bluuebunny/crossref_metadata_2025_split huggingface dataset:
Post Covid-19 Emergency Mitigation Strategies Through Parents Readiness in Children's Behavior and Social Development
Authors: Merina Nuning Dwi Merina , Rahmawati Iis , Sulistyorini Lantin , Afdi Septiyono Eka 
Published: February 2024

The COVID-19 pandemic has an impact on patterns of social interaction, education, and behavior on child development. Children with social development problems need good readiness from their parents in order to carry out their optimal growth functions. Parental readiness is one of the mitigation strategies to reduce the negative impact of COVID-19. The purpose of this research is to explore how parents are prepared for their children's social development after the COVID-19 emergency, in the Jember Regency. This research method uses qualitative research with a phenomenological design involving 7 parents in the Jember Regency area. The research instrument used a design theory from Prochaska, namely the transtheoretical model for parental preparation and Hurlock's theory, namely the ability to behave in accordance with social demands for children's social development. Data analysis used the induction method with specific conclusions drawn for the general public and presented descriptively. Parents have prepared and facilitated children's needs, learning environment, and provided motivation to children in their development period. Some parents admit that they have difficulty adjusting to their child's development. This is different from parents as housewives who have a lot of time with their children who claim that they understand their child's condition and can adapt to their child's development. Parents also provide time for their children to talk about their activities in their environment and limit their use of gadgets and replace them with other games that can stimulate their motor and sensory. The readiness of parents in the social development of children in the post-COVID-19 emergency shows positive results. Parents are well prepared to support their children's social development.
Keywords: Child, COVID-19, Development, Parent, Readiness.
Les déficits en micronutriments et leur traitement en réanimation
Authors: Berger Mette M. , Ben-Hamouda Nawfel 
Published: February 2024

Le déficit nutritionnel chez les patients de réanimation ne se limite pas à l’énergie et aux protéines, il intéresse également les micronutriments (MN). Les vitamines C, D et B1, le cuivre, le fer, le sélénium et le zinc sont les plus critiques.
Souvent soumis au stress oxydant et/ou à l’inflammation, ces patients présentent des particularités (comorbidités, pathologies sous-jacentes) rendant les déficits en micronutriments plus fréquents voire plus sévères. Les concentrations sériques basses sont omniprésentes, généralement abaissées par la réponse inflammatoire, mais aussi des déficits causés par des pertes ou des apports insuffisants. La prescription des MNs a dose standard doit faire partie de la prescription quotidienne de la nutrition qu’elle soit entérale ou parentérale, mais ne garantit pas les besoins accrus de nombreux patients. La supplémentation à très haute dose d’un MN isolé reste très controversée, et découragée hors étude clinique. Le but de cette mise au point est de préciser en se basant sur les recommandations internationales les besoins des patients de réanimation en micronutriments.
Evaluating two small-sample corrections for fixed-effects standard errors and inferences in multilevel models with heteroscedastic, unbalanced, clustered data
Authors: Zhang Yichi , Lai Mark H. C. 
Published: February 2024

AbstractMultilevel modeling (MLM) is commonly used in psychological research to model clustered data. However, data in applied research usually violate one of the essential assumptions of MLM—homogeneity of variance. While the fixed-effect estimates produced by the maximum likelihood method remain unbiased, the standard errors for the fixed effects are misestimated, resulting in inaccurate inferences and inflated or deflated type I error rates. To correct the bias in fixed effects standard errors and provide valid inferences, small-sample corrections such as the Kenward-Roger (KR) adjustment and the adjusted cluster-robust standard errors (CR-SEs) with the Satterthwaite approximation for t tests have been used. The current study compares KR with random slope (RS) models and the adjusted CR-SEs with ordinary least squares (OLS), random intercept (RI) and RS models to analyze small, heteroscedastic, clustered data using a Monte Carlo simulation. Results show the KR procedure with RS models has large biases and inflated type I error rates for between-cluster effects in the presence of level 2 heteroscedasticity. In contrast, the adjusted CR-SEs generally yield results with acceptable biases and maintain type I error rates close to the nominal level for all examined models. Thus, when the interest is only in within-cluster effect, any model with the adjusted CR-SEs could be used. However, when the interest is to make accurate inferences of the between-cluster effect, researchers should use the adjusted CR-SEs with RS to have higher power and guard against unmodeled heterogeneity. We reanalyzed an example in Snijders & Bosker (2012) to demonstrate the use of the adjusted CR-SEs with different models.
Donkey disjunctions and overlapping updates
Authors: Elliott Patrick David 
Published: February 2024

This paper is devoted to an analysis of anaphoric dependencies in disjunctive sentences, and consequences for the understanding of the ∃/∀ ambiguity observed with donkey anaphora. The primary focus is on donkey disjunctions, which are sentences where a (negated) existential in an initial disjunct appears to bind a pronoun in a later disjunct, such as "Either there's no bathroom, or its upstairs". The main empirical focus is that donkey disjunctions, like donkey anaphora, exhibit the ∃/∀ ambiguity, and more generally oscillate between homogeneous and heterogeneous readings in a context-sensitive fashion. The paper then proceeds in two steps: first, a principled analysis of donkey disjunctions is developed in the context of a Bilateral Update Semantics (BUS). BUS, by default, generates heterogeneous readings for donkey anaphora/donkey disjunctions (i.e., ∃ readings, in a positive context). In order to account of homogeneous readings, the conjecture is that sentences may be interpreted exhaustively relative to their negations. This has non-trivial consequences due to the non-classicality of BUS — specifically, a failure of the Law of Non-Contradiction.
Marketing Influencer y su Impacto en las Decisiones de Compra
Authors: Campines Barría Francisco Javier 
Published: February 2024

El marketing de influencer es una estrategia de marketing que se basa en colaborar con personas influyentes en las redes sociales para promocionar productos, servicios o marcas. El objetivo del presente estudio es determinar el nivel del influencia que tienen los influencers en la decisión de compra de los consumidores. El enfoque metodológico de la investigación es cuantitativo, de tipo descriptiva. El proceso de recolección de datos, estuvo apoyado en la aplicación de encuestas a una muestra de 88 personas a encuestar. Conforme a la muestra indagada un 87.5% de los encuestados revela que siguen a influencers, de estos un 21.6% da seguimiento a influencers tipo YouTubers. A pesar de que existe una gran cantidad de usuarios que dan a conocer seguir de una forma u otra a influencers por medios de distintas plataformas digitales el 61.4% destacan que estos no influyen en su decisón de compra.
Kindling the First Stars. I. Dependence of Detectability of the First Stars with JWST on the Population III Stellar Masses
Authors: Bovill Mia Sauda , Stiavelli Massimo , Wiggins Alessa Ibrahim , Ricotti Massimo , Trenti Michele 
Published: February 2024

Abstract
The first Population III (Pop III) stars formed out of primordial, metal-free gas, in minihalos at z > 20, and kickstarted the cosmic processes of reionization and enrichment. While these stars are likely more massive than their enriched counterparts, the current unknowns of their astrophysics include when the first Pop III stars ignited, how massive they were, and when and how the era of the first stars ended. Investigating these questions requires an exploration of a multidimensional parameter space, including the slope of the Pop III stellar initial mass function (IMF) and the strength of the nonionizing UV background. In this work, we present a novel model which treats both the slope and maximum mass of Pop III stars as truly free parameters while including the physics of the fragmentation of primordial gas. Our results also hint at a nonuniversal Pop III IMF which is dependent on the efficiency of primordial gas fragmentation. Our relatively simple model reproduces the results from hydrodynamic simulations, but with a computational efficiency which allows us to investigate the observable differences between a wide range of potential Pop III IMFs. In addition, the evolution of the number density of Pop III stars may provide insight into the evolution of the H2 dissociating background. While the slope of the Pop III IMF does not significantly affect the predicted number density of the first stars, more top-heavy IMFs produce Pop III star clusters which are 2–3 magnitudes brighter than their more bottom-heavy counterparts. While the Pop III star clusters are too dim for direct detection by JWST, we find they are within the reach of gravitational lensing.
Thermal Properties of the Hot Core Population in Sagittarius B2 Deep South
Authors: Jeff Desmond , Ginsburg Adam , Bulatek Alyssa , Budaiev Nazar , Sánchez-Monge Álvaro , Bonfand Mélisse , Battersby Cara , Meng Fanyi , Schilke Peter , Schmiedeke Anika 
Published: February 2024

Abstract
We report the discovery of nine new hot molecular cores in the Deep South (DS) region of Sagittarius B2 using Atacama Large Millimeter/submillimeter Array Band 6 observations. We measure the rotational temperature of CH3OH and derive the physical conditions present within these cores and the hot core Sgr B2(S). The cores show heterogeneous temperature structure, with peak temperatures between 252 and 662 K. We find that the cores span a range of masses (203–4842 M
⊙) and radii (3587–9436 au). CH3OH abundances consistently increase with temperature across the sample. Our measurements show the DS hot cores are structurally similar to Galactic disk hot cores, with radii and temperature gradients that are comparable to sources in the disk. They also show shallower density gradients than disk hot cores, which may arise from the Central Molecular Zone’s higher density threshold for star formation. The hot cores have properties which are consistent with those of Sgr B2(N), with three associated with Class II CH3OH masers and one associated with an ultra-compact H ii
region. Our sample nearly doubles the high-mass star-forming gas mass near Sgr B2(S) and suggests the region may be a younger, comparably massive counterpart to Sgr B2(N) and (M). The relationship between peak CH3OH abundance and rotational temperature traced by our sample and a selection of comparable hot cores is qualitatively consistent with predictions from chemical modeling. However, we observe constant peak abundances at higher temperatures (T ≳ 250 K), which may indicate mechanisms for methanol survival that are not yet accounted for in models.
TESS Stellar Rotation up to 80 Days in the Southern Continuous Viewing Zone
Authors: Claytor Zachary R. , van Saders Jennifer L. , Cao Lyra , Pinsonneault Marc H. , Teske Johanna , Beaton Rachael L. 
Published: February 2024

Abstract
The Transiting Exoplanet Survey Satellite (TESS) mission delivers time-series photometry for millions of stars across the sky, offering a probe into stellar astrophysics, including rotation, on a population scale. However, light-curve systematics related to the satellite’s 13.7 day orbit have prevented stellar rotation searches for periods longer than 13 days, putting the majority of stars beyond reach. Machine-learning methods have the ability to identify systematics and recover robust signals, enabling us to recover rotation periods up to 35 days for GK dwarfs and 80 days for M dwarfs. We present a catalog of 7245 rotation periods for cool dwarfs in the Southern Continuous Viewing Zone, estimated using convolutional neural networks. We find evidence for structure in the period distribution consistent with prior Kepler and K2 results, including a gap in 10–20 day cool-star periods thought to arise from a change in stellar spin-down or activity. Using a combination of spectroscopic and gyrochronologic constraints, we fit stellar evolution models to estimate masses and ages for stars with rotation periods. We find strong correlations between the detectability of rotation in TESS and the effective temperature, age, and metallicity of the stars. Finally, we investigate the relationships between rotation and newly obtained spot filling fractions estimated from Apache Point Observatory Galactic Evolution Experiment spectra. Field starspot filling fractions are elevated in the same temperature and period regime where open clusters’ magnetic braking stalls, lending support to an internal shear mechanism that can produce both phenomena.
Goodbye to Chi by Eye: A Bayesian Analysis of Photometric Binaries in Six Open Clusters
Authors: Childs Anna C. , Geller Aaron M. , von Hippel Ted , Motherway Erin , Zwicker Claire 
Published: February 2024

Abstract
We present a robust methodology for identifying photometric binaries in star clusters. Using Gaia DR3, Pan-STARRS, and Two Micron All Sky Survey data, we self-consistently define the cluster parameters and binary demographics for the open clusters (OCs) NGC 2168 (M35), NGC 7789, NGC 6819, NGC 2682 (M67), NGC 188, and NGC 6791. These clusters span in age from ∼200 Myr (NGC 2168) to more than ∼8 Gyr (NGC 6791) and have all been extensively studied in the literature. We use the Bayesian Analysis of Stellar Evolution software suite to derive the age, distance, reddening, metallicity, binary fraction, and binary mass-ratio posterior distributions for each cluster. We perform a careful analysis of our completeness and also compare our results to previous spectroscopic surveys. For our sample of main-sequence stars with masses between 0.6 and 1 M
⊙, we find that these OCs have similar binary fractions that are also broadly consistent with the field multiplicity fraction. Within the clusters, the binary fraction increases dramatically toward the cluster centers, likely a result of mass segregation. Furthermore nearly all clusters show evidence of mass segregation within the single and binary populations. The OC binary fraction increases significantly with cluster age in our sample, possibly due to a combination of mass-segregation and cluster-dissolution processes. We also find a hint of an anticorrelation between binary fraction and cluster central density as well as total cluster mass, possibly due to an increasing frequency of higher-energy close stellar encounters that inhibit long-period binary survival and/or formation.
Excitation of Quasiperiodic Fast-propagating Waves in the Early Stage of the Solar Eruption
Authors: Hu Jialiang , Ye Jing , Chen Yuhao , Mei Zhixing , Tang Zehao , Lin Jun 
Published: February 2024

Abstract
We propose a mechanism for the excitation of large-scale quasiperiodic fast-propagating magnetoacoustic (QFP) waves observed on both sides of the coronal mass ejection. Through a series of numerical experiments, we successfully simulated the quasi-static evolution of the equilibrium locations of the magnetic flux rope in response to the change of the background magnetic field, as well as the consequent loss of the equilibrium that eventually gives rise to the eruption. During the eruption, we identified QFP waves propagating radially outward of the flux rope, and tracing their origin reveals that they result from the disturbance within the flux rope. Acting as an imperfect waveguide, the flux rope allows the internal disturbance to escape to the outside successively via its surface, invoking the observed QFP waves. Furthermore, we synthesized the images of QFP waves on the basis of the data given by our simulations and found consistency with observations. This indicates that the leakage of the disturbance outside the flux rope could be a reasonable mechanism for QFP waves.
Differentiable Cosmological Simulation with the Adjoint Method
Authors: Li 李 Yin 寅 , Modi Chirag , Jamieson Drew , Zhang 张 Yucheng 宇澄 , Lu 陆 Libin 利彬 , Feng 冯 Yu 雨 , Lanusse François , Greengard Leslie 
Published: February 2024

Abstract
Rapid advances in deep learning have brought not only a myriad of powerful neural networks, but also breakthroughs that benefit established scientific research. In particular, automatic differentiation (AD) tools and computational accelerators like GPUs have facilitated forward modeling of the Universe with differentiable simulations. Based on analytic or automatic backpropagation, current differentiable cosmological simulations are limited by memory, and thus are subject to a trade-off between time and space/mass resolution, usually sacrificing both. We present a new approach free of such constraints, using the adjoint method and reverse time integration. It enables larger and more accurate forward modeling at the field level, and will improve gradient-based optimization and inference. We implement it in an open-source particle-mesh (PM) N-body library pmwd (PM with derivatives). Based on the powerful AD system JAX, pmwd is fully differentiable, and is highly performant on GPUs.
Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Narang Mayank , Manoj P. , Tyagi Himanshu , Watson Dan M. , Megeath S. Thomas , Federman Samuel , Rubinstein Adam E. , Gutermuth Robert , Caratti o Garatti Alessio , Beuther Henrik , Bourke Tyler L. , Van Dishoeck Ewine F. , Evans Neal J. , Anglada Guillem , Osorio Mayra , Stanke Thomas , Muzerolle James , Looney Leslie W. , Yang Yao-Lun , Klaassen Pamela , Karnath Nicole , Atnagulov Prabhani , Brunken Nashanty , Fischer William J. , Furlan Elise , Green Joel , Habel Nolan , Hartmann Lee , Linz Hendrik , Nazari Pooneh , Pokhrel Riwaj , Rahatgaonkar Rohan , Rocha Will R. M. , Sheehan Patrick , Slavicinska Katerina , Stutz Amelia M. , Tobin John J. , Tychoniec Lukasz , Wolk Scott 
Published: February 2024

Abstract
Investigating Protostellar Accretion (IPA) is a JWST Cycle 1 GO program that uses NIRSpec integral field units and MIRI Medium Resolution Spectrograph to obtain 2.9–28 μm spectral cubes of young, deeply embedded protostars with luminosities of 0.2–10,000 L
⊙ and central masses of 0.15–12 M
⊙. In this Letter, we report the discovery of a highly collimated atomic jet from the Class 0 protostar IRAS 16253−2429, the lowest-luminosity source (L
bol = 0.2 L
⊙) in the IPA program. The collimated jet is detected in multiple [Fe ii] lines and [Ne ii], [Ni ii], and H i lines but not in molecular emission. The atomic jet has a velocity of about 169 ± 15 km s−1, after correcting for inclination. The width of the jet increases with distance from the central protostar from 23 to 60 au, corresponding to an opening angle of 2.°6 ± 0.°5. By comparing the measured flux ratios of various fine-structure lines to those predicted by simple shock models, we derive a shock speed of 54 km s−1 and a preshock density of 2.0 × 103 cm−3 at the base of the jet. From these quantities and using a suite of jet models and extinction laws, we compute a mass-loss rate between 0.4 and 1.1 ×10−10
M
⊙ yr −1. The low mass-loss rate is consistent with simultaneous measurements of low mass accretion rate (2.4 ± 0.8 × 10−9
M
⊙ yr−1) for IRAS 16253−2429 from JWST observations, indicating that the protostar is in a quiescent accretion phase. Our results demonstrate that very low-mass protostars can drive highly collimated, atomic jets, even during the quiescent phase.
A Massive Protocluster Anchored by a Luminous Quasar at z = 6.63
Authors: Wang Feige , Yang Jinyi , Hennawi Joseph F. , Fan Xiaohui , Yue Minghao , Bañados Eduardo , Bechtel Shane , Bian Fuyan , Bosman Sarah , Champagne Jaclyn B. , Davies Frederick B. , Decarli Roberto , Farina Emanuele Paolo , Mazzucchelli Chiara , Venemans Bram , Walter Fabian 
Published: February 2024

Abstract
Protoclusters, the progenitors of galaxy clusters, trace large scale structures in the early Universe and are important to our understanding of structure formation and galaxy evolution. To date, only a handful of protoclusters have been identified in the Epoch of Reionization. As one of the rarest populations in the early Universe, distant quasars that host active supermassive black holes are thought to reside in the most massive dark matter halos at that cosmic epoch and could thus potentially pinpoint some of the earliest protoclusters. In this Letter, we report the discovery of a massive protocluster around a luminous quasar at z = 6.63. This protocluster is anchored by the quasar and includes three [C ii] emitters at z ∼ 6.63, 12 spectroscopically confirmed Lyα emitters (LAEs) at 6.54 < z ≤ 6.64, and a large number of narrow-band-imaging selected LAE candidates at the same redshift. This structure has an overall overdensity of

δ
=

3.3

−
0.9

+
1.1

within ∼35 × 74 cMpc2 on the sky and an extreme overdensity of δ > 30 in its central region (i.e., R ≲ 2 cMpc). We estimate that this protocluster will collapse into a galaxy cluster with a mass of

6.9

−
1.4

+
1.2

×

10

15

M

⊙

at the current epoch, more massive than the most massive clusters known in the local Universe such as Coma. In the quasar vicinity, we discover a double-peaked LAE, which implies that the quasar has a UV lifetime greater than 0.8 Myrs and has already ionized its surrounding intergalactic medium.
Comparison of Convolutional Neural Networks and Random Forest Classifiers for Strong Gravitational Lens Identification
Authors: Kothuri Maadhav , Saigal Surain , Ayyalasomayajula Sasidhar 
Published: February 2024

Abstract
Strong gravitational lenses have been instrumental in providing insight into various astronomical problems, including analyzing the dark matter distribution of the universe. Effective identification of these events is made possible through machine learning algorithms, with many recent studies focusing on neural networks. However, very few have investigated the tradeoffs between different algorithms besides neural networks for lens identification. Our paper compares a convolutional neural network (CNN) and a random forest classifier (RFC) to determine the benefits of each for this task. We find that while CNNs do achieve higher accuracy, using RFCs to supplement them could increase the effectiveness of such algorithms. As a result, models that utilize both side-by-side to make predictions may increase in accuracy. This should be explored by future research.