star formation rate increases.
Reprocessing Models for the Optical Light Curves of Hypervariable Quasars from the Sloan Digital Sky Survey Reverberation Mapping Project
Authors: Akiba Tatsuya , Dexter Jason , Brandt W. N. , Ho Luis C. , Homayouni Y. , Schneider Donald P. , Shen Yue , Trump Jonathan R. 
Published: August 2023

Abstract
We explore reprocessing models for a sample of 17 hypervariable quasars, taken from the Sloan Digital Sky Survey Reverberation Mapping project, which all show coordinated optical luminosity hypervariability with amplitudes of factors ≳2 between 2014 and 2020. We develop and apply reprocessing models for quasar light curves in simple geometries that are likely to be representative of quasar inner environments. In addition to the commonly investigated thin-disk model, we include the thick-disk and hemisphere geometries. The thick-disk geometry could, for instance, represent a magnetically elevated disk, whereas the hemisphere model can be interpreted as a first-order approximation for any optically thick out-of-plane material caused by outflows/winds, warped/tilted disks, and so on. Of the 17 quasars in our sample, 11 are best-fitted by a hemisphere geometry, five are classified as thick disks, and both models fail for just one object. We highlight the successes and shortcomings of our thermal reprocessing models in case studies of four quasars that are representative of the sample. While reprocessing is unlikely to explain all of the variability that we observe in quasars, we present our classification scheme as a starting point for revealing the likely geometries of reprocessing for quasars in our sample and hypervariable quasars in general.
Sequential Small Coronal Mass Ejections Observed In Situ and in White-Light Images by Parker Solar Probe
Authors: Wood Brian E. , Hess Phillip , Chen Yu , Hu Qiang 
Published: August 2023

Abstract
We reconstruct the morphology and kinematics of a series of small transients that erupted from the Sun on 2021 April 24 using observations primarily from Parker Solar Probe (PSP). These sequential small coronal mass ejections (CMEs) may be the product of a continuous reconnection at a current sheet, which is a macroscopic example of the more microscopic reconnection activity that has been proposed to accelerate the solar wind more generally. These particular CMEs are of interest because they are the first CMEs to hit PSP and be simultaneously imaged by it, using the Wide-field Imager for Solar Probe (WISPR) instrument. Based on imaging from WISPR and STEREO-A, we identify and model six discrete transients, and determine that it is the second of them (CME2) that first hits PSP, although PSP later more obliquely also encounters the third transient. Signatures of these encounters are seen in the PSP in situ data. Within these data, we identify six candidate magnetic flux ropes (MFRs), all but one of which are associated with the second transient. The five CME2 MFRs have orientations that are roughly consistent with PSP encountering the right-hand sides of roughly E-W oriented MFRs, which are sloping back toward the Sun.
Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Lei Zhenxin , He Ruijie , Németh Péter , Zou Xuan , Xiao Huaping , Yang Yong , Zhao Jingkun 
Published: August 2023

Abstract
Masses for 664 single-lined hot subdwarf stars identified in LAMOST were calculated by comparing synthetic fluxes from spectral energy distribution with observed fluxes from a Virtual Observatory service. Three groups of hot subdwarf stars were selected from the whole sample according to their parallax precision to study the mass distributions. We found that He-poor sdB/sdOB stars present a wide mass distribution from 0.1 to 1.0 M
⊙ with a sharp mass peak at around 0.46 M
⊙, which is consistent with canonical binary model prediction. He-rich sdB/sdOB/sdO stars present a much flatter mass distribution than He-poor sdB/sdOB stars and with a mass peak at around 0.42 M
⊙. By comparing the observed mass distributions to the predictions of different formation scenarios, we concluded that the binary merger channel, including two helium white dwarfs (He-WDs) and He-WD + main-sequence mergers, cannot be the only main formation channel for He-rich hot subdwarfs, and other formation channels, such as the surviving companions from Type Ia supernovae, could also make impacts on producing this special population, especially for He-rich hot subdwarfs with masses less than 0.44 M
⊙. He-poor sdO stars also present a flatter mass distribution with an inconspicuous peak mass at 0.18 M
⊙. The similar mass–

Δ

RV

max

distribution between He-poor sdB/sdOB and sdO stars supports the scenario that He-poor sdO stars could be the subsequent evolution stage of He-poor sdB/sdOB stars.
Modeling Solids in Nuclear Astrophysics with Smoothed Particle Hydrodynamics
Authors: Sagert I. , Korobkin O. , Tews I. , Tsao B.-J. , Lim H. , Falato M. , Loiseau J. 
Published: August 2023

Abstract
Smoothed particle hydrodynamics (SPH) is a frequently applied tool in computational astrophysics to solve the fluid dynamics equations governing the systems under study. For some problems, for example when involving asteroids and asteroid impacts, the additional inclusion of material strength is necessary in order to accurately describe the dynamics. In compact stars, that is white dwarfs and neutron stars, solid components are also present. Neutron stars have a solid crust, which is the strongest material known in nature. However, their dynamical evolution, when modeled via SPH or other computational fluid dynamics codes, is usually described as a purely fluid dynamics problem. Here, we present the first 3D simulations of neutron star crustal toroidal oscillations including material strength with the Los Alamos National Laboratory SPH code FleCSPH. In the first half of the paper, we present the numerical implementation of solid material modeling together with standard tests. The second half is on the simulation of crustal oscillations in the fundamental toroidal mode. Here, we dedicate a large fraction of the paper to approaches that can suppress numerical noise in the solid. If not minimized, the latter can dominate the crustal motion in the simulations.
Three-day Forecasting of Solar Wind Speed Using SDO/AIA Extreme-ultraviolet Images by a Deep-learning Model
Authors: Son Jihyeon , Sung Suk-Kyung , Moon Yong-Jae , Lee Harim , Jeong Hyun-Jin 
Published: August 2023

Abstract
In this study, we forecast solar wind speed for the next 3 days with a 6 hr cadence using a deep-learning model. For this we use Solar Dynamics Observatory/Atmospheric Imaging Assembly 211 and 193 Å images together with solar wind speeds for the last 5 days as input data. The total period of the data is from 2010 May to 2020 December. We divide them into a training set (January–August), validation set (September), and test set (October–December), to consider the solar cycle effect. The deep-learning model consists of two networks: a convolutional layer–based network for images and a dense layer–based network for solar wind speeds. Our main results are as follows. First, our model successfully predicts the solar wind speed for the next 3 days. The rms error (RMSE) of our model is from 37.4 km s−1 (for the 6 hr prediction) to 68.2 km s−1 (for the 72 hr prediction), and the correlation coefficient is from 0.92 to 0.67. These results are much better than those of previous studies. Second, the model can predict sudden increase of solar wind speeds caused by large equatorial coronal holes. Third, solar wind speeds predicted by our model are more consistent with observations than those by the Wang–Sheely–Arge–ENLIL model, especially in high-speed-stream regions. It is also noted that our model cannot predict solar wind speed enhancement by coronal mass ejections. Our study demonstrates the effectiveness of deep learning for solar wind speed prediction, with potential applications in space weather forecasting.