bluuebunny/crossref_metadata_2025_split huggingface dataset:
RETROCESSO SOCIAL: UM DISCURSO ANTIFEMINISTA
Authors: Santos Ana Letícia Chaves , Lopes Janaína Rodrigues 
Published: April 2024

O presente estudo propõe uma análise da entrevista de Pietra Bertolazzi no canal "Amigas da Onça" no YouTube, na qual ela expressa uma postura contrária ao feminismo. O objetivo é examinar os argumentos, utilizados por Bertolazzi na defesa de uma ideologia machista, visando oferecer uma análise crítica sobre como esse discurso conquista a atenção na sociedade. Destacam-se o forte apelo moral e religioso, especialmente nas considerações sobre a Lei Maria da Penha. O estudo se aprofundará na análise das declarações de Bertolazzi em relação a essa legislação, questionando a legalidade da lei e explorando de que maneira seus argumentos podem influenciar a percepção pública sobre essa importante ferramenta de combate à violência doméstica e proteção dos direitos das mulheres. A metodologia utilizada será a análise do discurso sociocognitivo, conforme apontada por Van Dijk, permitindo uma compreensão das estratégias discursivas empregadas
MATERNIDADE ATÍPICA: CARACTERIZAÇÃO DO SOFRIMENTO E SEUS ENFRENTAMENTOS
Authors: Pastorelli Simone de Oliveira Santos , Viana Cintia Teixeira de Sousa , Benicasa Miria Gomes 
Published: April 2024

O estudo tem como objetivo investigar estratégias de enfrentamento na maternidade atípica, identificar desafios, obstáculos e compreender os fatores que influenciam a abordagem das mães diante dessas situações. Foi realizada uma revisão sistemática, seguindo as diretrizes PRISMA, de artigos relacionados ao "Enfrentamento da Atípica". As buscas iniciais nas bases de dados BVS e CAPES resultaram em 418 artigos, dos quais 13 atenderam aos critérios de inclusão após remoção de duplicatas e avaliação detalhada. Identificou-se que o estresse e a depressão são desafios significativos para as mães de crianças neurodivergentes. As estratégias de enfrentamento envolvem a busca de diagnóstico precoce, intervenções e redes de apoio. As conclusões sublinham a importância de programas de assistência centrados no apoio a mães, pais e cuidadores. A revisão da literatura revela uma lacuna nos estudos que abordem as necessidades e desafios específicos das famílias com crianças atípicas, enfatizando a necessidade de programas de intervenção adaptados a esta população
Impact of Pharmacist-led Interventions on Medication Adherence and Inhalation Technique in Adult Patients with COPD and Asthma
Authors: Tiwari Rajib , Timilsina Menaka , Banstola Susmita 
Published: April 2024

Introduction: Inhalation technique and medication adherence are essential prerequisites for achieving optimal therapeutic effects in patients with chronic obstructive pulmonary disease (COPD) and asthma. Although there are various effective treatments for respiratory disorders, disease control in these patients is still sub-optimal because of incorrect inhalation techniques and poor medication adherence. Pharmacist-led interventions have demonstrated a positive impact on improving inhalation technique, better medication adherence, and thus subsequently improving the quality of life of patients.
Methods: Search engines such as PubMed, Google Scholar, and Science Direct were used to identify the relevant information using keywords: Chronic Obstructive Pulmonary Disease, Asthma, Pharmaceutical care, Pharmacist Intervention, Medication Adherence and Inhalation Technique. The relevant articles that were published between 2005 to 2021 were included and reviewed for the Pharmacist-led interventions to improve medication adherence, inhalation technique, and quality of life of patients with COPD and asthma.
Results: Of the 300 articles screened, a total of 14 articles met the inclusion criteria and were included for review. Pharmacist-led interventions help to improve the medication adherence, inhalation technique, and quality of life of patients with COPD and asthma. Similarly, the articles mentioned in this review found that the interventions provided by the pharmacist to COPD and asthma patients were cost-effective in terms of reducing hospitalization rates and severe exacerbation rates.
Conclusion: Our review concluded that the pharmacists’ interventions have a significant improvement in medication adherence and inhalation techniques with the enhancement of therapeutic effects in adult patients with COPD and asthma.
Effectiveness of Using Video Clip on Reduction of Anxiety During Venipuncture among Children in a Selected Hospital of Eastern Nepal
Authors: Khatri Shova , Yadav Upendra , Chaudhary Ramanand , Karn Basant Kumar , Tiwari Sirjana , Subedi Santosh , Lama Sami 
Published: April 2024

Introduction: Venipuncture can produce extreme anxiety to children who undergo it. Video clip as distraction is a simple technique which does not require any specific training and can be implemented by nurses, parents or other health staff members in any settings. Besides, it has a minimal cost and implies no risks for the children. This study aimed to assess the anxiety of children during venipuncture and determine the effectiveness of video clip in reducing anxiety.
Methods: A posttest only experimental research was conducted in BP Koirala Institute of Health Sciences (BPKIHS), Dharan Nepal including 50 school age children undergone venipuncture. Random sampling technique was applied to recruit respondents. Respondents were randomly assigned either to the experimental or control group with 25 in each. The Experimental group were shown video clip 3 minutes prior to the venipuncture till 3 minutes after completion of venipuncture while Control group had gone a routine venipuncture procedure only during venipuncture. Pearson’s chi square test and Fisher’s exact test was used for the analysis of anxiety response of both group.
Results: Showing video clips was effective in reducing venipuncture in children (p=0.001). Among the participants, 72% had high anxiety in control group while it was 24% in experimental group. In a same way 76% had low anxiety in the experiment group while it was 28% among control group. There is a significant difference in the anxiety level between the study and control group (p=0.001).
Conclusion: This study suggests that video clip is safe and cost effective method in reduction of anxiety in children undergoing venipuncture.
How Well is the International Celestial Reference System Maintained in Official IAU Implementations?
Authors: Malkin Zinovy 
Published: April 2024

Abstract
The International Celestial Reference Frame (ICRF) based on the VLBI-derived positions of 608 extragalactic radio sources was adopted by the International Astronomical Union (IAU) in 1998 as the first realization of the International Celestial Reference System (ICRS). Later, in 2009 and 2020, two extended ICRF versions, ICRF2 and ICRF3, respectively, were released. The latter is adopted by the IAU as the current implementation of the ICRF in the radio band. In the meantime, the Gaia mission delivered three versions of the optical ICRS realization in 2016, 2018, and 2022 with an accuracy similar to that achieved by VLBI-based ICRF. The Gaia-CRF catalogs were linked to the ICRF under no-rotation conditions and thus may suffer from ICRF systematic instability if the latter is substantial. In this work, a new analysis was performed to assess the long-term stability of radio and optical ICRS realizations. Based on the 16-parameter vector spherical harmonics expansion of the differences between the three ICRF catalogs, it can be concluded that the mutual orientation between them is at a level of a few tens of microarcseconds, while the components of the glide vector and E
2,0 term are several times greater. A comparison of the three Gaia-CRF catalogs with the ICRF3-SX showed that for the latest Gaia-CRF catalog, Gaia-CRF3, all rotational and deformation components are below 20 μas except for the E
2,0 term, which is several times greater. For both ICRF and Gaia-CRF catalogs, the evolution of the source position errors is also tracked.
Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: Luo An-Xu , Liu Hong-Li , Qin Sheng-Li , Yang Dong-ting , Pan Sirong 
Published: April 2024

Abstract
This paper is aimed at exploring the implications of velocity-dispersion scalings on high-mass star formation in molecular clouds, including the scalings of Larson’s linewidth–size (σ– R) and ratio–mass surface density (

L

– Σ; here

L

= σ/R
0.5). We have systematically analyzed the σ parameter of well-selected 221 massive clumps, complemented with published samples of other hierarchical density structures of molecular clouds over spatial scales of 0.01–10 pc. Those massive clumps are classified into four phases: quiescent, protostellar, H ii region, and PDR clumps in an evolutionary sequence. The velocity dispersion of clumps increases overall with the evolutionary sequence, reflecting enhanced stellar feedback in more evolved phases. The relations of σ– R and

L

– Σ are weak with the clump sample alone, but become evident when combined with others spanning a much wider spatial scales. For σ– R, its tight relation indicates a kinematic connection between hierarchical density structures, supporting theoretical models of multiscale high-mass star formation. From the

L

– Σ relation, cloud structures can be found to transition from overvirial state (α
vir > 2) to subvirial state (α
vir < 2) as they become smaller and denser, indicating a possible shift in the governing force from turbulence to gravity. This implies that the multiscale physical process of high-mass star formation hinges on the self-gravity of subvirial molecular clouds. However, the influence of turbulence may not be dismissed until large-scale clouds attain a subvirial state. This is pending confirmation from future multiscale kinematic observations of molecular clouds with uniform observing settings.
A High Incidence of Dusty Hα Emitters
at z > 3 Among UltraVISTA Dropout Galaxies in
COSMOS Revealed by JWST
Authors: van Mierlo Sophie E. , Caputi Karina I. , Ashby Matthew L. N. , Kokorev Vasily , Navarro-Carrera Rafael , Rinaldi Pierluigi 
Published: April 2024

Abstract
We have characterized 26 Spitzer/IRAC-selected sources from the SMUVS program
that are undetected in the UltraVISTA DR5 H-
and/or K
s-band images, covering 94 arcmin2 of the COSMOS field,
which have deep multiwavelength JWST photometry. We analyzed the JWST/NIRCam
imaging from the PRIMER survey and ancillary HST data to reveal the properties
of these galaxies from spectral energy distribution (SED) fitting. We find that
the majority of these galaxies are detected by NIRCam at λ < 2 μm, with only four
remaining as near-infrared dropouts in the deeper JWST images. Our results
indicate that the UltraVISTA dropouts candidates are primarily located at
z > 3 and are characterized by high dust
extinctions, with a typical color excess E(B − V) = 0.5 ± 0.3 and
stellar mass

log
(

M

*

/

M

⊙

)
=
9.5
±
1.0

. Remarkably, ∼75% of these sources show a flux enhancement
between the observed photometry and modeled continuum SED that can be attributed
to Hα emission in the corresponding NIRCam bands.
The derived (Hα+ N [ii] + S
[ii]) rest-frame equivalent widths and Hα
star formation rates (SFRs) span values ∼100–2200 Å and ∼5–375 M
⊙ yr−1, respectively. The locations of these sources on
the SFR–M
* plane indicate that 35% of them are starbursts, 40% are
main-sequence galaxies, and the remaining 25% are located in the star formation
valley. Our sample includes one active galactic nucleus and six submillimeter
sources, as revealed from ancillary X-ray and submillimeter photometry. The high
dust extinctions combined with the flux boosting from Hα emission explain why these sources are relatively bright Spitzer
galaxies and yet unidentified in the ultradeep UltraVISTA near-infrared
images.
Neutrino-driven Outflows and the Elemental Abundance Patterns of Very Metal-poor Stars
Authors: Psaltis A. , Jacobi M. , Montes F. , Arcones A. , Hansen C. J. , Schatz H. 
Published: April 2024

Abstract
The elemental abundances between strontium and silver (Z = 38–47) observed in the atmospheres of very metal-poor stars in the Galaxy may contain the fingerprint of the weak r-process and ν
p-process occurring in early core-collapse supernovae explosions. In this work, we combine various astrophysical conditions based on a steady-state model to cover the richness of the supernova ejecta in terms of entropy, expansion timescale, and electron fraction. The calculated abundances based on different combinations of conditions are compared with stellar observations, with the aim of constraining supernova ejecta conditions. We find that some conditions of the neutrino-driven outflows consistently reproduce the observed abundances of our sample. In addition, from the successful combinations, the neutron-rich trajectories better reproduce the observed abundances of Sr–Zr (Z = 38–40), while the proton-rich ones, Mo–Pd (Z = 42–47).
Oxygen Isotopic Variations in the Calcium, Aluminum-rich Inclusion–forming Region Recorded by a Single Refractory Inclusion from the CO3.1 Carbonaceous Chondrite Dar al Gani 083
Authors: Ebert Samuel , Nagashima Kazuhide , Krot Alexander N. , Patzek Markus , Bischoff Addi 
Published: April 2024

Abstract
Calcium, aluminum-rich inclusions (CAIs) are the oldest solids dated that formed in the solar system. Most CAIs in unmetamorphosed chondritic meteorites (chondrites; petrologic type ≤3.0) have uniform solar-like 16O-rich compositions (Δ17O ∼ −24‰) and a high initial 26Al/27Al ratio [(26Al/27Al)0] of ∼(4–5) × 10−5, consistent with their origin in a gas of approximately solar composition during a brief (<0.3 Ma) epoch at the earliest stage of our solar system. The nature of O-isotope heterogeneity in CAIs (Δ17O range from ∼−24 up to ∼+5‰) from weakly metamorphosed chondrites (petrologic type >3.0) remains an open issue. This heterogeneity could have recorded fluctuations of O-isotope composition of nebular gas in the CAI-forming region and/or postcrystallization O-isotope exchange of CAI minerals with aqueous fluids on the chondrite parent asteroids. To obtain insights into possible processes resulting in this heterogeneity, we investigated the mineralogy, rare-earth element abundances, and O- and Mg-isotope compositions of a CAI from the CO3.1 chondrite Dar al Gani 083. This concentrically zoned inclusion has a Zn-hercynite core surrounded by layers of (from core to edge) grossite, spinel, melilite, and Al-diopside. The various phases have heterogeneous Δ17O (from core to edge): −2.2 ± 0.6‰, −0.9 ± 2.1‰, −13.7 ± 2.1‰, −2.6 ± 2.3‰, and −22.6 ± 2.1‰, respectively. Magnesium-isotope compositions of grossite, spinel, melilite, and Al-diopside define an undisturbed internal Al–Mg isochron with (26Al/27Al)0 of (2.60 ± 0.29) × 10−6. We conclude that the variations in Δ17O of spinel and diopside recorded fluctuations in O-isotope composition of nebular gas in the CAI-forming region prior to injection and/or homogenization of 26Al at the canonical level. The 16O depletion of grossite and melilite resulted from O-isotope exchange with asteroidal fluid, which did not disturb Al–Mg isotope systematics of the CAI primary minerals.
Investigating the Chemically Homogeneous Evolution Channel and Its Role in the Formation of the Enigmatic Binary Black Hole Progenitor Candidate HD 5980
Authors: Sharpe K. , van Son L. A. C. , de Mink S. E. , Farmer R. , Marchant P. , Koenigsberger G. 
Published: April 2024

Abstract
Chemically homogeneous evolution (CHE) is a promising channel for forming massive binary black holes. The enigmatic, massive Wolf–Rayet binary HD 5980 A&B has been proposed to have formed through this channel. We investigate this claim by comparing its observed parameters with CHE models. Using MESA, we simulate grids of close massive binaries, then use a Bayesian approach to compare them with the stars’ observed orbital period, masses, luminosities, and hydrogen surface abundances. The most probable models, given the observational data, have initial periods ∼3 days, widening to the present-day ∼20 days orbit as a result of mass loss—correspondingly, they have very high initial stellar masses (≳150 M
⊙). We explore variations in stellar-wind mass loss and internal mixing efficiency, and find that models assuming enhanced mass loss are greatly favored to explain HD 5980, while enhanced mixing is only slightly favored over our fiducial assumptions. Our most probable models slightly underpredict the hydrogen surface abundances. Regardless of its prior history, this system is a likely binary black hole progenitor. We model its further evolution under our fiducial and enhanced wind assumptions, finding that both stars produce black holes with masses ∼19–37 M
⊙. The projected final orbit is too wide to merge within a Hubble time through gravitational waves alone. However, the system is thought to be part of a 2+2 hierarchical multiple. We speculate that secular effects with the (possible) third and fourth companions may drive the system to promptly become a gravitational-wave source.
How Long Will the Quasar UV/Optical Flickering Be Damped?
Authors: Zhou Shuying , Sun Mouyuan , Cai Zhen-Yi , Ren Guowei , Wang Jun-Xian , Xue Yongquan 
Published: April 2024

Abstract
The UV/optical light curves of Active Galactic Nuclei (AGNs) are commonly described by the Damped Random Walk (DRW) model. However, the physical interpretation of the damping timescale, a key parameter in the DRW model, remains unclear. Particularly, recent observations indicate a weak dependence of the damping timescale upon both wavelength and accretion rate, clearly being inconsistent with the accretion-disk theory. In this study, we investigate the damping timescale in the framework of the Corona Heated Accretion disk Reprocessing (CHAR) model, a physical model that describes AGN variability. We find that while the CHAR model can reproduce the observed power spectral densities of the 20 yr light curves for 190 sources from Stone et al., the observed damping timescale, as well as its weak dependence on wavelength, can also be well recovered through fitting the mock light curves with DRW. We further demonstrate that such weak dependence is artificial due to the effect of inadequate durations of light curves, which leads to best-fitting damping timescales lower than the intrinsic ones. After eliminating this effect, the CHAR model indeed yields a strong dependence of the intrinsic damping timescale on the bolometric luminosity and rest-frame wavelength. Our results highlight the demand for sufficiently long light curves in AGN variability studies and important applications of the CHAR model in such studies.
Gas Dynamical Friction on Accreting Objects
Authors: Suzuguchi Tomoya , Sugimura Kazuyuki , Hosokawa Takashi , Matsumoto Tomoaki 
Published: April 2024

Abstract
The drag force experienced by astronomical objects moving through gaseous media (gas dynamical friction) plays a crucial role in their orbital evolution. Ostriker derived a formula for gas dynamical friction by linear analysis, and its validity has been confirmed through subsequent numerical simulations. However, the effect of gas accretion onto the objects on the dynamical friction is yet to be understood. In this study, we investigate the Mach number dependence of dynamical friction considering gas accretion through three-dimensional nested-grid simulations. We find that the net frictional force, determined by the sum of the gravitational force exerted by surrounding gas and momentum flux transferred by accreting gas, is independent of the resolution of simulations. Only the gas outside the Bondi–Hoyle–Lyttleton radius contributes to dynamical friction, because the gas inside this radius is eventually absorbed by the central object and returns the momentum obtained through the gravitational interaction with it. In the subsonic case, the front–back asymmetry induced by gas accretion leads to larger dynamical friction than predicted by the linear theory. Conversely, in the slightly supersonic case with a Mach number between 1 and 1.5, the nonlinear effect leads to a modification of the density distribution in a way that reduces the dynamical friction, compared with the linear theory. At a higher Mach number, the modification becomes insignificant and the dynamical friction can be estimated with the linear theory. We also provide a fitting formula for dynamical friction based on our simulations, which can be used in a variety of applications.
Initiation and Eruption of a Two-turn Helical Quiescent Filament on 2013 August 2
Authors: Ou Yudi , Su Yingna , Chen Jialin , Liu Yanjie , Shen Jinhua , Ji Haisheng 
Published: April 2024

Abstract
We investigate a quiescent filament that erupted on 2013 August 2; the eruption was observed in EUV and Hα by the Solar Dynamics Observatory and GONG. After a B9.7 flare in the nearby active region, the dark filament materials near its eastern footpoint start to move in the direction of eruption, and are followed by a counterclockwise rotation identified as the motion of a combination of dark and bright filament materials. Then the entire filament rises up and keeps rotating in a clockwise direction during the eruption. More interestingly, the filament exhibits an unusual two-helix structure near its western footpoint during the eruption, which indicates the existence of a highly twisted flux rope. This hypothesis is confirmed by magnetic field modeling using the flux rope insertion method. In the best-fit unstable model, the lower limits of the estimated maximum and average twist numbers of the erupting flux rope reach 7.5π and 4π, which suggests that kink instability plays an important role in the eruption. During these magnetically coupled sympathetic eruptions, the highly twisted filament under the western lobe of a pseudo-streamer-like structure becomes unstable and erupts due to the removal of confinement by magnetic reconnection at the overlying hyperbolic flux tube, which is initiated by the B9.7 flare in the nearby active region. The initial filament motion occurs at the more unstable eastern footpoint, where the surrounding fields are weaker and decrease with height more rapidly.
Hα Time Delays of Active Galactic Nuclei from the Zwicky Transient Facility Broadband Photometry
Authors: Ma Qinchun , Wen Yuhan , Wu Xue-Bing , Gu Huapeng , Fu Yuming 
Published: April 2024

Abstract
In our previous work on broadband photometric reverberation mapping (PRM), we proposed the interpolated cross-correlation function (ICCF)-Cut process to obtain the time lags of the Hα emission line from two broadband lightcurves via subtracting the continuum emission from the line band. Extending the work, we enlarge our sample to the Zwicky Transient Facility (ZTF) database. We adopt two criteria to select 123 type 1 active galactic nuclei (AGNs) with sufficient variability and smooth light curves from 3537 AGNs at z < 0.09 with more than 100 epoch observations in the g and r bands from the ZTF database. We calculate the Hα time lags for 23 of them that have previous spectroscopic reverberation mapping (SRM) results using the ICCF-Cut, Just Another Vehicle for Estimating Lags In Nuclei (JAVELIN), and χ
2 methods. Our obtained Hα time lags are slightly larger than the Hβ time lags, which is consistent with the previous SRM results and the theoretical model of the AGN broad-line region. The comparisons between the SRM and PRM lag distributions and between the subtracted emission line light curves indicate that after selecting AGNs with the two criteria, combining the ICCF-Cut, JAVELIN, and χ
2 methods provides an efficient way to get the reliable Hα lags from the broadband PRM. Such techniques can be used to estimate the black hole masses of a large sample of AGNs in large multiepoch photometric sky surveys such as the Legacy Survey of Space and Time and the survey from the Wide Field Survey Telescope in the near future.