bluuebunny/crossref_metadata_2025_split huggingface dataset:
HUBUNGAN DUKUNGAN KELUARGA DENGAN KEPATUHAN MINUM OBAT ANTI TUBERKULOSIS (OAT) PADA PENDERITA PENYAKIT TUBERKULOSIS PARU DI PUSKESMAS MARIDAN KABUPATEN PENAJAM PASER UTARA
Authors: Suwanto Suwanto , Rusdi Rusdi , Kori Pasola Sarnica 
Published: November 2024

Latar Belakang : Tuberkulosis penyakit yang disebabkan Mycobacterium tuberculosis yang sampai saat ini menjadi masalah kesehatan masyarakat di dunia. Tuberkulosis (TBC) disebabkan oleh sejenis bakteri yang disebut mycobacterium tuberculosis. Penyakit ini menyebar saat penderita TB batuk atau bersin dan orang lain menghirup droplet yang dikeluarkan yang mengandung bakteri TB. Dukungan keluarga sangat diperlukan terutama pada penderita TB yang mengharuskan mengkonsumsi obat dengan jangka waktu yang lama. Untuk mencapai kesembuhan diperlukan keteraturan atau kepatuhan berobat bagi setiap penderita. Tujuan : untuk mengetahui hubungan dukungan keluarga dengan kepatuhan minum obat pada pasien TBC di Puskesmas Maridan. Metode : penelitian ini menggunakan kuantitatif dengan desain cross sectional. Analisis menggunakan uji Chi-square pada 52 pasien TBC di Puskesmas Maridan sebagai responden yang dilakukan pada bulan Mei 2024. Hasil : penelitian didapatkan pasien yang tidak patuh dengan dukungan keluarga kurang yaitu 6 (9,8%) dan pasien yang patuh 7 (11,2%), sedangkan pasien yang tidak patuh dengan dukungan keluarga baik yaitu 11 (22,9%) dan pasien yang patuh 28 (56,1%). Didapatkan (p=0,232) tidak adanya hubungan antara dukungan keluarga dengan kepatuhan minum obat pada pasien TBC di Puskesmas Maridan sama halnya dengan dukungan penghargaan (p=0,779), dukungan informasi (p=0,363) dan dukungan instrumental (p=0,494), tetapi berbeda dengan dukungan emosional (p=0,008) terdapat hubungan dengan kepatuhan minum obat. Kesimpulan : Kepatuhan minum obat tidak di pengaruhi oleh dukungan keluarga tetapi pada dukungan emosional mempengaruhi kepatuhan minum obat sedangkan pada dukungan penghargaan, dukungan informasi dan dukungan instrumental tidak mempengaruhi kepatuhan minum obat pada pasien TBC.
Improving Vehicle Detection in Challenging Datasets: YOLOv5s and Frozen Layers Analysis
Authors: Yuma Rafi Ahmad Nanda , Yusuf Mohamad 
Published: November 2024

Small datasets and imbalanced classes often cause problems when it used as primary research material. In case of classification and object detection, some researchers proposed Transfer Learning (TF) with several frozen layers. Moreover, YOLO (You Only Look Once) is one of the algorithms that works in real-time object detection. In this research, we focused on evaluating the YOLOv5s version of detecting vehicles in small and imbalanced datasets. The original YOLOv5s were trained and compared with YOLOv5s with freezing layers method (10 and 24 frozen layers). The experimental results of original YOLOv5s were precision score of 0.779, recall value of 0.933, mAP@0.5 of 0.93 and mAP@0.5:0.95 of 0.684 while YOLOv5s with 10 frozen layers where precision score was decreased to 0.639, but the other value increase with recall value of 0.939, mAP@0.5 of 0.951 and mAP@0.5:0.95 of 0.732. Overall, the version with 10 frozen layers demonstrated superior performance in addressing the challenges of small and imbalanced datasets, particularly excelling in recall and mAP metrics.
The Impact of Gender Stereotypes and Self-Efficacy on the Glass Ceiling Phenomenon in the Religious Affairs Office of Purwakarta Regency
Authors: Kurniasih Nia , Hayati Neuneung Ratna 
Published: November 2024

This study aimed at gender stereotypes and self-efficacy as determinants of the glass ceiling effect. Data was collected through questionnaires distributed to employees in the office. The linear regression analysis method is used to analyze the data. Office of the Ministry of Religious Affairs of Purwakarta District. The results showed that Gender Streotypes partially had a significant influence on Glass Ceiling, Self-Efficacy had a significant influence on Glass Ceiling. The implications of these findings are discussed in the context of the Importance of addressing Gender Stereotypes in the workplace: Organizations need to be aware of the impact of Gender Stereotypes on the Glass Ceiling and take steps to reduce or eliminate those stereotypes
EFEITOS DA REABILITAÇÃO FÍSICA NO RISCO DE QUEDAS E NA QUALIDADE DE VIDA DE IDOSOS: UMA REVISÃO DE LITERATURA
Authors: Moraes Mayk Kevin Lobo , Nascimento Ana Beatriz Vicente do , Oliveira Jhennefer Teles , Reis Mariete Freitas dos , Souza Leonardo Brynne Ramos de 
Published: November 2024

Objetivo: analisar a eficácia de protocolos de reabilitação física contra quedas em idosos. Métodos: trata-se de uma revisão de literatura, que abrangeu estudos observacionais, que utilizaram intervenções fisioterapêuticas em idosos, publicados entre 2018 e 2023, indexados nas bases de dados PUBMed, Scielo, Lilacs e BIREME em inglês e português. Os artigos incluídos foram avaliados pelo Checklist STROBE. Resultados: um total de 2.534 artigos foram encontrados com a busca. Porém, sete artigos foram selecionados ao final do processo de revisão, os quais todos cumpriram mais de 50% das exigências do Checklist STROBE. Para todas as intervenções selecionadas, houve resultados estatisticamente significativos, favorecendo as intervenções fisioterapêuticas de fortalecimento nas amostras de cada estudo, com protocolos promovendo ganhos em variáveis físicas e fatores de risco para quedas. Conclusão: Conclui-se que a intervenção fisioterapêutica se mostrou uma abordagem eficaz na prevenção de quedas e, portanto, é essencial em programas para reduzir o risco de quedas.
Analysis of Factors Influencing Agricultural Commercialisation Among Youth Group in Agricultural Output Market: Empirical Evidence from Mwanza City and Ukerewe Districts, Tanzania
Authors: Kilamlya Jacob , Mhina Juma Almasi , Regnard Irene Joseph 
Published: November 2024

Although agriculture has great potential for Sub-Saharan Africa particularly in the creation of decent jobs for youth, the youth are less attracted and reluctant to pursue agriculture as both a career and activity for livelihood due to several aspects. For this reason, the study examined the Agricultural Commercialisation among youth groups in the agricultural Output Market in the Mwanza region, Tanzania. The cross-sectional study used a quantitative and qualitative approach and included ninety-three (93) youth groups from two selected Districts (Mwanza City and Ukerewe District) Data were analyzed with the Commercialisation Index and Tobit Regression Model with the aid of statistical tools for analysis which were R-Software (Ri3863.6.1) and SPSS version 20. The results showed that the commercialisation index for this study is about 79.4 %, then empowered youth groups were highly participating in the agricultural output market for both Mwanza City and Ukerewe District. This justifies the assumption of the Commercialisation Index (CI) when CI is greater than 50% of farmers are considered they be commercial oriented which in other words they participate in agricultural output markets. Moreover, the degree of participation in agricultural output among empowered youth groups was also influenced by market experience, market arrangement and market infrastructure. The participation of empowered youth groups from both agricultural output markets seemed also to be determined by the education level of group leaders. Youth groups in which their leaders had attained diploma education level had less participation in the agricultural output market as compared to groups with leaders who attained primary school education level
Self-consistent Strong Screening Applied to Thermonuclear Reactions
Authors: Grayson Christopher , Yang Cheng Tao , Formanek Martin , Rafelski Johann 
Published: November 2024

Abstract
Self-consistent strong plasma screening around light nuclei is implemented in the Big Bang nucleosynthesis (BBN) epoch to determine the short-range screening potential, e
ϕ(r)/T ≥ 1, relevant for thermonuclear reactions. We numerically solve the nonlinear Poisson–Boltzmann equation incorporating Fermi–Dirac statistics, adopting a generalized screening mass to find the electric potential in the cosmic BBN electron–positron plasma for finite-sized α particles (4He++) as an example. Although the plasma follows Boltzmann statistics at large distances, Fermi–Dirac statistics is necessary when work performed by ions on electrons is comparable to their rest-mass energy. While self-consistent strong screening effects are generally minor owing to the high BBN temperatures, they can enhance the fusion rates of high-Z (Z > 2) elements while leaving fusion rates of lower-Z (Z ≤ 2) elements relatively unaffected. Our results also reveal a pronounced spatial dependence of the self-consistent strong screening potential near the nuclear surface. These findings about the electron–positron plasma’s role refine BBN theory predictions and offer broader applications for studying weakly coupled plasmas in diverse cosmic and laboratory settings.
The ALMA-CRISTAL Survey: Spatially Resolved Star Formation Activity and Dust Content in 4 < z < 6 Star-forming Galaxies
Authors: Li Juno , Da Cunha Elisabete , González-López Jorge , Aravena Manuel , De Looze Ilse , Förster Schreiber N. M. , Herrera-Camus Rodrigo , Spilker Justin , Tadaki Ken-ichi , Barcos-Munoz Loreto , Battisti Andrew J. , Birkin Jack E. , Bowler Rebecca A. A. , Davies Rebecca , Díaz-Santos Tanio , Ferrara Andrea , Fisher Deanne B. , Hodge Jacqueline , Ikeda Ryota , Killi Meghana , Lee Lilian , Liu Daizhong , Lutz Dieter , Mitsuhashi Ikki , Naab Thorsten , Posses Ana , Relaño Monica , Solimano Manuel , Übler Hannah , van der Giessen Stefan Anthony , Villanueva Vicente 
Published: November 2024

Abstract
Using a combination of Hubble Space Telescope (HST), JWST, and Atacama Large Millimeter/submillimeter Array (ALMA) data, we perform spatially resolved spectral energy distributions (SED) fitting of fourteen 4 < z < 6 ultraviolet (UV)-selected main-sequence galaxies targeted by the ALMA Large Program [C ii] Resolved ISM in Star-forming Galaxies. We consistently model the emission from stars and dust in ∼0.5–1 kpc spatial bins to obtain maps of their physical properties. We find no offsets between the stellar masses (M
*) and star formation rates (SFRs) derived from their global emission and those from adding up the values in our spatial bins, suggesting there is no bias of outshining by young stars on the derived global properties. We show that ALMA observations are important to derive robust parameter maps because they reduce the uncertainties in L
dust (hence, AV
and SFR). Using these maps, we explore the resolved star-forming main sequence for z ∼ 5 galaxies, finding that this relation persists in typical star-forming galaxies in the early Universe. We find less obscured star formation where the M
* (and SFR) surface densities are highest, typically in the central regions, contrary to the global relation between these parameters. We speculate this could be caused by feedback driving gas and dust out of these regions. However, more observations of IR luminosities with ALMA are needed to verify this. Finally, we test empirical SFR prescriptions based on the UV+IR and [C ii] line luminosity, finding they work well at the scales probed (approximately kiloparsec). Our work demonstrates the usefulness of joint HST-, JWST-, and ALMA-resolved SED modeling analyses at high redshift.
The Ancient Star Formation History of the Extremely Low-mass Galaxy Leo P: An Emerging Trend of a Post-reionization Pause in Star Formation
Authors: McQuinn Kristen B. W. , Newman Max J. B. , Skillman Evan D. , Telford O. Grace , Brooks Alyson , Adams Elizabeth A. K. , Berg Danielle A. , Boyer Martha L. , Cannon John M. , Dolphin Andrew E. , Pahl Anthony J. , Rhode Katherine L. , Salzer John J. , Cohen Roger E. , Goldman Steve R. 
Published: November 2024

Abstract
Isolated, low-mass galaxies provide the opportunity to assess the impact of reionization on their star formation histories (SFHs) without the ambiguity of environmental processes associated with massive host galaxies. There are very few isolated, low-mass galaxies that are close enough to determine their SFHs from resolved star photometry reaching below the oldest main-sequence turnoff. The James Webb Space Telescope (JWST) has increased the volume for which this is possible, and here we report on JWST observations of the low-mass, isolated galaxy Leo P. From NIRCam imaging in F090W, F150W, and F277W, we derive an SFH that shows early star formation followed by a pause subsequent to the Epoch of Reionization, which is then later followed by a reignition of star formation. This is very similar to the SFHs from previous studies of other dwarf galaxies in the “transition zone” between quenched very-low-mass galaxies and the more massive galaxies that show no evidence of the impact of reionization on their SFHs; this pattern is rarely produced in simulations of SFHs. The lifetime SFH reveals that Leo P’s stellar mass at the Epoch of Reionization was in the range that is normally associated with being totally quenched. The extended pause in star formation from z ∼ 5 to 1 has important implications for the contribution of low-mass galaxies to the ultraviolet photon budget at intermediate redshifts. We also demonstrate that, due to higher sensitivity and angular resolution, observing in two NIRCam short-wavelength filters is superior to observing in a combination of a short- and a long-wavelength filter.
A NICER View of PSR J1231−1411: A Complex Case
Authors: Salmi Tuomo , Deneva Julia S. , Ray Paul S. , Watts Anna L. , Choudhury Devarshi , Kini Yves , Vinciguerra Serena , Cromartie H. Thankful , Wolff Michael T. , Arzoumanian Zaven , Bogdanov Slavko , Gendreau Keith , Guillot Sebastien , Ho Wynn C. G. , Morsink Sharon M. , Cognard Ismaël , Guillemot Lucas , Theureau Gilles , Kerr Matthew 
Published: November 2024

Abstract
Recent constraints on neutron star mass and radius have advanced our understanding of the equation of state (EOS) of cold dense matter. Some of them have been obtained by modeling the pulses of three millisecond X-ray pulsars observed by the Neutron Star Interior Composition Explorer (NICER). Here, we present a Bayesian parameter inference for a fourth pulsar, PSR J1231−1411, using the same technique with NICER and XMM-Newton data. When applying a broad mass-inclination prior from radio timing measurements and the emission region geometry model that can best explain the data, we find likely converged results only when using a limited radius prior. If limiting the radius to be consistent with the previous observational constraints and EOS analyses, we infer the radius to be 12.6 ± 0.3 km and the mass to be

1.04

−
0.03

+
0.05

M
⊙, each reported as the posterior credible interval bounded by the 16% and 84% quantiles. If using an uninformative prior but limited between 10 and 14 km, we find otherwise similar results, but

R

eq

=

13.5

−
0.5

+
0.3

km for the radius. In both cases, we find a nonantipodal hot region geometry where one emitting spot is at the equator or slightly above, surrounded by a large colder region, and where a noncircular hot region lies close to southern rotational pole. If using a wider radius prior, we only find solutions that fit the data significantly worse. We discuss the challenges in finding the better fitting solutions, possibly related to the weak interpulse feature in the pulse profile.
Gamma-Ray Burst Interaction with the Circumburst Medium: The CBM Phase Following the Prompt Phase in GRBs
Authors: Pe’er Asaf , Ryde Felix 
Published: November 2024

Abstract
Progenitor stars of long gamma-ray bursts (GRBs) could be surrounded by a significant and complex nebula structure lying at a parsec-scale distance. After the initial release of energy from the GRB jet, the jet will interact with this nebula environment. We show here that for a large, plausible parameter space region, the interaction between the jet blast wave and the wind termination (reverse) shock is expected to be weak, and may be associated with a precursor emission. As the jet blast wave encounters the contact discontinuity separating the shocked wind and the shocked interstellar medium, we find that a bright flash of synchrotron emission from the newly formed reverse shock is produced. This flash is expected to be observed at around ∼100 s after the initial explosion and precursor. Such a delayed emission thus constitutes a circumburst medium (CBM) phase in a GRB, having a physically distinct origin from the preceding prompt phase and the succeeding afterglow phase. The CBM phase emission may thus provide a natural explanation for bursts observed to have a precursor followed by an intense, synchrotron-dominated main episode that is found in a substantial minority, ∼10% of GRBs. A correct identification of the emission phase is thus required to infer the properties of the flow and of the immediate environment around GRB progenitors.
Identifying the Origin of Fast Radio Burst–Associated X-Ray Bursts with X-Ray Polarization
Authors: Zhong Shu-Qing , Li Long , Zhang Biao , Dai Zi-Gao 
Published: November 2024

Abstract
The origin of an extraordinary X-ray burst (XRB) associated with a fast radio burst (FRB) such as FRB 20200428 is still unclear, though several models, such as the emission of a trapped fireball modified by resonant cyclotron scattering, the outflow from a polar trapped-expanding fireball, and the synchrotron radiation of a far-away relativistic shock, have been proposed. To determine which model is true, we study the possible X-ray polarization signature for each model, inspired by the importance of radio polarization in identifying the FRB origin. We first numerically simulate or calculate the XRB spectrum for each model and fit it to the observed data, then compute the corresponding polarization signal based on the fit. We find that these three models predict different polarization patterns in terms of phase/time and energy variations. The differences can be used to test the models with future X-ray polarization observations.
Dust Drift Timescales in Protoplanetary Disks at the Cusp of Gravitational Instability
Authors: Williams Jonathan P. , Painter Caleb , Anderson Alexa R. , Ribas Alvaro 
Published: November 2024

Abstract
Millimeter emitting dust grains have sizes that make them susceptible to drift in protoplanetary disks due to the difference between their orbital speed and that of the gas. The characteristic drift timescale depends on the surface density of the gas. By comparing disk radius measurements from Atacama Large Millimeter/submillimeter Array CO and continuum observations at millimeter wavelengths, the gas surface density profile and dust drift time can be self-consistently determined. We find that profiles which match the measured dust mass have very short drift timescales, an order of magnitude or more shorter than the stellar age, whereas profiles for disks that are on the cusp of gravitational instability, defined via the minimum value of the Toomre parameter,

Q

min

∼
1
−
2

, have drift timescales comparable to the stellar lifetime. This holds for disks with masses of dust ≳5 M
⊕ across a range of absolute ages from less than 1 Myr to over 10 Myr. The inferred disk masses scale with stellar mass as

M

disk

≈

M

*

/

5

Q

min

. This interpretation of the gas and dust disk sizes simultaneously solves two long standing issues regarding the dust lifetime and exoplanet mass budget, and suggests that we consider millimeter wavelength observations as a window into an underlying population of particles with a wide size distribution in secular evolution with a massive planetesimal disk.
Asteroseismology of One of the Most Rapidly Rotating DBV Stars: EPIC 248705247
Authors: Zhang Jiayi , Fu Jianning , Cang Tianqi , Su Jie , Chen Yanhui , Ma Xiaoyu , Meng Gang 
Published: November 2024

Abstract
We present a comprehensive analysis of oscillations of the helium-rich white dwarf DBV star EPIC 248705247 (SDSS J102106.69+082724.8). We extract the light curves from 79.7 days of K2 Campaign 14 data and identify 21 independent frequencies, including three complete and three incomplete dipole modes, with an average frequency splitting of 20.37 ± 0.40 μHz. Our analyses reveal a rotation period of EPIC 248705247 of approximately 6.82 ± 0.07 hr, making it one of the most rapidly rotating DBV stars currently known. We utilize the White Dwarf Evolution Code (WDEC) to compute models to look for the seismic best-fitted model, yielding the following stellar parameters: M/M
⊙ = 0.650 ± 0.003, T
eff = 23,660 ± 68 K,

log
(

M

env

/

M

*

)
=
−
2.01
±
0.01

and

log
(

M

He

/

M

*

)

=
−
4.90
±
0.05

. We also explore the phenomenon of mode trapping, as well as the potential influence of a weak magnetic field. We find that this star is located near the red edge of the theoretical instability strip of DBVs. Hence, our asteroseismological analysis of EPIC 248705247 provides the properties and behaviors of a rapidly rotating DBV.
Examining the Relationship between the Persistent Emission and the Accretion Rate during a Type I X-Ray Burst
Authors: Speicher J. , Ballantyne D. R. , Fragile P. C. 
Published: November 2024

Abstract
The accretion flow onto a neutron star will be impacted by irradiation from a type I X-ray burst. The burst radiation exerts Poynting–Robertson (PR) drag on the accretion disk, leading to an enhanced mass accretion rate. Observations of X-ray bursts often find evidence that the normalization of the disk-generated persistent emission (commonly denoted by the factor f

a
) increases during a burst, and changes in f

a
have been used to infer the evolution of the mass accretion rate due to PR drag. Here, we examine this proposed relationship between f

a
and mass accretion rate enhancement using time-resolved data from simulations of accretion disks impacted by type I X-ray bursts. We consider bursts from both spinning and nonspinning neutron stars and track both the change in accretion rate due to PR drag and the disk emission spectra during the burst. Regardless of the neutron star spin, we find that f

a
strongly correlates with the disk temperature and only weakly follows the mass accretion rate (the Pearson correlation coefficients are ≤0.63 in the latter case). Additionally, heating causes the disk to emit at higher energies, reducing its contribution to a soft excess. We conclude that f

a
cannot accurately capture the mass accretion rate enhancement and is rather a tracer of the disk temperature.
Predicting Photospheric Ultraviolet Emission from Stellar Evolutionary Models
Authors: Wang Song , Li Xue , Han Henggeng , Liu Jifeng 
Published: November 2024

Abstract
Stellar ultraviolet (UV) emission serves as a crucial indicator for estimating magnetic activity and evaluating the habitability of exoplanets orbiting stars. In this paper, we present a straightforward method to derive stellar photospheric UV emission for F to M main-sequence stars. By using PARSEC models, we establish relations between near-UV (NUV) and far-UV (FUV) magnitudes from the Galaxy Evolution Explorer, NUV magnitudes from the China Space Station Telescope, and stellar effective temperatures and Gaia blue photometer–red photometer colors for different metallicities. Together with the observed sample, we find that for NUV emission, the photospheric contribution to the observed flux is less than 20% for M stars, around 10%–70% for K stars, and in a range from 30% to 85% for G and F stars. For FUV emission, the photospheric contribution is less than 10−6 for M stars, below 10−4 for K stars, around 10−4–10% for G stars, and between 6% and 50% for F stars. Our work enables the simple and effective determination of stellar excess UV emission and the exploration of magnetic activity.