bluuebunny/crossref_metadata_2025_split huggingface dataset:
Criterios para el Diseño de un Currículo Incluyente de la Diversidad de una Comunidad Educativa
Authors: Vela Neiva Jairo Alfonso 
Published: February 2024

A partir de la identificación de la educación como un proceso multidireccional mediante el cual se transmiten conocimientos, valores, costumbres y formas de actuar, pero que, no obstante, ha sido instrumentalizada como forma de colonización y dominación, en la presente investigación se analiza la nueva tendencia mundial orientada por la necesidad de consolidar, en el contexto de las políticas educativas, elementos transversales que propicien la inclusión educativa, la cual debe fortalecerse en todos los niveles educativos, la implementación de currículos flexibles en los que se integre de manera inclusiva diferentes lógicas, saberes, prácticas y modos distintos y diversos de pensar, actuar y vivir de los integrantes del sistema educativo. En el presente artículo de revisión se analiza la posibilidad de diseñar un currículo que reformule las áreas del saber en términos de intereses, realidades y versatilidad en el mundo actual, y que sirva de paradigma con el que diferentes comunidades, con lógicas, saberes, prácticas y modos distintos y diversos de pensar, actuar y vivir, encuentren en la educación la comprensión y proyección de su propia significación, sentido e identidad colectiva, consolidando así criterios para el diseño de un currículo incluyente de la diversidad de una comunidad educativa; proceso que comprende, desde la formación docente y la capacitación de los docentes como punto de partida para garantizar una Educación Inclusiva de calidad, el fortalecimiento la educación rural y la educación y tecnología al servicio de los niños con diversidad de potencialidades y necesidades o dificultades de aprendizaje. Los resultados apuntan a la necesidad de diseñar e implementar acciones para que el currículo brinde la adecuación, cohesión y coherencia de los programas planteados para cada región, según sea su cultura, campo productivo, intereses o tipo de habitantes, lo cual depende, en gran medida, de que pueda garantizarse que los profesores sean personas competentes, que su enseñanza sea de calidad y que todos los estudiantes tengan acceso a una docencia de excelente calidad.
HUBUNGAN BEBAN KERJA, MOTIVASI, DAN KOMPENSASI DENGAN KINERJA TENAGA KEPERAWATAN DI RUMAH SAKIT UMUM DEWISARTIKA KENDARI TAHUN 2023
Authors: Muhaymin Muhaymin , Yuniar Nani , Lestari Hariati 
Published: February 2024

Abstrak
Latar Belakang: Tenaga keperawatan merupakan ujung tombak dalam memberikan pelayanan perawatan bagi pasien di rumah sakit, sebagai faktor yang berhubungan langsung dengan pasien dalam waktu yang lama. Rekapan absensi di RSU Dewi Sartika Kendari pada tiga bulan awal tahun 2023 tingkat keterlambatan setiap bulannya mengalami kenaikan, yaitu pada Januari sebanyak 38%, Februari sebanyak 46%, dan Maret sebanyak 48%. Dengan keterlambatan kehadiran tenaga keperawatan ini berakibat pada penurunan kinerja tenaga keperawatan.
Tujuan: Mengetahui hubungan antara beban kerja, motivasi, dan kompensasi dengan kinerja tenaga keperawatan di RSU Dewi Sartika Kendari tahun 2023.
Metode: Jenis penelitian ini merupakan penelitian kuantitatif dengan rancangan cross sectional study. Teknik pengambilan sampel yaitu total sampling, dengan sampel sebanyak 74 responden sesuai dengan jumlah populasi.
Hasil: Menunjukan bahwa ada hubungan antara beban kerja dengan kinerja dengan nilai p=0,000 (p
FAKTOR YANG BERHUBUNGAN DENGAN KEIKUTSERTAAN MASYARAKAT SEBAGAI PESERTA BPJS MANDIRI DIWILAYAH KERJA PUSKESMAS ABELI TAHUN 2023
Authors: Dewi Nilam Shari , Suhadi Suhadi , Kalza Lade Albar 
Published: February 2024

Abstrak
Latar Belakang: Berdasarkan data langsung dari Puskesmas Abeli bahwa kepesertaan BPJS Mandiri dari tahun 2021 sebanyak 774 jiwa menurun pada tahun 2022 menjadi 734 jiwa.

Tujuan: Tujuan penelitian ini adalah untuk mengetahui Faktor Yang Berhubungan Dengan Keikutsertaan Masyarakat Sebagai Peserta BPJS Mandiri Di Wilayah Kerja Puskesmas Abeli Tahun 2023.

Metode: Jenis penelitian yang digunakan pada penelitian ini adalah penelitian kuantitatif dengan desain cross sectional study. Jumlah sampel pada penelitian ini 84 responden.

Hasil: Hasil penelitian ini menunjukan bahwa ada hubungan antara pengetahuan dengan keikutsertaan menjadi peserta BPJS Mandiri dengan nilai (value =0,001 < 0,05), tidak ada hubungan antara pendapatan dengan keikutsertaan menjadi peserta BPJS Mandiri dengan nilai (value =0,349 > 0,05), dan tidak ada hubungan antara sikap dengan keikutsertaan menjadi peserta BPJS Mandiri dengan nilai (value =0,467 > 0,05).

Kesimpulan: Kesimpulan penelitian ini yaitu ada hubungan yang signifikan antara pengetahuan dengan kepesertaan BPJS Mandiri, dan tidak terdapat hubungan antarapendapatan dan sikap dengan keikut sertaan menjadi peserta BPJS Mandiri di wilayah kerja Puskesmas Abeli Tahun 2023.

Abstract
Background: Based on direct data from the Abeli health center, BPJS Mandiri membership from 2021 was 774 people decreased in 2022 to 734 people.

Methods: study using a cross sectional study design. The number of samples was 84 people.

Results: The results of the study there is a relationship between knowledge and partisipation in BPJS Mandiri (value = 0.001 < 0,05), there is no relationship between income and the participation of BPJS Mandiri (value = 0.349 > 0,05) and there is no relationship between attitude and the participation of BPJS Mandiri (value = 0.467 > 0,05) in this study related to community participation as participants of BPJS Mandiri.

Conclusion: the conclusions of this study is that there is a significant relationship between knowledge and community participantion as BPJS Mandiri, and there is no relationship between income, and attitude and community participantion as BPJS Mandiri participants in the working area of the Abeli Community Health Center in 2023.
Haze Optical Depth in Exoplanet Atmospheres Varies with Rotation Rate: Implications for Observations
Authors: Cohen Maureen , Palmer Paul I. , Paradise Adiv , Bollasina Massimo A. , Tiranti Paola Ines 
Published: February 2024

Abstract
Transmission spectroscopy supports the presence of uncharacterized, light-scattering and -absorbing hazes in the atmospheres of many exoplanets. The complexity of factors influencing the formation, 3D transport, radiative impact, and removal of hazes makes it challenging to match theoretical models to the existing data. Our study simplifies these factors to focus on the interaction between planetary general circulation and haze distribution at the planetary limb. We use an intermediate-complexity general circulation model, ExoPlaSim, to simulate idealized organic haze particles as radiatively active tracers in the atmospheres of tidally locked terrestrial planets for 32 rotation rates. We find three distinct 3D spatial haze distributions, corresponding to three circulation regimes, each with a different haze profile at the limb. All regimes display significant terminator asymmetry. In our parameter space, super-Earth-sized planets with rotation periods greater than 13 days have the lowest haze optical depths at the terminator, supporting the choice of slower rotators as observing targets.
An Optical Search for New Outbursting Low Mass X-Ray Binaries
Authors: Wang Yuankun , Bellm Eric C. , Crossland Allison , Clarkson William I. , Mazzi Alessandro , Riddle Reed , Laher Russ R. , Rusholme Ben 
Published: February 2024

Abstract
Transient low-mass X-ray binaries (LMXBs) are discovered largely by X-ray and gamma-ray all-sky monitors. The X-ray outburst is also accompanied by an optical brightening, which empirically can precede the detection of X-rays. Newly sensitive optical synoptic surveys may offer a complementary pathway for discovery and potential for insight into the initial onset and propagation of the thermal instability that leads to the ionization of the accretion disk. We use the Zwicky Transient Facility (ZTF) alert stream to perform a comprehensive search at optical wavelengths for previously undiscovered outbursting LMXBs. Our pipeline first crossmatches the positions of the alerts to cataloged X-ray sources, and then analyzes the 30 day lightcurve of matched alerts by thresholding on differences with an 8 day exponentially weighted moving average. In addition to a 19 month long live search, we ran our pipeline over 4 yr of ZTF archival data, recovering four known LMXBs. We also independently detected an outburst of MAXI J1957+032 in the live search and found the first outburst of Swift J1943.4+0228, an unclassified X-ray transient, in 10 yr. Using Monte Carlo simulations of the Galactic LMXB population, we estimate that 29% of outbursting LMXBs are detectable by ZTF and that 4.4% of LMXBs would be present in the crossmatched X-ray catalogs, giving an estimated Galactic population of

3390

−
1930

+
3980

. We estimate that our current pipeline can detect 1.3% of all outbursting LMXBs, including those previously unknown, but that Rubin Observatory’s Legacy Survey of Space and Time will be able to detect 43% of outbursting LMXBs.
Disentangling CO Chemistry in a Protoplanetary Disk Using Explanatory Machine-learning Techniques
Authors: Diop Amina , Cleeves L. Ilsedore , Anderson Dana E. , Pegues Jamila , Plunkett Adele 
Published: February 2024

Abstract
Molecular abundances in protoplanetary disks are highly sensitive to the local physical conditions, including gas temperature, gas density, radiation field, and dust properties. Often multiple factors are intertwined, impacting the abundances of both simple and complex species. We present a new approach to understanding these chemical and physical interdependencies using machine learning. Specifically, we explore the case of CO modeled under the conditions of a generic disk and build an explanatory regression model to study the dependence of CO spatial density on the gas density, gas temperature, cosmic-ray ionization rate, X-ray ionization rate, and UV flux. Our findings indicate that combinations of parameters play a surprisingly powerful role in regulating CO abundance compared to any singular physical parameter. Moreover, in general we find the conditions in the disk are destructive toward CO. CO depletion is further enhanced in an increased cosmic-ray environment and in disks with higher initial C/O ratios. These dependencies uncovered by our new approach are consistent with previous studies, which are more modeling intensive and computationally expensive. Our work thus shows that machine learning can be a powerful tool not only for creating efficient predictive models, but also for enabling a deeper understanding of complex chemical processes.
Small-amplitude Compressible Magnetohydrodynamic Turbulence Modulated by Collisionless Damping in Earth’s Magnetosheath: Observation Matches Theory
Authors: Zhao Siqi , Yan Huirong , Liu Terry Z. , Yuen Ka Ho , Shi Mijie 
Published: February 2024

Abstract
Plasma turbulence is a ubiquitous dynamical process that transfers energy across many spatial and temporal scales and affects energetic particle transport. Recent advances in the understanding of compressible magnetohydrodynamic (MHD) turbulence demonstrate the important role of damping in shaping energy distributions on small scales, yet its observational evidence is still lacking. This study provides the first observational evidence of substantial collisionless damping (CD) modulation on the small-amplitude compressible MHD turbulence cascade in Earth’s magnetosheath using four Cluster spacecraft. Based on an improved compressible MHD decomposition algorithm, turbulence is decomposed into three eigenmodes: incompressible Alfvén modes and compressible slow and fast (magnetosonic) modes. Our observations demonstrate that CD enhances the anisotropy of compressible MHD modes because CD has a strong dependence on wave propagation angle. The wavenumber distributions of slow modes are mainly stretched perpendicular to the background magnetic field (
B

0) and weakly modulated by CD. In contrast, fast modes are subjected to a more significant CD modulation. Fast modes exhibit a weak, scale-independent anisotropy above the CD truncation scale. Below the CD truncation scale, the anisotropy of fast modes enhances as wavenumbers increase. As a result, fast-mode fractions in the total energy of compressible modes decrease with the increase of perpendicular wavenumber (to
B

0) or wave propagation angle. Our findings reveal how the turbulence cascade is shaped by CD and its consequences for anisotropies in the space environment.
The EDGE-CALIFA Survey: Molecular Gas and Star Formation Activity across the Green Valley
Authors: Villanueva Vicente , Bolatto Alberto D. , Vogel Stuart N. , Wong Tony , Leroy Adam K. , Sánchez Sebastian F. , Levy Rebecca C. , Rosolowsky Erik , Colombo Dario , Kalinova Veselina , Cronin Serena , Teuben Peter , Rubio Mónica , Bazzi Zein 
Published: February 2024

Abstract
We present a 12CO(J = 2−1) survey of 60 local galaxies using data from the Atacama Compact Array as part of the Extragalactic Database for Galaxy Evolution: the ACA EDGE survey. These galaxies all have integral field spectroscopy from the CALIFA survey. Compared to other local galaxy surveys, ACA EDGE is designed to mitigate selection effects based on CO brightness and morphological type. Of the 60 galaxies in ACA EDGE, 36 are on the star formation main sequence, 13 are on the red sequence, and 11 lie in the “green valley” transition between these sequences. We test how star formation quenching processes affect the star formation rate (SFR) per unit molecular gas mass, SFEmol = SFR/M
mol, and related quantities in galaxies with stellar masses 10 ≤ log[M
⋆/M
⊙] ≤ 11.5 covering the full range of morphological types. We observe a systematic decrease of the molecular-to-stellar mass fraction (

R

⋆

mol

) with a decreasing level of star formation activity, with green valley galaxies also having lower SFEmol than galaxies on the main sequence. On average, we find that the spatially resolved SFEmol within the bulge region of green valley galaxies is lower than in the bulges of main-sequence galaxies if we adopt a constant CO-to-H2 conversion factor, α
CO. While efficiencies in main-sequence galaxies remain almost constant with galactocentric radius, in green valley galaxies, we note a systematic increase of SFEmol,

R

⋆

mol

, and specific SFR with increasing radius. As shown in previous studies, our results suggest that although gas depletion (or removal) seems to be the most important driver of the star formation quenching in galaxies transiting through the green valley, a reduction in star formation efficiency is also required during this stage.
Aggregation and Charging of Mineral Cloud Particles under High-energy Irradiation
Authors: Bach-Møller Nanna , Helling Christiane , Jørgensen Uffe G. , Enghoff Martin B. 
Published: February 2024

Abstract
It is known from Earth that ionizing high-energy radiation can lead to ion-induced nucleation of cloud condensation nuclei in the atmosphere. Since the amount of high-energy radiation can vary greatly based on the radiative environment of a host star, understanding the effect of high-energy radiation on cloud particles is critical to understand exoplanet atmospheres. This study aims to explore how high-energy radiation affects the aggregation and charging of mineral cloud particles. We present experiments conducted in an atmosphere chamber on mineral SiO2 particles with diameters of 50 nm. The particles were exposed to gamma radiation in either low-humidity (RH ≈ 20%) or high-humidity (RH > 50%) environments. The aggregation and charging state of the particles were studied with a scanning mobility particle sizer. We find that the single SiO2 particles (N1) cluster to form larger aggregates (N2–N4), and that this aggregation is inhibited by gamma radiation. We find that gamma radiation shifts the charging of the particles to become more negative by increasing the charging state of negatively charged particles. Through an independent t-test, we find that this increase is statistically significant within a 5% significance level for all aggregates in the high-humidity environment and all except the N1 particles in the low-humidity environment. For the positively charged particles, the changes in charging state are not within the 5% significance level. We suggest that the overall effect of gamma radiation could favor the formation of a high number of small particles over a lower number of larger particles.
Formation of Galactic Disks. I. Why Did the Milky Way’s Disk Form Unusually Early?
Authors: Semenov Vadim A. , Conroy Charlie , Chandra Vedant , Hernquist Lars , Nelson Dylan 
Published: February 2024

Abstract
Recent results from spectroscopic and astrometric surveys of nearby stars suggest that the stellar disk of our Milky Way (MW) was formed quite early, within the first few billion years of its evolution. Chemokinematic signatures of disk formation in cosmological zoom-in simulations appear to be in tension with these data, implying that MW-like disk formation is delayed in simulations. We investigate the formation of galactic disks using a representative sample of MW-like galaxies from the cosmological volume simulation TNG50. We find that on average MW-mass disks indeed form later than the local data suggest. However, their formation time and metallicity exhibit a substantial scatter, such that ∼10% of MW-mass galaxies form disks early, similar to the MW. Thus, although the MW is unusual, it is consistent with the overall population of MW-mass disk galaxies. The direct MW analogs assemble most of their mass early, ≳10 Gyr ago, and are not affected by destructive mergers after that. In addition, these galaxies form their disks during the early enrichment stage when the interstellar medium metallicity increases rapidly, with only ∼25% of early-forming disks being as metal-poor as the MW was at the onset of disk formation, [Fe/H] ≈ −1.0. In contrast, most MW-mass galaxies either form disks from already enriched material or experience late destructive mergers that reset the signatures of galactic disk formation to later times and higher metallicities. Finally, we also show that earlier disk formation leads to more dominant rotationally supported stellar disks at redshift zero.
Multiple Habitable Phases on Outer Exosolar Worlds
Authors: Sparrman Viktor , Bladh Sara , Way M. J. 
Published: February 2024

Abstract
As stars evolve to higher luminosities during first ascension of the giant branch, previously frozen terrestrial worlds may thaw and host liquid water on their surfaces. Eventually these outer worlds again become uninhabitable due to receiving too much incident light and their water inventory evaporating. Solar-mass stars experience a sudden decrease in luminosity entering the horizontal branch, which could result in a secondary habitable phase for their outer worlds. The outer worlds’ time with habitable surface climates is key in evaluating the possibility of extraterrestrial life arising. The times inside the habitable zone (TIHZ) are calculated for outer worlds orbiting between 5 and 45 au around a Sun-like star. By comparing the TIHZ to time estimates for life to arise on Earth, we evaluate whether such outer worlds are promising candidates in the search for extraterrestrial life. We use two different solar evolution models (PARSEC and Dartmouth) and both optimistic and conservative habitable zone (HZ) definitions. Multiple habitable phases are found for each outer world. Outer worlds with orbits as large as Saturn are found to have a secondary habitable phase which exceeds the first in duration. Generally, the time inside the HZ is found to decrease almost monotonically with orbiting distance. Water loss is calculated after the first habitable phase to determine whether a secondary habitable phase is possible. For all orbiting distances the water loss is insufficient to deplete a water inventory equivalent to that of many moons in the outer solar system.
Updated Proper Motion of the Neutron Star in the Supernova Remnant Cassiopeia A
Authors: Holland-Ashford Tyler , Slane Patrick , Long Xi 
Published: February 2024

Abstract
In this paper, we present updated estimates of the velocity of the neutron star (NS) in the supernova remnant Cassiopeia A using over two decades of Chandra observations. We use two methods: (1) recording the NS positions from dozens of Chandra observations, including the astrometric uncertainty estimates on the data points, but not correcting the astrometry of the observations; and (2) correcting the astrometry of the 13 Chandra observations that have a sufficient number of point sources with identified Gaia counterparts. For method #1, we observe a heliocentric velocity of 275 ± 121 km s−1, with an angle of 177° ± 22° east of north. For method #2, we observe a heliocentric velocity of 436 ± 89 km s−1 at an angle of 158° ± 12°. Correcting for galactic rotation and the Sun’s peculiar motion decreases these estimates to 256 km s−1 at 167° and 433 km s−1 at 151°, respectively. Both of our estimates match with the explosion-center-estimated velocity of ∼350 km s−1 and the previous 10 yr baseline proper-motion measurement of 570 ± 260 km s−1, but our use of additional data over a longer baseline has led to a smaller uncertainty by a factor of 2–3. Our estimates rule out velocities ≳600 km s−1 and better match with simulations of Cassiopeia A that include NS kick mechanisms.
The Orbital Structure and Selection Effects of the Galactic Center S-star Cluster
Authors: Burkert A. , Gillessen S. , Lin D. N. C. , Zheng X. , Schoeller P. , Eisenhauer F. , Genzel R. 
Published: February 2024

Abstract
The orbital distribution of the S-star cluster surrounding the supermassive black hole in the center of the Milky Way is analyzed. A tight dependence of the pericenter distance r
p on orbital eccentricity e
⋆ is found,

log
(

r
p

)
∼
(
1
−

e
⋆

)

, which cannot be explained simply by a random distribution of semimajor axis and eccentricities. No stars are found in the region with high e
⋆ and large

log
(

r
p

)

or in the region with low e
⋆ and small

log
(

r
p

)

. Although the sample is still small, the G-clouds show a very similar distribution. The likelihood

P
(
log
(

r
p

)
,
(
1
−

e
⋆

)
)

to determine the orbital parameters of S-stars is determined. P is very small for stars with large e
⋆ and large

log
(

r
p

)

. S-stars might exist in this region. To determine their orbital parameters, one however needs observations over a longer time period. On the other hand, if stars would exist in the region of low

log
(

r
p

)

and small e
⋆, their orbital parameters should by now have been determined. That this region is unpopulated therefore indicates that no S-stars exist with these orbital characteristics, providing constraints for their formation. We call this region, defined by

log
(

r
p

/
AU
)
<
1.57
+
2.6
(
1
−

e
⋆

)

, the zone of avoidance. Finally, it is shown that the observed frequency of eccentricities and pericenter distances is consistent with a random sampling of

log
(

r
p

)

and e
⋆ if one takes into account the fact that no stars exist in the zone of avoidance and that orbital parameters cannot yet be determined for stars with large r
p and large e
⋆.