bluuebunny/crossref_metadata_2025_split huggingface dataset:
Pengaruh Foot Reflexology dan Back Massage Terhadap Nilai Skor Fatique pada Pasien Hemodialisa di RSUD Kota Bekasi
Authors: Khamid Abdul , Suradika Agus , Irawati Diana , S Hentu Ardin 
Published: October 2024

End Stage Renal Disease (ESRD) menjadi salah satu penyebab kematian dinegara maju dan negara berkembang di mana permasalahan ESRD memerlukan terapi pengganti.Hemodialisis merupakan terapi yang dilakukan seumur hidup dengan frekuensi tindakan setiap 2-3 kali/minggu dan durasi yang dibutuhkan yaitu 4-5 jam dalam setiap satu sesi hemodialisis. Proses dialisis yang berkepanjangan akan menyebabkan stres dan dapat menimbulkan berbagai psikologis dan sosial yaang dapat menyebabkan gangguan psikologis. Pasien dengan hemodialisa jangka p5anjang akan menderita tekanan fisik dan mental.Fatique adalah perasaan subyektif yang tidak menyenangkan berupa keluhan yang paling sering dirasakan yaitu sebanyak 60-97% dari total pasien yang menjalani HD. Desain penelitian ini menggunakan two grup Pre post-test design dengan analisa data uji T dependen untuk data bivariat, dan distribusi frekuensi untuk data univariat sebelum dan setelah pemberian Foot Reflexology dan Back Massage di uji menggunakan instrumen Fatique Assament Scale FAS. Terdapat 48 pasien yang mengalami nilai skala fatique. Setelah diberikan intervensi terjadi penurunan nilai skala fatiqueleep sebesar 1.32 dengan pvalue < 0,00. Dapat disimpulkan bahwa Foot refleksiologi dan back massage berpengaruh dalam menurunkan nilai skor fatique.
Real-world estimation taps into basic numeric abilities
Authors: Kreis Barbara K. , Groß Julia , Pachur Thorsten 
Published: October 2024

AbstractAccurately estimating and assessing real-world quantities (e.g., how long it will take to get to the train station; the calorie content of a meal) is a central skill for adaptive cognition. To date, theoretical and empirical work on the mental resources recruited by real-world estimation has focused primarily on the role of domain knowledge (e.g., knowledge of the metric and distributional properties of objects in a domain). Here we examined the role of basic numeric abilities – specifically, symbolic-number mapping – in real-world estimation. In Experiment 1 ($$N=286$$

N
=
286

) and Experiment 2 ($$N=592$$

N
=
592

), participants first completed a country-population estimation task (a task domain commonly used to study real-world estimation) and then completed a number-line task (an approach commonly used to measure symbolic-number mapping). In both experiments, participants with better performance in the number-line task made more accurate estimates in the estimation task. Moreover, Experiment 2 showed that performance in the number-line task predicts estimation accuracy independently of domain knowledge. Further, in Experiment 2 the association between estimation accuracy and symbolic-number mapping did not depend on whether the number-line task involved small numbers (up to 1000) or large numbers that matched the range of the numbers in the estimation task (up to 100,000,000). Our results show for the first time that basic numeric abilities contribute to the estimation of real-world quantities. We discuss implications for theories of real-world estimation and for interventions aiming to improve people’s ability to estimate real-world quantities.
Manejo Quirúrgico Mínimamente Invasivo en Pólipo Juvenil no Susceptible a Resección Endoscópica, en el Hospital Pediátrico Baca Ortiz, Quito – Ecuador, Reporte de Caso
Authors: Crisrtina Sola Naranjo Md. Diana , Rodrigo Zambrano Cárdenas Dr. Esp. Eduardo , Jiménez Morejón Dr. Esp. Vinicio Xavier , María Ugazzi Betancourt Dr. Esp. Michele José 
Published: October 2024

El pólipo intestinal es un tumor que protruye desde la pared hacia la luz intestinal, pueden ser único (aislado) o múltiple. Pese a que se reporta su mayor frecuencia en varones en su primera infancia, la incidencia oscila del 1 al 2%. Se ha reportado que el 70 al 80% son de presentación única y de localización distal (colon, recto sigmoides). Clínicamente varían desde asintomáticos a cuadros de constipación o diarreas y enteropatía perdedora de proteínas, desnutrición, anemia y hemorragia gastrointestinal, entre otras. El diagnóstico se establece en la colonoscopía, endoscopia digestiva alta o cápsulas endoscópicas para establecer su localización real. El tratamiento de elección en pólipos pediculados es la exéresis de la lesión durante la endoscopia o colonoscopia, sin embargo, las lesiones de mayor tamaño y de acuerdo a sus características se prefiere la resección quirúrgica mediante abordaje abierto o por laparoscopía. En base a lo mencionado se reporta el caso de un niño de 9 años, con cuadro de rectorragias y dolor abdominal esporádico, en estudios de imagen se evidenció una lesión compatible con pólipo localizado en intestino delgado, por su tamaño y localización se le realizó resección de la lesión mediante laparoscopía, con excelentes resultados. Con lo que concluimos que las lesiones intestinales asiladas, sintomáticas deben ser estudiadas en el paciente pediátrico, para un diagnóstico y manejo oportuno, en las lesiones de mayor tamaño que de difícil resección mediante endoscopia, la laparoscopía es una adecuada opción terapéutica por las ventajas que presenta y menor riesgo de complicaciones.
3D Morphology and Motions of the Canis Major Region from Gaia DR3
Authors: Dong Yiwei , Xu Ye , Hao Chaojie , Li Yingjie , Liu Dejian , Sun Yan , Lin Zehao 
Published: October 2024

Abstract
The Canis Major (CMa) region is known for its prominent arc-shaped morphology, visible at multiple wavelengths. This study integrates molecular gas data with high-precision astrometric parameters of young stellar objects (YSOs) from Gaia DR3 to provide the first three-dimensional (3D) insights into the dynamical evolution and star formation history of the CMa region. By utilizing the average distances and proper motions of the YSOs as proxies for those of the molecular clouds (MCs), we confirm the presence of a slowly expanding shell-like morphology in the CMa region, with an estimated radius of 47 ± 11 pc and expansion velocity of 1.6 ± 0.7 km s−1. Further, the dynamical evolution of the shell supports its expansion, with an expansion timescale of ∼4.4 Myr obtained by the traceback analysis assuming constant velocities. Finally, a momentum estimate suggests that at least two supernova explosions are needed to power the observed expanding shell, reinforcing the previous hypothesis of multiple supernova events. This study effectively combines CO data with the astrometric data of YSOs from Gaia, offering significant support for future studies of the 3D morphology and kinematics of MCs.
On the Corotation of Milky Way Satellites: LMC-mass Satellites Induce Apparent Motions in Outer Halo Tracers
Authors: Garavito-Camargo Nicolás , Price-Whelan Adrian M. , Samuel Jenna , Cunningham Emily C. , Patel Ekta , Wetzel Andrew , Johnston Kathryn V. , Arora Arpit , Sanderson Robyn E. , Garrison Lehman , Horta Danny 
Published: October 2024

Abstract
Understanding the physical mechanism behind the formation of a corotating thin plane of satellite galaxies, like the one observed around the Milky Way (MW), has been challenging. The perturbations induced by a massive satellite galaxy, like the Large Magellanic Cloud (LMC), provide valuable insight into this problem. The LMC induces an apparent corotating motion in the outer halo by displacing the inner regions of the halo with respect to the outer halo. Using the Latte suite of Feedback In Realistic Environments cosmological simulations of MW-mass galaxies, we confirm that the apparent motion of the outer halo induced by the infall of a massive satellite changes the observed distribution of orbital poles of outer-halo tracers, including satellites. We quantify the changes in the distribution of orbital poles using the two-point angular correlation function and find that all satellites induce changes. However, the most massive satellites with pericentric passages between ≈30 and 100 kpc induce the largest changes. The best LMC-like satellite analog shows the largest change in orbital pole distribution. The dispersion of orbital poles decreases by 20° during the first two pericentric passages. Even when excluding the satellites brought in with the LMC-like satellite, there is clustering of orbital poles. These results suggest that in the MW, the recent pericentric passage of the LMC should have changed the observed distribution of orbital poles of all other satellites. Therefore, studies of kinematically coherent planes of satellites that seek to place the MW in a cosmological context should account for the existence of a massive satellite like the LMC.
Origin of Line Broadening in Fading Granules: Influence of Small-scale Turbulence
Authors: Ishikawa Ryohtaroh T. , Katsukawa Yukio 
Published: October 2024

Abstract
In the quiet region of the solar photosphere, turbulent convective motions of the granular flows naturally drive the subgranular-scale flows. However, evaluating such small-scale velocities is challenging because of the limited instrumental resolution. Our previous study, R. T. Ishikawa et al., found line-broadening events during the fading process of granules; however, their physical mechanism has remained unclear. In the present study, we observed the fading granules with the Hinode-SOT/SP and performed spectral line inversions. Moreover, we investigated the broadening events of synthesized spectra in fading granules reproduced by the MURaM simulation. Our results demonstrated that the small-scale turbulent motions are excited in the fading process, and such turbulent flows contribute to line broadening. The spectral line widths can be potential tracers of the photospheric turbulent flows.
Mass-transfer Outbursts Reborn: Modeling the Light Curve of the Dwarf Nova EX Draconis
Authors: Schlindwein Wagner , Baptista Raymundo 
Published: October 2024

Abstract
EX Draconis is an eclipsing dwarf nova that shows outbursts with moderate amplitude (≃2 mag) and a recurrence timescale of ≃20–30 days. Dwarf novae outbursts are explained in terms of either a thermal-viscous instability in the disc or an instability in the mass-transfer rate of the donor star (MTIM). We developed simulations of the response of accretion discs to events of enhanced mass transfer, in the context of the MTIM, and applied them to model the light curve and variations in the radius of the EX Dra disc throughout the outburst. We obtain the first modeling of a dwarf nova outburst by using χ
2 to select, from a grid of simulations, the best-fit parameters to the observed EX Dra outbursts. The observed time evolution of the system brightness and the changes in the radius of the outer disc along the outburst cycle are satisfactorily reproduced by a model of the response of an accretion disc with a viscosity parameter α = 4.0 and a quiescent mass-transfer rate

M

̇

2

(
quiescence
)
=
4.0
×

10

16

g s−1 to an event of width Δt = 6.0 × 105 s (∼7 days) where the mass-transfer rate increases to

M

̇

2

(
outburst
)
=
1.5
×

10

18

g s−1.
Systematically Measuring Ultradiffuse Galaxies. VII. The H i Survey Overview
Authors: Karunakaran Ananthan , Motiwala Khadeejah , Spekkens Kristine , Zaritsky Dennis , Donnerstein Richard L. , Dey Arjun 
Published: October 2024

Abstract
We present the results from the neutral hydrogen (H i) follow-up survey of 378 optically detected ultradiffuse galaxy (UDG) candidates from the Systematically Measuring Ultra-Diffuse Galaxies survey using the Robert C. Byrd Green Bank Telescope. We detect H i in 110 targets and determine 37 to be UDGs and 73 to be low-surface-brightness (LSB) dwarfs based on their effective radii and central surface brightnesses. In line with previous studies, we find that: (i) our H i detections have on average bluer g − r colors and more irregular morphologies than our H i nondetections, (ii) our H i detections populate the tail end of the star-forming main sequence from the ALFALFA catalog with marginally lower specific star formation rates, and (iii) H i detections are mostly in relatively isolated (i.e., field) environments, while most nondetections have at least one nearby neighbor in projection. We find that the H i mass to stellar mass ratios (i.e., gas richnesses) scale with the physical sizes for UDGs and LSB dwarfs alike, suggesting that mechanisms other than bursty star formation feedback may be at play for UDGs. However, we find a stronger trend between gas richnesses and physical sizes if we define UDGs using their effective surface brightness instead of their central surface brightness. We are in the process of using this unprecedented sample of UDG candidates to carry out detailed follow-up studies (i.e., star formation and environmental analysis, comparisons to simulations) and are obtaining resolved H i observations for several of them.
The Cumulation of Debris Clouds around a Fast-rotating Asteroid
Authors: Huang Chenyang , Yu Yang , Song Zhijun , Cheng Bin , Michel Patrick , Baoyin Hexi 
Published: October 2024

Abstract
The rotational mass loss has been realized to be a prevalent mechanism to produce low-speed debris near the asteroid, and the size composition of the asteroid’s surface regolith has been closely measured by in situ explorations. However, the full-scale evolution of the shedding debris has not been examined using the observed particle sizes, which may hold vital clues to the initial growth of an asteroid moonlet and help us to understand the general mechanisms that dominate the formation of asteroid systems. This paper presents our study on the cumulative evolution of the debris cloud formed by a rotationally unstable asteroid. A semianalytical model is developed to characterize the spatiotemporal evolution of the debris cloud posterior to a shedding event. Large-scale discrete element method (DEM) simulations are performed to quantify the clustering behavior of the debris particles in the mechanical environment near the asteroid. As a result, we found that the cumulation of a steady debris cloud is dominated by large pieces of debris, and the shedding particles follow a common migration trend, which fundamentally determines the mass distribution of the debris cloud. For the accretion analysis, we sketched the life cycle of a debris cluster and showed its dependency on particle size. The DEM simulations adopt physical parameters estimated from observations and asteroid missions. The results confirm that porous fluffy cluster structures can form shortly after a shedding event with magnitudes the same as the observed shedding activities. Measurements of these structures show that they themselves possess a certain strength and have the capacity to collisions to absorb dissociative particles that collide with them.
JWST View of Four Infant Galaxies at z = 8.31–8.49 in the MACS J0416.1−2403 Field and Implications for Reionization
Authors: Ma Zhiyuan , Sun Bangzheng , Cheng Cheng , Yan Haojing , Ling Chenxiaoji , Sun Fengwu , Foo Nicholas , Egami Eiichi , Diego José M. , Cohen Seth H. , Jansen Rolf A. , Summers Jake , Windhorst Rogier A. , D’Silva Jordan C. J. , Koekemoer Anton M. , Coe Dan , Conselice Christopher J. , Driver Simon P. , Frye Brenda , Grogin Norman A. , Marshall Madeline A. , Nonino Mario , Ortiz Rafael , Pirzkal Nor , Robotham Aaron , Ryan Russell E. , Willmer Christopher N. A. , Adams Nathan J. , Hathi Nimish P. , Dole Hervé , Willner S. P. , Espada Daniel , Furtak Lukas J. , Hsiao Tiger Yu-Yang , Li Qiong , Chen Wenlei , Jolly Jean-Baptiste , Chen Chian-Chou 
Published: October 2024

Abstract
New JWST/NIRCam wide-field slitless spectroscopy provides redshifts for four z > 8 galaxies located behind the lensing cluster MACS J0416.1−2403. Two of them, “Y1” and “JD,” have previously reported spectroscopic redshifts based on Atacama Large Millimeter/submillimeter Array measurements of [O iii] 88 μm and/or [C ii] 157.7 μm lines. Y1 is a merging system of three components, and the existing redshift z = 8.31 is confirmed. However, JD is at z = 8.34 instead of the previously claimed z = 9.28. JD’s close companion, “JD-N,” which was a previously discovered z > 8 candidate, is now identified at the same redshift as JD. JD and JD-N form an interacting pair. A new candidate at z > 8, “f090d_018,” is also confirmed and is at z = 8.49. These four objects are likely part of an overdensity that signposts a large structure extending ∼165 kpc in projected distance and ∼48.7 Mpc in radial distance. They are magnified by less than 1 mag and have an intrinsic M
UV ranging from −19.57 to −20.83 mag. Their spectral energy distributions show that the galaxies are all very young with ages ∼ 4–18 Myr and stellar masses of about 107–8
M
⊙. These infant galaxies have very different star formation rates ranging from a few to over a hundred solar masses per year, but only two of them (JD and f090d_018) have blue rest-frame UV slopes β < −2.0 indicative of a high Lyman-continuum photon escape fraction that could contribute significantly to the cosmic hydrogen-reionizing background. Interestingly, these two galaxies are the least massive and least active ones among the four. The other two systems have much flatter UV slopes largely because of their high dust extinction (A

V
= 0.9–1.0 mag). Their much lower indicated escape fractions show that even very young, actively star-forming galaxies can have a negligible contribution to reionization when they quickly form dust throughout their bodies.
Testing of UV fluorescence marking with daily recaptures of a low-mobile bush-cricket species
Authors: Varga Szabolcs , Kenyeres Zoltán 
Published: October 2024

The primary goal of developing new mark–release–recapture (MRR) methods is to make MMR more cost-effective and able to provide more information. To test the effectiveness of UV fluorescence marking, a case study was carried out on an Isophya costata population occurring in a mown grassland with a heterogeneous vegetation pattern. The marked individuals were examined daily, from the emergence of imagos until the mowing of the habitat.
The 40 marked insects (20 males and 20 females) were recaptured in 206 cases over 16 days (32.2% of the potential maximal recaptures). The finding of males was 26.2% successful, and the finding of females was 38.1% successful. Females released in shorter and sparse vegetation were recaptured more than those released in dense vegetation or than males. Recaptures showed a significant decrease during the study period in almost all groups based on Mann–Kendall trend tests. Detections were made on the upper third of the vertical structure of the vegetation in 88% of cases. In most of the detections (males: 70%, females: 62%), the axis of the insect’s body was more likely to be located vertically. The results showed that the chance of detection is significantly reduced when the position of the insect’s body is facing the axis of UV illumination. Thus, the visibility of individuals can be greatly increased by marking all sides of the body.
Using Mortality and Morbidity Conferences in Advanced Practice Nurse Education to Enhance Student Self-Efficacy
Authors: Bellinger Kayla , Nicholas Cleo , Mainwaring Jacqueline , Tobias Jane 
Published: October 2024

Background
The integration of morbidity and mortality (M and M) conferences into advanced practice nurse (APN) nursing curricula is a novel approach aimed at enhancing education, reflective learning, and continuous improvement. M and M conferences have traditionally been a standard practice for medical specialties, yet a gap exists in their utilization within APN education.

Method
A quasiexperimental pilot study with 20 student registered nurse anesthetists was conducted at a large urban academic center. The General Self-Efficacy Scale was utilized to evaluate student self-efficacy and confidence in managing adverse events.

Results

Significant improvement in self-efficacy scores (
p
= .003) postintervention indicated the educational benefits of M and M conferences. All participants reported increased confidence in navigating unexpected events.

Conclusion

The M and M conference is a valuable tool within APN education for cultivating self-efficacy and confidence in navigating adverse events.

[
J Nurs Educ
. 2024;63(X):XXX–XXX.]
La Importancia del Sistema de Vigilancia en España SiViEs Plus
Authors: Sastre María , Arroyo Virginia , Cabezas Cristina , Olivares David , Puerto Ana , Cano Rosa 
Published: October 2024

Vivimos en una época donde la Salud Pública enfrenta desafíos constantes, la implementación de sistemas de vigilancia epidemiológica es clave. Uno de estos sistemas es SiViEs Plus, el Sistema para Vigilancia en España, que se ha convertido en una herramienta fundamental para la descripción del patrón epidemiológico y control de las enfermedades transmisibles. Es una nueva plataforma versátil y atractiva que puede satisfacer de manera avanzada todas las necesidades relacionadas con el tratamiento, análisis y gestión de información epidemiológica en el nivel nacional, independientemente de la enfermedad.
La flexibilidad de la plataforma radica en que el Centro Nacional de Epidemiología (CNE) es capaz de gestionar de manera independiente todo el sistema: creación de fichas para enfermedades nuevas, modificación de fichas para adaptar las enfermedades ya existentes a nuevos protocolos, creación de nuevos códigos, creación de periodos de consolidación, gestionar usuarios (altas, bajas, cambios en los datos de los usuarios).
Además, los datos alojados y gestionados por SIVIES Plus se envían al Centro Europeo para la Prevención y el Control de Enfermedades (ECDC) a través del portal europeo de vigilancia de enfermedades infecciosas EpiPulse, siguiendo el calendario de recogida de datos que establece el ECDC, como centro coordinador de la vigilancia epidemiológica en la Unión Europea.
Sin embargo, es importante recordar que el éxito de SiViEs Plus depende de la participación activa de sus usuarios. El trabajo conjunto del CNE, las comunidades y ciudades autónomas y los diferentes ministerios, es clave para mejorar la calidad de la información a la hora de notificar los casos de enfermedades que se vigilan en el ámbito nacional. Solo a través de un esfuerzo conjunto podremos fortalecer este sistema y garantizar una respuesta adecuada en las decisiones e intervenciones en el ámbito de la salud pública.
En conclusión, SiViEs Plus representa un avance significativo en la vigilancia epidemiológica, pero su éxito depende de la colaboración y el compromiso de todos.

El equipo de SiViEs quiere agradecer el trabajo y esfuerzo de todos los usuarios del sistema.