bluuebunny/crossref_metadata_2025_split huggingface dataset:
O uso indiscriminado do Ozempic® para fins estéticos: uma revisão de literatura
Authors: Rodrigues Williane Lima , Silva Tallyson Menezes Bento da 
Published: October 2024

Introdução: A busca pelo emagrecimento tornou-se comum na sociedade contemporânea, no qual diversas pessoas desejam atingir um determinado padrão estético. Muitos fazem uso do OZEMPIC®, um medicamento prescrito para o tratamento do diabetes tipo 2. Porém, esta prática pode acarretar sérios problemas em pacientes não diabéticos, o que requer atenção e monitoramento cuidadoso. Objetivo: Realizar uma revisão de literatura acerca do uso off-label do OZEMPIC® (semaglutida) para perda de peso, enfocando os efeitos colaterais, a importância do acompanhamento farmacêutico, e os riscos do uso indiscriminado para fins estéticos. Método: Foi realizado um levantamento da literatura nas bases de dados: Scientific Electronic Library Online (SCIELO), Biblioteca Virtual em Saúde (BVS) e PubMed. Só foram validados trabalhos no idioma potuguês e inglês publicados durante o período de 2019 a 2024. Resultados: Foram encontrados 11 artigos relevantes sobre as tendências e popularidade do uso off-label de Ozempic®, impactos na saúde e segurança do uso off-label, aspectos regulatórios e práticas profissionais, além do conhecimento, atitudes e supervisão na prescrição. Conclusões: O uso off-label de Ozempic® para perda de peso estética cresce nas redes sociais, mas com pouca conscientização sobre os riscos à saúde.
The ∼50 Myr Old TOI-942c is Likely on an Aligned, Coplanar Orbit and Losing Mass
Authors: Teng 滕 Huan-Yu 环宇 , Dai 戴 Fei 飞 , Howard Andrew W. , Isaacson Howard , Rubenzahl Ryan A. , Angelo Isabel , Polanski Alex S. 
Published: October 2024

Abstract
We report the observation of the transiting planet TOI-942c, a Neptunian planet orbiting a young K-type star approximately 50 Myr years old. Using the Keck/High Resolution Echelle Spectrometer, we observed a partial transit of the planet and detected an associated radial velocity anomaly. By modeling the Rossiter–McLaughlin effect, we derived a sky-projected obliquity of

λ

=

24

−
14

+
14

degrees, indicating TOI-942c is in a prograde and likely aligned orbit. Upon incorporation of the star’s inclination and the planet’s orbital inclination, we determined a true obliquity for TOI-942c of ψ < 43° at 84% confidence, while dynamic analysis strongly suggests TOI-942c is aligned with stellar spin and coplanar with the inner planet. Furthermore, TOI-942c is also a suitable target for studying atmospheric loss of young Neptunian planets that are likely still contracting from the heat of formation. We observed a blueshifted excess absorption in the Hα line at 6564.7 Å, potentially indicating atmospheric loss due to photoevaporation. However, due to the lack of preingress data, additional observations are needed to confirm this measurement.
Improving Power Spectrum Estimation Using Multitapering: Efficient Asteroseismic Analyses for Understanding Stars, the Milky Way, and Beyond
Authors: Patil Aarya A. , Eadie Gwendolyn M. , Speagle 沈 Joshua S. 佳士 , Thomson David J. 
Published: October 2024

Abstract
Asteroseismic time series data have imprints of stellar oscillation modes, whose detection and characterization through time series analysis allows us to probe stellar interior physics. Such analyses usually occur in the Fourier domain by computing the Lomb–Scargle (LS) periodogram, an estimator of the power spectrum underlying unevenly sampled time series data. However, the LS periodogram suffers from the statistical problems of (1) inconsistency (or noise) and (2) bias due to high spectral leakage. Here, we develop a multitaper power spectrum estimator using the nonuniform fast Fourier transform (mtNUFFT) to tackle the inconsistency and bias problems of the LS periodogram. Using a simulated light curve, we show that the mtNUFFT power spectrum estimate of solar-like oscillations has lower variance and bias than the LS estimate. We also apply our method to the Kepler-91 red giant, and combine it with PBjam peakbagging to obtain mode parameters and a derived age estimate of 3.97 ± 0.52 Gyr. PBjam allows the improvement of age precision relative to the 4.27 ± 0.75 Gyr APOKASC-2 (uncorrected) estimate, whereas partnering mtNUFFT with PBjam speeds up peakbagging thrice as much as LS. This increase in efficiency has promising implications for Galactic archaeology, in addition to stellar structure and evolution studies. Our new method generally applies to time-domain astronomy and is implemented in the public Python package tapify, available at https://github.com/aaryapatil/tapify.
Far-field Pattern Analysis Based on Piecewise Aperture Field Integration for Leighton Chajnantor Telescope Antenna under Gravity and Wind Load
Authors: You Jia , Wang Zheng 
Published: October 2024

Abstract
The Caltech Submillimeter Observatory telescope will be relocated from Mauna Kea, Hawaii to Chajnantor Plateau, Chile, refurbished there and renamed the Leighton Chajnantor Telescope (LCT). At the new site, the open-air environment, as well as the high altitude, will amplify the influence of gravity and wind load on structural deformation, thus affecting the antenna’s radiation characteristics, which can be characterized by a far-field pattern. To quickly and accurately compensate for the effect of reflector structural deformation on the far-field pattern of LCT’s antenna, we propose a far-field pattern quick calculation method (FPQCM) to analyze the antenna’s radiation characteristics under gravity and various wind loads, which combines the optical path difference calculation method on the aperture plane, the piecewise Zernike polynomial function, and the piecewise aperture field integration method. Through extensive experimental comparisons with the numerical method based on physical optics and physical theory of diffraction, it is validated that the proposed FPQCM significantly reduces the time by more than 100 times for acquiring the far-field patterns while maintaining the accuracy of the main figure of merits at the highest frequency (i.e., 856 GHz). In addition, we analyzed the far-field pattern of the antenna at different zenith angles, gravity, and winds of different strengths and directions by FPQCM, which provided guidance for performing more precise control through an active surface optimization system after LCT resumes operation, thus facilitating the acquisition of higher surface accuracy and better observation effect.
Exploring the Broadband Spectral and Timing Characteristics of GRS 1915+105 with AstroSat and NICER Observations
Authors: Dhaka Ruchika , Misra Ranjeev , Jain Pankaj , Yadav J. S. 
Published: October 2024

Abstract
In this study, we undertake a spectral-timing analysis of the black hole X-ray binary source GRS 1915+105 using simultaneous observations carried out by AstroSat (Large Area X-ray Proportional Counter, LAXPC and Soft X-ray Telescope, SXT) and Neutron Star Interior Composition Explorer (NICER) in 2017. The source showed two flux levels (high and low), whose energy spectra can be described by the thermal comptonization of disk photons. The spectral parameters obtained by the joint fitting of SXT/LAXPC and NICER/LAXPC were consistent. The power density spectra from LAXPC and NICER revealed a broad, prominent feature at ∼2 Hz. The energy dependence of the fractional rms and time lag of this feature cannot be explained by only variations of coronal spectral parameters. Instead, a model where the coronal heating rate varies first and induces a change in the disk temperature and inner radius can explain the variation. Our results underline the importance of simultaneous observations by AstroSat and NICER and highlight the need for more sophisticated models to explain the spectral-temporal behavior of black hole systems.
IllustrisTNG in the HSC-SSP: No Shortage of Thin Disk Galaxies in TNG50
Authors: Xu 徐 Dewang 德望 , Gao 高 Hua 桦 , Bottrell Connor , Yesuf Hassen M. , Shi Jingjing 
Published: October 2024

Abstract
We perform a thorough analysis of the projected shapes of nearby galaxies in both observations and cosmological simulations. We implement a forward-modeling approach to overcome the limitations in previous studies, which hinder accurate comparisons between observations and simulations. We measure axis ratios of z = 0 (snapshot 99) TNG50 galaxies from their synthetic Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) images and compare them with those obtained from real HSC-SSP images of a matched galaxy sample. Remarkably, the comparison shows excellent agreement between the observations and the TNG50 simulation, challenging previous claims that ΛCDM models underproduced the abundance of thin galaxies. Specifically, for galaxies with stellar masses

10
≤
log
(

M

⋆

/

M

☉

)
≤
11.5

, we find ≲0.1σ tensions between the observations and the simulation, a stark contrast to the previously reported ≳10σ tensions. We reveal that low-mass galaxies

(

M

⋆

≲

10
9.5

M

☉

)

in TNG50 are thicker than their observed counterparts in HSC-SSP and attribute this to the spurious dynamical heating effects that artificially puff up galaxies. We also find that, despite the overall broad agreement, TNG50 galaxies are more concentrated than the HSC-SSP ones at the low- and high-mass end of the stellar mass range of

9.0
≤
log
(

M

⋆

/

M

☉

)
≤
11.2

and are less concentrated at intermediate stellar masses. But we argue that the higher concentrations of the low-mass TNG50 galaxies are not likely the cause of their thicker/rounder appearances. Our study underscores the critical importance of conducting mock observations of simulations and applying consistent measurement methodologies to facilitate proper comparison with observations.
Spectroastrometry and Reverberation Mapping of Active Galactic Nuclei. I. The Hβ Broad-line Region Structure and Black Hole Masses of Five Quasars
Authors: Li Yan-Rong , Hu Chen , Yao Zhu-Heng , Chen Yong-Jie , Bai Hua-Rui , Yang Sen , Du Pu , Fang Feng-Na , Fu Yi-Xin , Liu Jun-Rong , Peng Yue-Chang , Songsheng Yu-Yang , Wang Yi-Lin , Xiao Ming , Zhai Shuo , Winkler Hartmut , Bai Jin-Ming , Ho Luis C. , Petrov Romain G. , Aceituno Jesús , Wang Jian-Min ,   SARM Collaboration
Published: October 2024

Abstract
We conduct a reverberation mapping (RM) campaign to spectroscopically monitor a sample of selected bright active galactic nuclei with large anticipated broad-line region (BLR) sizes adequate for spectroastrometric (SA) observations by the GRAVITY instrument on the Very Large Telescope Interferometer. We report the first results for five objects, IC 4329A, Mrk 335, Mrk 509, Mrk 1239, and PDS 456, among which Mrk 1239 and PDS 456 are for the first time spectroscopically monitored. We obtain multiyear monitoring data and perform multicomponent spectral decomposition to extract the broad Hβ profiles. We detect significant time lags between the Hβ and continuum variations, generally obeying the previously established BLR size–luminosity relation. Velocity-resolved Hβ time lags illustrate diverse, possibly evolving, BLR kinematics. We further measure the Hβ line widths from mean and rms spectra and the resulting virial products show good consistency among different observing seasons. Adopting a unity virial factor and the FWHM of the broad Hβ line from the mean spectra as a measure of velocity, the obtained black hole masses averaged over seasons are

log

M

•

/

M

⊙

=

8.02

−
0.14

+
0.09

,

6.92

−
0.12

+
0.12

,

8.01

−
0.25

+
0.16

,

7.44

−
0.14

+
0.13

, and

8.59

−
0.11

+
0.07

for the five objects, respectively. Black hole mass estimations using other line width measures are also reported. For objects with previous RM campaigns, our mass estimates are in agreement with earlier results. In a companion paper, we will employ BLR dynamical modeling to directly infer the black hole mass and thereby determine the virial factors.
NuSTAR Observation of the TeV-detected Radio Galaxy 3C 264: Core Emission and the Hot Accretion Flow Contribution
Authors: Wong Ka-Wah , Steiner Colin M. , Blum Allison M. , Lin Dacheng , Nemmen Rodrigo , Irwin Jimmy A. , Wik Daniel R. 
Published: October 2024

Abstract
3C 264 is one of the few FRI radio galaxies with detected TeV emission. It is a low-luminosity active galactic nucleus (LLAGN) and is generally associated with a radiatively inefficient accretion flow (RIAF). Earlier multiwavelength studies suggest that the X-ray emission originates from a jet. However, the possibility that the RIAF can significantly contribute to the X-rays cannot be ruled out. In particular, hard X-ray emission ≳10 keV has never been detected, making it challenging to distinguish between X-ray models. Here we report a NuSTAR detection up to 25 keV from 3C 264. We also present subpixel deconvolved Chandra images to resolve jet emission down to ∼0.″2 from the center of the unresolved X-ray core. Together with a simultaneous Swift observation, we have constrained the dominant hard X-ray emission to be from its unresolved X-ray core, presumably in its quiescent state. We found evidence of a cutoff in the energy around 20 keV, indicating that at least some of the X-rays from the core can be attributed to the RIAF. The Comptonization model suggests an electron temperature of about 15 keV and an optical depth ranging between 4 and 7, following the universality of coronal properties of black hole accretion. The cutoff energy or electron temperature of 3C 264 is the lowest among those of other LLAGNs. The detected hard X-ray emission is at least an order of magnitude higher than that predicted by synchrotron self-Compton models introduced to explain γ-ray and TeV emission, suggesting that the synchrotron electrons might be accelerated to higher energies than previously thought.
Unraveling the Hybrid Origins of the X-Ray Nonthermal Emission from IGR J17091–3624
Authors: Lin Zikun , Wang Yanan , del Palacio Santiago , Méndez Mariano , Zhang Shuang-Nan , Russell Thomas D. , Ji Long , Zhang Jin , Zhang Liang , Altamirano Diego , Liu Jifeng 
Published: October 2024

Abstract
We present a comprehensive study based on multiwavelength observations from the NuSTAR, NICER, Swift, Fermi, NEOWISE, and ATCA telescopes during the 2022 outburst of the black-hole X-ray binary IGR J17091–3624. Our investigation concentrates on the heartbeat-like variability in the X-ray emission, with the aim of using it as a tool to unravel the origin of the nonthermal emission during the heartbeat state. Through X-ray timing and spectral analysis, we observe that the heartbeat-like variability correlates with changes in the disk temperature, supporting the disk radiation pressure instability scenario. Moreover, in addition to a Comptonization component, our time-averaged and phase-resolved spectroscopy reveal the presence of a power-law component that varies independently from the disk component. Combined with the radio–X-ray spectral energy distribution fitting, our results suggest that the power-law component could originate from synchrotron self-Compton radiation in the jet, which requires a strong magnetic field of about B = (0.3–3.5) × 106 G. Additionally, assuming that IGR J17091-3624 and GRS 1915 + 105 share the same radio–X-ray correlation coefficient during both the hard and the heartbeat states, we obtain a distance of 13.7 ± 2.3 kpc for IGR J17091–3624.
Realistic Uncertainties for Fundamental Properties of Asteroseismic Red Giants and the Interplay between Mixing Length, Metallicity, and

ν

max
Authors: Li 李 Yaguang 亚光 , Bedding Timothy R. , Huber Daniel , Stello Dennis , van Saders Jennifer , Zhou 周 Yixiao 一啸 , Crawford Courtney L. , Joyce Meridith , Li 李 Tanda 坦达 , Murphy Simon J. , Sreenivas K. R. 
Published: October 2024

Abstract
Asteroseismic modeling is a powerful way to derive stellar properties. However, the derived quantities are limited by built-in assumptions used in stellar models. This work presents a detailed characterization of stellar model uncertainties in asteroseismic red giants, focusing on the mixing-length parameter α
MLT, the initial helium fraction Y
init, the solar abundance scale, and the overshoot parameters. First, we estimate error floors due to model uncertainties to be ≈0.4% in mass, ≈0.2% in radius, and ≈17% in age, primarily due to the uncertain state of α
MLT and Y
init. The systematic uncertainties in age exceed typical statistical uncertainties, suggesting the importance of their evaluation in asteroseismic applications. Second, we demonstrate that the uncertainties from α
MLT can be entirely mitigated by direct radius measurements or partially through

ν

max

. Utilizing radii from Kepler eclipsing binaries, we determined the α
MLT values and calibrated the α
MLT–[M/H] relation. The correlation observed between the two variables is positive, consistent with previous studies using 1D stellar models, but in contrast with outcomes from 3D simulations. Third, we explore the implications of using asteroseismic modeling to test the

ν

max

scaling relation. We found that a perceived dependency of

ν

max

on [M/H] from individual frequency modeling can be largely removed by incorporating the calibrated α
MLT–[M/H] relation. Variations in Y
init can also affect

ν

max

predictions. These findings suggest that

ν

max

conveys information not fully captured by individual frequencies, and that it should be carefully considered as an important observable for asteroseismic modeling.
New Versus Past Silica Crush Curve Experiments: Application to Dimorphos Benchmarking Impact Simulations
Authors: Malamud Uri , Schäfer Christoph M. , Luciana San Sebastián Irina , Timpe Maximilian , Alexander Essink Karl , Kreuzig Christopher , Meier Gerwin , Blum Jürgen , Perets Hagai B. , Burger Christoph 
Published: October 2024

Abstract
Crush curves are of fundamental importance to numerical modeling of small and porous astrophysical bodies. The empirical literature often measures them for silica grains, and different studies have used various methods, sizes, textures, and pressure conditions. Here, we review past studies and supplement further experiments in order to develop a full and overarching understanding of the silica crush curve behavior. We suggest a new power-law function that can be used in impact simulations of analog materials similar to microgranular silica. We perform a benchmarking study to compare this new crush curve to the parametric quadratic crush curve often used in other studies, based on the study case of the DART impact onto the asteroid Dimorphos. We find that the typical quadratic crush curve parameters do not closely follow the silica crushing experiments, and as a consequence, they under (over) estimate compression close (far) from the impact site. The new crush curve presented here, applicable to pressures between a few hundred Pa and up to 1.1 GPa, might therefore be more precise. Additionally, it is not calibrated by case-specific parameters, and can be used universally for comet- or asteroid-like bodies, given an assumed composition similar to microgranular silica.
Simultaneous Proton and Electron Energization during Macroscale Magnetic Reconnection
Authors: Yin 尹 Zhiyu 志宇 , Drake J. F. , Swisdak M. 
Published: October 2024

Abstract
The results of simulations of magnetic reconnection accompanied by electron and proton heating and energization in a macroscale system are presented. Both species form extended power-law distributions that extend nearly three decades in energy. The primary drive mechanism for the production of these nonthermal particles is Fermi reflection within evolving and coalescing magnetic flux ropes. While the power-law indices of the two species are comparable, the protons overall gain more energy than electrons, and their power law extends to higher energy. The power laws roll into a hot thermal distribution at low energy with the transition energy occurring at lower energy for electrons compared with protons. A strong guide field diminishes the production of nonthermal particles by reducing the Fermi drive mechanism. In solar flares, proton power laws should extend down to tens of keV, far below the energies that can be directly probed via gamma-ray emission. Thus, protons should carry much more of the released magnetic energy than expected from direct observations.
Medication Adherence and Functioning in Individuals With Bipolar Disorder Type I
Authors: Yilmaz Emel Bahadir , Dikmen Sema Nur Türkoğlu , Yüksel Arzu 
Published: October 2024

Purpose
To determine the correlation between medication adherence and functioning in individuals with bipolar disorder (BD) and the predictors of functionality.

Method
This cross-sectional and correlational study was conducted with 145 individuals with BD type I. Data were collected using a Patient Information Form, the Medication Adherence Rating Scale, and Functioning Assessment Short Test.

Results
Findings showed that most participants did not take medication as prescribed. Medication adherence was negatively correlated with functionality. Predictors of functionality were years of treatment, number of hospitalizations, working status, medication adherence, family history of mental illness, and history of suicide.

Conclusion

Medication nonadherence is a fundamental problem for individuals with BD. Nursing interventions to increase functionality and medication adherence among this at-risk group should be planned and implemented. [
Journal of Psychosocial Nursing and Mental Health Services, 63
(2), 25–33.]
Una aproximación diacrónica a la gestación de confiar como verbo de transferencia
Authors: Conde Noguerol María Eugenia 
Published: October 2024

En este trabajo se apuntan las características semántico-sintácticas de confiar como verbo de transferencia desde su gestación en la Edad Media hasta el siglo XIX. El análisis cualitativo y cuantitativo de una muestra de datos extraída de un corpus longitudinal diacrónico permite afirmar que fue en el siglo XVIII cuando se produjo el proceso de cristalización del esquema triactancial actual confiar(le) algo a alguien.
Revolutionizing Rural Health Care: The Power of Telehealth and Digital Health Literacy
Authors: Chandrakar Mayank 
Published: October 2024

Abstract
For many living in remote areas, accessing quality health care remains a significant hurdle. Long distances, limited specialists, and transportation challenges create a gap in care that telehealth has the potential to bridge. This article explores how telehealth, the use of telecommunication technologies for health-care delivery, can revolutionize rural health care. Telehealth consultations can connect patients with specialists in distant locations, reducing travel burdens and wait times. It can also enhance preventative care through remote monitoring and medication management. However, the success of telehealth hinges on digital health literacy. Equipping rural communities with the skills to navigate these technologies is crucial for maximizing their benefits. This article delves into the challenges and opportunities presented by telehealth in rural areas. It discusses how initiatives promoting digital health literacy can empower communities and ensure equitable access to quality health care. Ultimately, it argues that by embracing technological advancements and fostering digital literacy, we can create a future where location no longer dictates the quality of health care received.