bluuebunny/crossref_metadata_2025_split huggingface dataset:
QUÍMICA PARA BAIXINHOS: ABORDAGEM EXPERIMENTAL E LÚDICA PARA O ENSINO DE QUÍMICA A CRIANÇAS DE 5 A 12 ANOS
Authors: Malacarne Majorie Mara , SCARDUA DALMONECH DHÉBORA , JACOB TONN DANIEL , PIRES DALMASCHIO GUILHERME , FRIZERA BORGHI MOTA MARIANA , RODRIGUES PRETTI IRANY 
Published: November 2024

Este trabalho possui o objetivo de promover o contato inicial de crianças e adolescentes de 5 a 12 anos com a Química, para contribuir com seu futuro aprendizado científico e despertar seu interesse pelo componente. Para tal, de setembro de 2019 a setembro de 2020, foram selecionados experimentos de Química considerando: disponibilidade de materiais, manuseio seguro, correlação com cotidiano, ludicidade e faixa etária. Estes foram aplicados em momento científico no Ifes campus Itapina com alunos do ensino municipal de Colatina, publicados na rede social do campus durante o isolamento social da pandemia de COVID-19 e compilados em um e-book que foi utilizado por alunos do quinto ano da escola EMEF João Manoel Meneguelli, durante o ensino remoto. As demonstrações de interesse e entusiasmo observados no momento científico, nas mensagens coletadas nas publicações do Instagram e em relatos de professores da escola João Manoel Meneguelli mostraram boa aceitação desta metodologia de ensino.
INICIAÇÃO CIENTÍFICA NO ENSINO MÉDIO
Authors: Ferreira Picolo Geovana , Kotsuka da Silva Lincoln 
Published: November 2024

O trabalho apresenta um relato de experiência da vivência da iniciação científica (IC) por estudantes do ensino médio de escolas públicas da cidade de Cruzeiro do Oeste, Paraná. Com o objetivo de discutir a IC como metodologia ativa e propô-la como ferramenta de superação do esoterismo, a IC foi dividida em oito etapas e teve como tema a análise do teor de etanol presente na gasolina comercializada na região, considerando a NBR 13992. O trabalho promoveu discussões acerca da IC como metodologia ativa de ensino e ferramenta para a migração do esoterismo para o exoterismo. As discussões permearam diante das características inerentes às correntes teóricas e suas relações com os aspectos observados no ensino-aprendizagem dos participantes do projeto. A partir disso, estabeleceu-se que a IC promoveu resultados alinhados aos princípios das metodologias ativas e contribuiu para remodelar a ideia de ciência esotérica que está presente na sociedade para a concepção de ciência exotérica.
TRATAMENTO DE PITIOSE EM EQUINO
Authors: da Costa Josiane Rosa , Silva Maria Raquel , Barbosa Alves Junior Carlos Donato , Da Silva Martins Jéssica Rayla , De Oliveira Cleber Souza , Ganasevici Fernandes Tatiana , Oliveira Trajano da Silva Maria Bernardete , Dorea Reis Luciano Wagner , Ferreira Alves Heberth Gustavo , De Figueiredo Ventura Sheila 
Published: December 2024

A pitiose é uma doença causada pelo fungo Pythium insidiosumde e gera uma lesão de aspecto granulomatosa, afetando com maior frequência o tecido cutâneo e subcutâneo dos animais domésticos, selvagens e humanos. No dia 12 de junho de 2019 deu entrada na Estância toca da Seriema / Comunidade Morro de São Gerônimo - Cuiabá – MT, em atendimento na área de grandes animais; um equino macho, castrado, com oito anos de idade, apresentando uma lesão circular na região ventral do abdômen, drenando secreção serossanguinolenta, áreas de necrose e presença de pequenos grânulos firmes de coloração amarelada, denominados de “Kunkers”, achado comum em lesões de pitiose, após uma anamnese detalhada e exame físico, foi possível obter o diagnóstico presuntivo para pitiose equina, sendo confirmado posteriormente pelo exame histopatológico. O tratamento instituído para o animal foi com o uso de acetato de triancinolona, 50 mg/animal por via intramuscular com intervalo de 15 dias, em um total de duas aplicações, associados a uma limpeza diária da lesão com clorexidine a 2%, pomada antiótica e repelente spray administrado na aréa adjacentes às bordas da ferida, no período de toda fase de intenação, que foi do dia 20 de maio a 03 de julho. O tratamento resultou em grande melhora na cicatrização, diminuindo o tamanho da lesão prurido, que ficou ausente após 19 dias do início terapêutico, mostrando-se uma ótima alternativa no tratamento da pitiose equina.
The role of biotransformation and chemical structure of drugs in the diagnosis of drug allergies
Authors: Myasnikova T. N. , Smirnov V. V. 
Published: November 2024

Relevance. Despite the fact that the pharmacological effect of drugs is well known and studied, unfortunately, it is impossible to predict the development of drug allergies, since the individual characteristics of the body's reactivity are of great importance in its development. The goal is to analyze the clinical situation of the development of drug allergies to illustrate the importance of the role of biotransformation and the chemical structure of drugs in its diagnosis.Methods. The study was carried out on the patient after signing informed consent and included anamnesis, physical examination, skin prick tests with inhalant allergens, installation of a peripheral venous catheter, and provocative testing.Results. prick tests with: 0.9 % NaCl solution (negative control), histamine solution (10 mg/ml) (positive control), amoxicillin + clavulanic acid (100 mg + 20 mg), ampicillin (100 mg/ml), cephalexin (50 mg/ml) — positive results, ceftazidime (20 mg/ml), clarithromycin (20 mg/ml) — negative results; intravenous tests with: 0.9 % NaCl solution (negative control), ceftazidime (2 mg/ml), clarithromycin (0.01 mg/ml) — negative results; oral PDT with cefuroxime (cumulative dose — 250 mg), josamycin (cumulative dose — 1000 mg) — negative results. As a result of skin testing, LA for the amino group of beta-lactams was confirmed; No data have been obtained for LA on the beta-lactam ring, clavulanic acid, or macrolides.
Characterizing the Broadband Reflection Spectrum of MAXI J1803-298 during Its 2021 Outburst with NuSTAR and NICER
Authors: Adegoke Oluwashina K. , García Javier A. , Connors Riley M. T. , Ding Yuanze , Mastroserio Guglielmo , Steiner James F. , Ingram Adam , Harrison Fiona A. , Tomsick John A. , Kara Erin , Mehdipour Missagh , Fukumura Keigo , Stern Daniel , Ubach Santiago , Lucchini Matteo 
Published: November 2024

Abstract
MAXI J1803-298 is a transient black hole candidate discovered in 2021 May during an outburst that lasted several months. Multiple X-ray observations reveal recurring “dipping” intervals in several of its light curves, particularly during the hard/intermediate states, with a typical recurrence period of ∼7 hr. We report analysis of four NuSTAR observations of the source, supplemented with NICER data where available, over the duration of the outburst evolution covering the hard, intermediate, and the soft states. Reflection spectroscopy reveals the black hole to be rapidly spinning (a
* = 0.990 ± 0.001) with a near edge-on viewing angle (i = 70° ± 1°). Additionally, we show that the light-curve dips are caused by photoelectric absorption from a moderately ionized absorber whose origin is not fully understood, although it is likely linked to material from the companion star impacting the outer edges of the accretion disk. We further detect absorption lines in some of the spectra, potentially associated with Fe xxv and Fe xxvi, indicative of disk winds with moderate to extreme velocities. During the intermediate state and just before transitioning into the soft state, the source showed a sudden flux increase, which we found to be dominated by soft disk photons and consistent with the filling of the inner accretion disk, at the onset of state transition. In the soft state, we show that models of disk self-irradiation provide a better fit and a preferred explanation to the broadband reflection spectrum, consistent with previous studies of other accreting sources.
Neural Network Constraints on the Cosmic-Ray Ionization Rate and Other Physical Conditions in NGC 253 with ALCHEMI Measurements of HCN and HNC
Authors: Behrens Erica , Mangum Jeffrey G. , Viti Serena , Holdship Jonathan , Huang Ko-Yun , Bouvier Mathilde , Butterworth Joshua , Eibensteiner Cosima , Harada Nanase , Martín Sergio , Sakamoto Kazushi , Muller Sebastien , Tanaka Kunihiko , Colzi Laura , Henkel Christian , Meier David S. , Rivilla Víctor M. , van der Werf Paul P. ,   ALMA Comprehensive High-resolution Extragalactic Molecular Inventory (ALCHEMI) collaboration
Published: November 2024

Abstract
We use a neural network model and Atacama Large Millimeter/submillimeter Array (ALMA) observations of HCN and HNC to constrain the physical conditions, most notably the cosmic-ray ionization rate (CRIR, ζ), in the Central Molecular Zone (CMZ) of the starburst galaxy NGC 253. Using output from the chemical code UCLCHEM, we train a neural network model to emulate UCLCHEM and derive HCN and HNC molecular abundances from a given set of physical conditions. We combine the neural network with radiative transfer modeling to generate modeled integrated intensities, which we compare to measurements of HCN and HNC from the ALMA Large Program ALCHEMI. Using a Bayesian nested sampling framework, we constrain the CRIR, molecular gas volume and column densities, kinetic temperature, and beam-filling factor across NGC 253's CMZ. The neural network model successfully recovers UCLCHEM molecular abundances with ∼3% error and, when used with our Bayesian inference algorithm, increases the parameter-inference speed tenfold. We create images of these physical parameters across NGC 253's CMZ at 50 pc resolution and find that the CRIR, in addition to the other gas parameters, is spatially variable with ζ ∼ a few ×10−14 s−1 at r ≳ 100 pc from the nucleus, increasing to ζ > 10−13 s−1 at its center. These inferred CRIRs are consistent within 1 dex with theoretical predictions based on nonthermal emission. Additionally, the high CRIRs estimated in NGC 253's CMZ can be explained by the large number of cosmic-ray-producing sources as well as a potential suppression of cosmic-ray diffusion near their injection sites.
Turbulent Pressure Heats Gas and Suppresses Star Formation in Galactic Bar Molecular Clouds
Authors: Nilipour Andy , Ott Juergen , Meier David S. , Svoboda Brian , Sormani Mattia C. , Ginsburg Adam , Gramze Savannah R. , Butterfield Natalie O. , Klessen Ralf S. 
Published: November 2024

Abstract
The Central Molecular Zone (CMZ) of the Milky Way is fed by gas inflows from the Galactic disk along almost radial trajectories aligned with the major axis of the Galactic bar. However, despite being fundamental to all processes in the nucleus of the Galaxy, these inflows have been studied significantly less than the CMZ itself. We present observations of various molecular lines between 215 and 230 GHz for 20 clouds with ∣ℓ∣ < 10°, which are candidates for clouds in the Galactic bar due to their warm temperatures and broad lines relative to typical Galactic disk clouds, using the Atacama Large Millimeter/submillimeter Array Atacama Compact Array. We measure gas temperatures, shocks, star formation rates, turbulent Mach numbers, and masses for these clouds. Although some clouds may be in the Galactic disk despite their atypical properties, nine clouds are likely associated with regions in the Galactic bar, and in these clouds, turbulent pressure is suppressing star formation. In clouds with no detected star formation, turbulence is the dominant heating mechanism, whereas photoelectric processes heat the star-forming clouds. We find that the ammonia (NH3) and formaldehyde (H2CO) temperatures probe different gas components, and in general, each transition appears to trace different molecular gas phases within the clouds. We also measure the CO-to-H2 X-factor in the bar to be an order of magnitude lower than the typical Galactic value. These observations provide evidence that molecular clouds achieve CMZ-like properties before reaching the CMZ.
BD+44°493: Chemo-dynamical Analysis and Constraints on Companion Planetary Masses from WIYN/NEID Spectroscopy*
Authors: Placco Vinicius M. , Gupta Arvind F. , Almeida-Fernandes Felipe , Logsdon Sarah E. , Rajagopal Jayadev , Holmbeck Erika M. , Roederer Ian U. , Della Costa John , Fernandez Pipa , Golub Eli , Higuera Jesus , Patel Yatrik , Ridgway Susan , Schweiker Heidi 
Published: November 2024

Abstract
In this work, we present high-resolution (R ∼ 100,000), high signal-to-noise ratio (S/N ∼ 800) spectroscopic observations for the well-known, bright, extremely metal-poor, carbon-enhanced star BD+44°493. We determined chemical abundances and upper limits for 17 elements from WIYN/NEID data, complemented with 11 abundances redetermined from Subaru and Hubble data, using the new, more accurate, stellar atmospheric parameters calculated in this work. Our analysis suggests that BD+44°493 is a low-mass (0.83 M
⊙), old (12.1–13.2 Gyr) second-generation star likely formed from a gas cloud enriched by a single metal-free 20.5 M
⊙ Population III star in the early Universe. With a disk-like orbit, BD+44°493 does not appear to be associated with any major merger event in the early history of the Milky Way. From the precision radial-velocity NEID measurements (median absolute deviation = 16 m s−1), we were able to constrain companion planetary masses around BD+44°493 and rule out the presence of planets as small as

m
sin
i
=
2

M
J out to periods of 100 days. This study opens a new avenue of exploration for the intersection between stellar archaeology and exoplanet science using NEID.
GOALS-JWST: The Warm Molecular Outflows of the Merging Starburst Galaxy NGC 3256
Authors: Bohn Thomas , Inami Hanae , Togi Aditya , Armus Lee , Lai Thomas S.-Y. , Barcos-Munoz Loreto , Song Yiqing , Linden S. T. , Surace Jason , Bianchin Marina , U Vivian , Evans Aaron S. , Böker Torsten , Malkan Matthew A. , Larson Kirsten L. , Stierwalt Sabrina , Buiten Victorine A. , Charmandaris Vassilis , Diaz-Santos Tanio , Howell Justin H. , Privon George C. , Ricci Claudio , van der Werf Paul P. , Aalto Susanne , Hayward Christopher C. , Kader Justin A. , Mazzarella Joseph M. , Muller-Sanchez Francisco , Sanders David B. 
Published: November 2024

Abstract
We present James Webb Space Telescope (JWST) integral-field spectrograph observations of NGC 3256, a local infrared-luminous late-stage merging system with two nuclei roughly 1 kpc apart, both of which have evidence of cold molecular outflows. Using JWST/NIRSpec and Mid-Infrared Instrument data sets, we investigate this morphologically complex system on spatial scales of <100 pc, where we focus on the warm molecular H2 gas surrounding the nuclei. We detect collimated outflowing warm H2 gas originating from the southern nucleus, though we do not find significant outflowing H2 gas surrounding the northern nucleus. We measure maximum intrinsic outflow velocities of ∼1000 km s−1, which extend out to a distance of 0.7 kpc. Based on H2 S(7)/S(1) ratios, we find a larger fraction of warmer gas near the southern nucleus, which decreases with increasing distance from the nucleus, signifying the southern nucleus as a primary source of H2 heating. The gas mass of the warm H2 outflow component is estimated to be M
warm
,out = (1.4 ± 0.2) × 106
M
⊙, as much as 6% of the cold H2 mass estimated using Atacama Large Millimeter/submillimeter Array CO data. The outflow timescale is about 7 × 105 yr, resulting in a mass outflow rate

M
̇

warm
,
out

=
2.0
±
0.8

M
⊙

yr

−
1

and kinetic power P
warm,out ∼ 4 × 1041 erg s−1. Lastly, regions within our 3.″0 × 3.″0 NIRSpec data, where the outflowing gas reside show high [Fe ii]/Paβ and H2/Brγ line ratios, indicate enhanced mechanical heating caused by the outflows. The fluxes and ratios of polycyclic aromatic hydrocarbons (PAHs) in these regions are not significantly different compared to those elsewhere in the disk, suggesting the outflows may not significantly alter the PAH ionization state or grain size.
Constraints on Common Envelope Ejection from Double Helium White Dwarfs
Authors: Zhang Yangyang , Li Zhenwei , Chen Xuefei , Han Zhanwen 
Published: November 2024

Abstract
Double helium white dwarfs (He WDs) are a type of gravitational wave source and are greatly important in studies of binary interaction, particularly in common envelope (CE) ejection physics. Most double He WDs with mass ratios of q ∼ 1 are formed through a particular channel. In this channel, one He WD is initially produced from a red giant (RG) with a degenerate core via stable Roche lobe overflow, and another He WD is formed from an RG with a degenerate core via CE ejection. They may have significant implications for binary evolution processes but have not received specific studies, especially for the CE phase. This paper adopts a semianalytic method and a detailed stellar evolution simulation to model the formation of double He WDs. We find that most double He WDs show mass ratios slightly greater than 1, and their orbital period–mass ratio relations are broadly consistent with observations. There is also a relation between the mass ratios and progenitor masses of the He WDs produced via CE ejection for double He WDs with determined WD masses. Based on this relation, the mass of the He WD progenitor can be inferred from the mass ratio. Then, the CE ejection efficiency can be constrained with the orbital period. In addition, we constrain the CE ejection efficiency for two double He WDs, J1005-2249 and WD0957-666. The results show that the CE ejection efficiencies increase with the WD progenitor masses.
Multiwavelength Emission from Jets and Magnetically Arrested Disks in Nearby Radio Galaxies: Application to M87
Authors: Kuze Riku , Kimura Shigeo S. , Toma Kenji 
Published: November 2024

Abstract
Radio galaxies are a subclass of active galactic nuclei that drive relativistic jets from their center and are observed in radio to very-high-energy gamma rays. The emission mechanisms and regions are still unknown. High-energy gamma rays can be explained by the emission from the magnetically arrested disks (MADs) around the central supermassive black hole (BH), for which the magnetic flux threading the BH is in a saturation level, although the emission from the MADs does not explain the optical and X-ray data. We construct a two-zone multiwavelength emission model in which optical and X-rays come from jets, while millimeter/submillimeter and gamma rays come from MADs. Our model takes into account the particle injection by the magnetic reconnection at the jet base close to the BH and particle entrainment from the ambient gas at the jet emission zone. We apply our model to M87 and find that our model can explain the simultaneous multiwavelength data, except for the radio data, which could be explained if we extend our one-zone emission model to a one-dimensional one. We also find that the strong plasma entrainment is necessary to explain the multiwavelength data. Our model will be tested by variability analysis among the multiwavelength data.
Water Enrichment from Pebble Drift in Disks with Gap-forming Planets
Authors: Easterwood Whittney , Kalyaan Anusha , Banzatti Andrea 
Published: November 2024

Abstract
Volatiles like H2O are present as ice in solids in the cold outer regions of protoplanetary disks and as vapor in the warm inner regions within the water snow line. Icy pebbles drifting inwards from the outer disk sublimate after crossing the snow line, enriching the inner disk with solid mass and water vapor. Meanwhile, protoplanets forming within the disk open gaps in the disk gas, creating traps against the inward drift of pebbles and in turn reducing water enrichment in the inner disk. Recent disk observations from millimeter interferometry and infrared spectroscopy have supported this broad picture by finding a correlation between the outer radial distribution of pebbles and the properties of inner water vapor spectra. In this work, we aim at further informing previous and future observations by building on previous models to explore pebble drift in disks with multiple gaps. We systematically explore multiple gap locations and their depths (equivalent to the specific masses of planets forming within), and different particle sizes to study their impact on inner disk water enrichment. We find that the presence of close-in deep gaps carved by a Jupiter-mass planet is likely crucial for blocking icy pebble delivery into the inner disk, while planets with lower masses only provide leaky traps. We also find that disks with multiple gaps show lower vapor enrichment in the inner disk. Altogether, these model results support the idea that inner disk water delivery and planet formation are regulated by the mass and location of the most massive planets.
Mass Function of Stellar Black Holes as Revealed by the LIGO–Virgo–KAGRA Observations
Authors: Dong Xiao-Fei , Huang Yong-Feng , Zhang Zhi-Bin , Li Xiu-Juan , Zou Ze-Cheng , Hu Chen-Ran , Deng Chen , Liu Yang 
Published: November 2024

Abstract
Ninety gravitational-wave events have been detected by the LIGO–Virgo–KAGRA network and are released in the Gravitational-Wave Transient Catalog. Among these events, 83 cases are definitely binary black hole mergers, since the masses of all the objects involved significantly exceed the upper limit of neutron stars. The black holes in these merger events naturally form two interesting samples, a premerger sample that includes all the black holes before the mergers and a postmerger sample that consists of the black holes generated during the merging processes. The former represents black holes that once existed in the Universe, while the latter represents newly born black holes. Here we present a statistical analysis of these two samples. The nonparametric τ statistic method is adopted to correct for the observational selection effect. The Lynden-Bell C
− method is further applied to derive the mass distribution and density function of black holes. It is found that the mass distribution can be expressed as a broken power-law function. More interestingly, the power-law index in the high-mass region is comparable for the two samples. The number density of black holes is found to depend on redshift as ρ(z) ∝ z
−2.06—z
−2.12 based on the two samples. The implications of these findings on the origin of black holes are discussed.
Estimating the Masses of Supercluster-scale Filaments from Redshift Dispersions
Authors: Crone Odekon Mary , Viscardi Trevor W. , Rabinowitz Jake , Young Brandon 
Published: November 2024

Abstract
We present a strategy for estimating the mass per unit length along supercluster-scale filaments that are oriented across the sky, based on mock redshift surveys of 264 filaments from the Millennium simulation. In our fiducial scenario, we place each simulated filament at a distance of 300 Mpc, perpendicular to the line of sight, and calculate the redshift dispersion using galaxies with magnitudes r < 19.5. Some regions are dynamically complicated in ways that interfere with finding a simple relationship between dispersion σ and linear mass density μ. However, by examining individual overlapping segments along the filaments, we find a relationship that allows us to successfully predict

log
μ

from

log
σ

with a scatter of about ±0.20 dex, for ∼70% of the regions along filaments. This relationship is robust to changes in the distance to the filament if the physical segment length and the absolute magnitude for galaxy selection are held constant. The relationship between redshift dispersion and mass is similar to that obtained for a simple analytical model where filaments are dynamically relaxed, and we examine the possibility that the galaxies are indeed relaxed within the gravitational potential of the filament. We find that this is not the case; galaxy dynamics are strongly affected by infall to the filament and by orbits within groups and clusters.