bluuebunny/crossref_metadata_2025_split huggingface dataset:
Growth Pattern of Staphylococcus aureus Bacteria on Blood Agar Plate (BAP) Media Using Human Blood, Chicken Blood, and Sheep Blood
Authors: Krihariyani Dwi 
Published: August 2024

ABSTRACT

Transmission of infection from Staphylococcus aureus bacteria generally occurs in people who have low awareness of maintaining body hygiene, starting with the bacteria entering the skin through scratches and then multiplying causing inflammation. Blood Agar Plate (BAP) is a general medium that is used as a special growth medium to identify certain types of bacteria using the addition of sheep's blood. The aim of this research was to find the growth pattern of Staphylococcus aureus bacteria on Blood Agar Plate (BAP) media which used human blood, chicken blood and sheep blood. Add 5% chicken blood, human blood and sheep blood to the Blood Agar Plate (BAP) then plant Staphylococcus aureus and observe for 24 hours followed by 48 hours. In the 24 hour sample with a total of 27 samples, the results obtained for the number of colonies in sheep blood were 246 x 10-12 CFU/mL, in human blood it was 198.5 x 10-12 CFU/mL, in chicken blood the TBUD results were obtained (Cannot be calculated). In the 48 hour sample with a total of 27 samples, the results obtained for the number of sheep blood colonies were 224.5 x 10-12 CFU/mL, for human blood it was 203 x 10-12 CFU/mL, for chicken blood the results were TBUD (Cannot to be calculated). The macroscopic results are round in shape, grayish white in color, and have a zone of complete hemolysis.
Keywords: Staphylococcus aureus, Blood Agar Plate, blood
ABSTRAK
Penularan infeksi dari bakteri Staphylococcus aureus umumnya terjadi pada masyarakat yang memiliki kesadaran rendah dalam menjaga kebersihan tubuh, diawali dengan masuknya bakteri ke kulit melalui goresan luka kemudian berkembang biak menyebabkan peradangan. Blood Agar Plate (BAP) adalah media umum yang digunakan sebagai media pertumbuhan khusus untuk mengidentifikasi jenis bakteri tertentu menggunakan penambahan darah domba. Tujuan pada penelitian ini untuk mengetahui pola pertumbuhan bakteri Staphylococcus aureus pada media Blood Agar Plate (BAP) yang menggunakan darah manusia, darah ayam, dan darah domba. Ditambahkan sebanyak 5% darah ayam, darah manusia, dan darah domba pada Blood Agar Plate (BAP) lalu ditanam Staphylococcus aureus dan dilakukan pengamatan dalam waktu 24 jam dilanjutkan pada 48 jam. Pada sampel 24 jam dengan total 27 sampel, maka diperoleh hasil pada jumlah koloni pada darah domba sebanyak 246 x 10-12 CFU/mL, pada darah manusia sebanyak 198,5 x 10-12 CFU/mL, pada darah ayam didapatkan hasil TBUD (Tidak Bisa Untuk Dihitung). Pada sampel 48 jam dengan total 27 sampel, diperoleh hasil pada jumlah koloni darah domba sebanyak 224,5 x 10-12 CFU/mL, pada darah manusia sebanyak 203 x 10-12 CFU/mL, pada darah ayam didapatkan hasil TBUD (Tidak Bisa Untuk Dihitung). Hasil makroskopis yaitu berbentuk bulat, berwarna putih keabuan, serta zona hemolisis sempurna.
Kata Kunci : Staphylococcus aureus, Blood Agar Plate, darah
Identificação e mapeamento de áreas infestadas por Capim-annoni (eraglostis plana) através do uso de índice de vegetação no município de Dom Pedrito/RS
Authors: Madruga Farinha Cristhiane , Hanke Daniel , Da Silva Nascimento Shirley Grazieli , Rockenbach de Ávila Mariana , Paz Deble Leonardo 
Published: August 2024

O Eraglostis plana Ness, popularmente conhecido como Capim-annoni, é considerada hoje uma espécie invasora de difícil erradicação dos campos sulinos. O objetivo deste trabalho é avaliar a possibilidade de uso das técnicas aerofotogramétricas como forma de identificação da distribuição do Capim-annoni, de maneira a contribuir no monitoramento da referida planta. Para este trabalho foram realizadas a coleta de informações relativa Ã presença ou não de Capim-annoni a campo, a análise de Índice de Vegetação, a altura de planta e a condutividade elétrica do solo. Os resultados apresentados mostram que o Índice é uma ferramenta promissora na identificação de Capim-annoni por sensoriamento remoto.
Efektifitas Pembelajaran Daring dengan Menggunakan Aplikasi Zoom Meeting di Saat Pandemi Covid-19
Authors: Fathurrahman Fathurrahman 
Published: August 2024

Pandemi Covid-19 telah mengganggu proses pembelajaran secara konvensional. Masalah tersebut diperlukan solusi untuk menjawab permasalahan tersebut. Pembelajaran secara daring adalah salah satu alternatif yang dapat mengatasi masalah tersebut. Tujuan penelitian adalah untuk memperoleh gambaran pelaksanaan pembelajaran daring mata pelajaran Fisika Kelas X SMA Negeri 3 Bondowoso sebagai upaya menekan penyebaran covid-19 di Lingkungan Sekolah. Penelitian ini adalah penelitian survei dengan tipe cross-sectional. Subjek penelitian adalah siswa Kelas X MIPA 1. Data dikumpulkan dengan wawancara melalui zoom cloud meeting. Penelitian dilakukan dengan terlebih dahulu mengadakan survey kepada siswa mengenai penerapan pembelajaran daring. Dengan menggunakan google form, analisis data dilakukan menggunakan teknik analisis interaktif Miles Huberman. Hasil penelitian menunjukkan bahwa: (1) siswa telah memiliki fasilitas-fasilitas dasar yang dibutuhkan untuk mengikuti pembelajaran daring; (2) pembelajaran daring memiliki fleksibilitas dalam pelaksanaannya dan mampu mendorong munculnya kemandirian belajar dan motivasi untuk lebih aktif dalam belajar dan (3) pembelajaran jarak jauh mendorong munculnya perilaku social distancing dan meminimalisir munculnya keramaian siswa sehingga dianggap dapat mengurangi potensi penyebaran Covid-19 di lingkungan sekolah. Tantangan tersendiri dalam pembelajaran daring yaitu lemahnya pengawasan terhadap siswa, kurang kuatnya sinyal di daerah pelosok, dan mahalnya biaya kuota. keuntungan lain dari pembelajaran daring adalah peningkatan kemandirian belajar, minat dan motivasi, keberanian mengemukakan gagasanÂ serta pertanyaan.
Impediments to Effective Leadership in Public Service: A Case of Administrative and Political Challenges in County Governments in Kenya
Authors: Barasa Didmus Wekesa , Omariba Alice 
Published: August 2024

This study addresses the substantial challenges facing leadership effectiveness in Kenya's county governments, focusing on bureaucratic inertia, political interference, resource limitations, and issues with meritocratic appointments that undermine governance and public trust. The research aimed to comprehensively analyze these barriers and propose actionable strategies for improvement. What are the primary administrative impediments to effective leadership in public service within county governments in Kenya? How do political dynamics influence leadership effectiveness in the public service sector at the county level? And what strategies can be implemented to overcome these impediments and enhance leadership effectiveness in county governments? The research questions were: Grounded in theories of transformational and transactional leadership the study explores the contrast between these leadership styles in overcoming the identified challenges. The study employs a mixed-methods approach. Qualitative data from interviews and case studies, alongside quantitative insights gathered through surveys of county officials, public servants, and community leaders, provide a holistic perspective. Purposive sampling ensured diverse participant viewpoints were captured because it allows for targeted sampling. Key findings using Likert scale of 1-5 underscore significant impediments to effective leadership: bureaucratic inertia (rated 4.0), political interference (3.9), resource constraints (3.8), insufficient training (3.7), and political appointments lacking meritocracy (4.2), corruption (4.1), fraudulent academic credentials (3.5), patronage (3.8), and tribalism (3.7). These findings reveal systemic challenges that hinder leadership effectiveness and governance outcomes. In conclusion, entrenched bureaucratic practices, external political pressures, and systemic flaws in leadership appointments hinder effective governance in Kenyan county governments. Addressing these issues necessitates comprehensive reforms, including transparent appointment processes, strengthened anti-corruption measures, strategic resource allocation, and enhanced professional development for public service leaders. From the findings the study recommends implementing transparent and merit-based appointment systems, bolstering anti-corruption efforts, prioritizing targeted resource allocation, and investing in continuous leadership development programs. These measures are crucial for fostering transparency, accountability, and sustainable development in Kenya's county governments
Pola Struktur Gaya Bahasa Tasybīh dalam Al-Qur'an
Authors: Ilham Muhammad Arifin , Hibatullah Fairuz Azhar , Sopian Asep , Nurmala Mia 
Published: August 2024

This research aims to determine the structural analysis of the tasybih language style in the verses of the Al-Qur'an. With a literature study approach, the qualitative method collects data by understanding and studying theories from various relevant literature sources. The main data source in this research is the Al-Qur'an, while additional data sources were obtained from various journals and research articles about Tasybih. Next, data from these research sources will be classified to find several Qur'an verses containing Tasybih. After the data from the research source is presented, the final step is to verify or conclude from the data that has been collected. At this stage, analysis is carried out to identify Koran verses containing Tasybih. The research results show that although Bayan Science has several discussion branches, Tasybih has its function and characteristics. There are similarities in the structure of the 7 Tasybih verses in the Al-Qur'an studied: they are all in the form of mujmal tasybih. It is hoped that this research can provide a deeper understanding of Tasybih and contribute to the study of Arabic linguistics and literature in general.
Automatic Detection of Large-scale Flux Ropes and Their Geoeffectiveness with a Machine-learning Approach
Authors: Pal Sanchita , G. dos Santos Luiz F. , Weiss Andreas J. , Narock Thomas , Narock Ayris , Nieves-Chinchilla Teresa , Jian Lan K. , Good Simon W. 
Published: August 2024

Abstract
Detecting large-scale flux ropes (FRs) embedded in interplanetary coronal mass ejections (ICMEs) and assessing their geoeffectiveness are essential, since they can drive severe space weather. At 1 au, these FRs have an average duration of 1 day. Their most common magnetic features are large, smoothly rotating magnetic fields. Their manual detection has become a relatively common practice over decades, although visual detection can be time-consuming and subject to observer bias. Our study proposes a pipeline that utilizes two supervised binary classification machine-learning models trained with solar wind magnetic properties to automatically detect large-scale FRs and additionally determine their geoeffectiveness. The first model is used to generate a list of autodetected FRs. Using the properties of the southward magnetic field, the second model determines the geoeffectiveness of FRs. Our method identifies 88.6% and 80% of large-scale ICMEs (duration ≥ 1 day) observed at 1 au by the Wind and the Solar TErrestrial RElations Observatory missions, respectively. While testing with continuous solar wind data obtained from Wind, our pipeline detected 56 of the 64 large-scale ICMEs during the 2008–2014 period (recall = 0.875), but also many false positives (precision = 0.56), as we do not take into account any additional solar wind properties other than the magnetic properties. We find an accuracy of 0.88 when estimating the geoeffectiveness of the autodetected FRs using our method. Thus, in space-weather nowcasting and forecasting at L1 or any planetary missions, our pipeline can be utilized to offer a first-order detection of large-scale FRs and their geoeffectiveness.
Effects of Radiative Transfer on the Observed Anisotropy in Magnetohydrodynamic Turbulent Molecular Simulations
Authors: Hernández-Padilla D. , Esquivel A. , Lazarian A. , Velázquez P. F. , Cho J. 
Published: August 2024

Abstract
We study the anisotropy of centroid and integrated intensity maps with synthetic observations. We perform postprocess radiative transfer including the optically thick regime that was not covered in Hernández-Padilla et al. We consider the emission in various CO molecular lines that range from optically thin to optically thick (12CO, 13CO, C18O, and C17O). The results for the velocity centroids are similar to those in the optically thin case. For instance, the anisotropy observed can be attributed to the Alfvén mode, which dominates over the slow and fast modes when the line of sight is at a high inclination with respect to the mean magnetic field. A few differences arise in the models with higher opacity, where some dependence on the sonic Mach number becomes evident. In contrast to the optically thin case, maps of integrated intensity become more anisotropic in optically thick lines. In this situation the scales probed are restricted, due to absorption, to smaller scales, which are known to be more anisotropic. We discuss how the sonic Mach number can affect the latter results, with highly supersonic cases exhibiting a lower degree of anisotropy.
A Census of the Deep Radio Sky with the VLA. I. 10 GHz Survey of the GOODS-N Field*
Authors: Jiménez-Andrade Eric F. , Murphy Eric J. , Momjian Emmanuel , Condon James J. , Chary Ranga-Ram , Taylor Russ , Dickinson Mark 
Published: August 2024

Abstract
We present the first high-resolution, high-frequency radio continuum survey that fully maps an extragalactic deep field: the 10 GHz survey of the Great Observatories Origins Deep Survey-North (GOODS-N) field. This is a Large Program of the Karl G. Jansky Very Large Array (VLA) that allocated 380 hr of observations using the X-band (8–12 GHz) receivers, leading to a 10 GHz mosaic of the GOODS-N field with an average rms noise σ
n = 671 nJy beam−1 and angular resolution θ
1/2 = 0.″22 across 297 arcmin2. To maximize the brightness sensitivity we also produce a low-resolution mosaic with θ
1/2 = 1.″0 and σ
n = 968 nJy beam−1, from which we derive our master catalog containing 256 radio sources detected with peak signal-to-noise ratio ≥ 5. Radio source size and flux density estimates from the high-resolution mosaic are provided in the master catalog as well. The total fraction of spurious sources in the catalog is 0.75%. Monte Carlo simulations are performed to derive completeness corrections of the catalog. We find that the 10 GHz radio source counts in the GOODS-N field agree, in general, with predictions from numerical simulations/models and expectations from 1.4 and 3 GHz radio counts.
Exploring the Complex Ionization Environment of the Turbulent DM Tau Disk
Authors: Long Deryl E. , Cleeves L. Ilsedore , Adams Fred C. , Andrews Sean , Bergin Edwin A. , Guzmán Viviana V. , Huang Jane , Hughes A. Meredith , Qi Chunhua , Schwarz Kamber , Simon Jacob B. , Wilner David 
Published: August 2024

Abstract
Ionization drives important chemical and dynamical processes within protoplanetary disks, including the formation of organics and water in the cold midplane and the transportation of material via accretion and magnetohydrodynamic flows. Understanding these ionization-driven processes is crucial for understanding disk evolution and planet formation. We use new and archival Atacama Large Millimeter/submillimeter Array observations of HCO+, H13CO+, and N2H+ to produce the first forward-modeled 2D ionization constraints for the DM Tau protoplanetary disk. We include ionization from multiple sources and explore the disk chemistry under a range of ionizing conditions. Abundances from our 2D chemical models are postprocessed using non-LTE radiative transfer, visibility sampling, and imaging, and are compared directly to the observed radial emission profiles. The observations are best fit by a modestly reduced cosmic-ray ionization rate (ζ
CR ∼10−18 s−1) and a hard X-ray spectrum (hardness ratio = 0.3), which we associate with stellar flaring conditions. Our best-fit model underproduces emission in the inner disk, suggesting that there may be an additional mechanism enhancing ionization in DM Tau’s inner disk. Overall, our findings highlight the complexity of ionization in protoplanetary disks and the need for high-resolution multiline studies.
Measurement of Anisotropies in Supernova Remnant Observations and Their Interpretation Using Numerical Models
Authors: Mandal Soham , Duffell Paul C. , Polin Abigail , Milisavljevic Dan 
Published: August 2024

Abstract
Supernova remnants (SNRs) exhibit varying degrees of anisotropy, which have been extensively modeled using numerical methods. We implement a technique to measure anisotropies in SNRs by calculating power spectra from their high-resolution images. To test this technique, we develop 3D hydrodynamical models of SNRs and generate synthetic X-ray images from them. Power spectra extracted from both the 3D models and the synthetic images exhibit the same dominant angular scale, which separates large-scale features from small-scale features due to hydrodynamic instabilities. The angular power spectrum at small length scales during relatively early times is too steep to be consistent with Kolmogorov turbulence, but it transitions to Kolmogorov turbulence at late times. As an example of how this technique can be applied to observations, we extract a power spectrum from a Chandra observation of Tycho’s SNR and compare with our models. Our predicted power spectrum picks out the angular scale of Tycho’s fleecelike structures and also agrees with the small-scale power seen in Tycho. We use this to extract an estimate for the density of the circumstellar gas (n ∼ 0.28 cm−3), consistent with previous measurements of this density by other means. The power spectrum also provides an estimate of the density profile of the outermost ejecta. Moreover, we observe additional power at large scales, which may provide important clues about the explosion mechanism itself.
Occurrence of Kelvin–Helmholtz Instability at Lunar Distance Magnetopause: ARTEMIS Observation
Authors: Feng J. Y. , Zhou Y. , Lu J. Y. , Wang M. , Li J. Y. , Zhang H. X. , Tang F. , Yue F. L. 
Published: August 2024

Abstract
Kelvin–Helmholtz waves can be observed frequently at the near-Earth magnetopause and play an important role in the transport of particles, momentum, and energy from the solar wind to the magnetosphere. This work analyzes the occurrence of Kelvin–Helmholtz instability (KHI) at lunar distance magnetopause, which has not been thoroughly studied currently based on Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun satellite observations, and it also investigates the effect of the upstream solar wind and interplanetary magnetic field (IMF). Statistical results show that (1) the occurrence rate is about 15% of the time at lunar distance, lower than at the flank magnetopause, and (2) the occurrence rate decreases with the magnetoacoustic Mach number, Alfvén Mach number, solar wind velocity, and dynamic pressure but only shows a slightly positive correlation with solar wind density. Unlike at the dayside magnetopause, the occurrence rate of KHI diminishes as the solar wind velocity increases at the lunar distance magnetopause, and (3) the occurrence rate decreases with IMF amplitude and is influenced by IMF orientation. As a function of the IMF clock angle, the occurrence rate reaches its maximum at ∼24% when the clock angle is zero. The statistical results are basically consistent with the currently accepted linear theory of KHI, except for a lower rate for higher-speed solar wind. This work contributes to understanding the excitation and evolution of KHI along the magnetopause and plasma transport process in the tail magnetopause.
Two Models for the Orbital Modulation of Gamma Rays in Cyg X-3
Authors: Dmytriiev Anton , Zdziarski Andrzej A. , Malyshev Denys , Bosch-Ramon Valentí , Chernyakova Maria 
Published: August 2024

Abstract
We model the currently available γ-ray data on Cyg X-3 from the Fermi Large Area Telescope. Thanks to Cyg X-3’s very strong γ-ray activity during 2018–2021, the data quality has significantly improved. We study the strong orbital modulation of the γ-rays observed at high γ-ray fluxes. The modulation, as found earlier, is well modeled by anisotropic Compton scattering of the donor blackbody emission by relativistic electrons in a jet strongly misaligned with respect to the orbital axis. We confirm that this model fits well both the average γ-ray modulation light curve and the spectrum. However, we find that if the jet were aligned with the spin axis of a rotating black hole, it would undergo geodetic precession with a period of ∼50 yr. However, its presence is ruled out by both the γ-ray and radio data. Therefore, we consider an alternative model in which the average jet direction is aligned, but it is bent outside the orbit owing to the thrust of the donor stellar wind, and thus precesses at the orbital period. The γ-ray modulation then appears as a result of the variable Doppler boosting of synchrotron self-Compton jet emission. This model also fits the data well. However, the fitted bending angle is much larger than the theoretical one based on the binary and wind parameters as currently known. Thus, both models disagree with important aspects of our current theoretical understanding of the system. We discuss possible ways to find the correct model.
Likely Detection of GeV γ-Ray Emission from Pulsar Wind Nebula G32.64+0.53 with Fermi-LAT
Authors: Xiao Yifan , Wu Keyao , Fang Jun 
Published: August 2024

Abstract
In this study, we report the likely GeV γ-ray emissions originating from the pulsar PSR J1849-0001's pulsar wind nebula (PWN) G32.64+0.53. Our analysis covers approximately 14.7 yr of data from the Fermi Large Area Telescope Pass 8. The position of the source and its spectrum matches those in X-ray and TeV energy bands, so we propose that the GeV γ-ray source is indicative of PWN G32.64+0.53. We interpret the broadband spectral energy distribution (SED) using a time-dependent one-zone model, which assumes that the multiband nonthermal emission of the target source can be generated by synchrotron radiation and inverse Compton scattering (ICS) of the electrons/positrons. Our findings demonstrate that the model substantially elucidates the observed SED. These results lend support to the hypothesis that the γ-ray source originates from the PWN G32.64+0.53 powered by PSR J1849-0001. Furthermore, the γ-rays in TeV bands are likely generated by electrons/positrons within the nebula through ICS.