bluuebunny/crossref_metadata_2025 huggingface dataset:
Pembuatan Logo Untuk UMKM Ibu Vivi di Desa Weru Lor
Authors: Haikal Avicenna  , Dinda Rizka Yunita  , Aris Riyanto  , Muhammad Furqon
Published: October 2024

This study aims to design and develop a logo for the SME "Warung Ibu Vivi" located in Weru Lor as part of an effort to enhance its visual identity and competitiveness. In today's globalized era, having a strong and appealing visual identity is essential for any business, including SMEs, to attract consumer attention and distinguish itself from competitors. The methods used in this service project include needs analysis, logo creation, finalization, and implementation. The design process involves active participation from the business owner to ensure that the logo aligns with the vision and values of "Warung Ibu Vivi". The final output of this project is a logo that effectively represents the SME's identity and a banner that incorporates the new logo. The new logo and banner are expected to improve brand awareness and increase the appeal of "Warung Ibu Vivi" to potential customers, thereby contributing to increased sales and business growth.
Pengaruh Manajemen Keuangan Terhadap Efektivitas dan Efisiensi Lembaga PAUD
Authors: Rahman Lutfi Kausar , Suhendar Asep Dadan , Fauzia Annisa Eka
Published: October 2024

Most PAUD Institutions are still obstacles in managing their finances, especially for small-scale institutions. The importance of financial management is applied well to be able to allow PAUD institutions to allocate each resource its resources effectively and efficiently. So the purpose of this study was to investigate and analyze the influence of financial management on the effectiveness and efficiency of the PAUD Agency, especially in Nurun Nisa TK. The method used is qualitative, because researchers do not use questionnaires in performing their research, and by using a comparaive research approach, namely understanding the cause-effect relationship between financial management, effectiveness, and efficiency. Data collection techniques were carried out through interviews, direct observation and analyzed financial statements on Nisa's Nurun Nisa. The results showed that there was a positive relationship between financial management practices and good level of effectiveness and PAUD agency efficiency in Nurun Nisa TK. There has been an increase in each July-December 2022 and January-June 2023, with the percentage of effectiveness ratios from 88.41% to 91.55%, revenue efficiency from 66.1% to 58.99%, and operational efficiency of 82.11% to 77.01%. So the existence of good level of effectiveness and efficiency in Nurun Nisa TK provides concrete evidence that the optimal implementation of financial management can directly contribute to increased effectiveness of education quality and resource use efficiency.
CORINOS. II. JWST-MIRI Detection of Warm Molecular Gas from an Embedded, Disk-bearing Protostar
Authors: Salyk Colette , Yang Yao-Lun , Pontoppidan Klaus M. , Bergner Jennifer B. , Okoda Yuki , Kim Jaeyeong , Evans Neal J. , Cleeves Ilsedore , van Dishoeck Ewine F. , Garrod Robin T. , Green Joel D.
Published: October 2024

We present James Webb Space Telescope (JWST) Mid-InfraRed Instrument (MIRI) observations of warm CO and H2O gas in emission toward the low-mass protostar IRAS 15398-3359, observed as part of the CORINOS program. The CO is detected via the rovibrational fundamental band and hot band near 5 μm, whereas the H2O is detected in the rovibrational bending mode at 6–8 μm. Rotational analysis indicates that the CO originates in a hot reservoir with an excitation temperature of 1598 ± 118 K, while the water is much cooler at 204 ± 7 K. Neither the CO nor the H2O line images are significantly spatially extended, constraining the emission to within ∼40 au of the protostar. The compactness and high temperature of the CO are consistent with an origin in the embedded protostellar disk, or in a compact disk wind. In contrast, the water must arise from a cooler region and requires a larger emitting area (compared to the CO) to produce the observed fluxes. The water may arise from a more extended part of the disk, or from the inner portion of the outflow cavity. Thus, the origin of the molecular emission observed with JWST remains ambiguous. Better constraints on the overall extinction, comparison with realistic disk models, and future kinematically resolved observations may all help to pinpoint the true emitting reservoirs.
The Local Group L-band Survey: The First Measurements of Localized Cold Neutral Medium Properties in the Low-metallicity Dwarf Galaxy NGC 6822
Authors: Pingel Nickolas M. , Chen Hongxing , Stanimirović Snežana , Koch Eric W. , Leroy Adam K. , Rosolowsky Erik , Kim Chang-Goo , Dalcanton Julianne J. , Walter Fabian , Busch Michael P. , Chown Ryan , Donovan Meyer Jennifer , Eibensteiner Cosima , Hunter Deidre A. , Sarbadhicary Sumit K. , Tarantino Elizabeth , Villanueva Vicente , Williams Thomas G.
Published: October 2024

Measuring the properties of the cold neutral medium (CNM) in low-metallicity galaxies provides insights into heating and cooling mechanisms in early Universe-like environments. We report detections of two localized atomic neutral hydrogen (H i) absorption features in NGC 6822, a low-metallicity (0.2 Z
⊙) dwarf galaxy in the Local Group. These are the first unambiguous CNM detections in a low-metallicity dwarf galaxy outside the Magellanic Clouds. The Local Group L-band Survey (LGLBS) enabled these detections, due to its high spatial (15 pc for H i emission) and spectral (0.4 km s−1) resolution. We introduce LGLBS and describe a custom pipeline for searching for H i absorption at high angular resolution and extracting associated H i emission. A detailed Gaussian decomposition and radiative transfer analysis of the NGC 6822 detections reveals five CNM components, with key properties: a mean spin temperature of 32 ± 6 K, a mean CNM column density of 3.1 × 1020 cm−2, and CNM mass fractions of 0.33 and 0.12 for the two sightlines. Stacking nondetections does not reveal low-level signals below our median optical depth sensitivity of 0.05. One detection intercepts a star-forming region, with the H i absorption profile encompassing the CO (2−1) emission, indicating coincident molecular gas and a depression in high-resolution H i emission. We also analyze a nearby sightline with deep, narrow H i self-absorption dips, where the background warm neutral medium is attenuated by intervening CNM. The association of CNM, CO, and Hα emissions suggests a close link between the colder, denser H i phase and star formation in NGC 6822.
GRB Progenitor Classification from Gamma-Ray Burst Prompt and Afterglow Observations
Authors: Nuessle P. , Racusin J. L. , White N. E.
Published: October 2024

Using an established classification technique, we leverage standard observations and analyses to predict the progenitors of gamma-ray bursts (GRBs). This technique, utilizing support vector machine statistics, provides a more nuanced prediction than the previous two-component Gaussian mixture in duration of the prompt gamma-ray emission. Based on further covariance testing from Fermi/Gamma Ray Burst Monitor, Swift/Burst Alert Telescope, and Swift/X-Ray Telescope data, we find that our classification based only on prompt emission properties gives perspective on the recent evidence that mergers and collapsars exist in both “long” and “short” GRB populations.
Flare-accelerated Electrons in the Kappa Distribution from X-Ray Spectra with the Warm-target Model
Authors: Luo 骆 Yingjie 英杰 , Kontar Eduard P. , Bhattacharjee Debesh
Published: October 2024

X-ray observations provide important and valuable insights into the acceleration and propagation of nonthermal electrons during solar flares. Improved X-ray spectral analysis requires a deeper understanding of the dynamics of energetic electrons. Previous studies have demonstrated that the dynamics of accelerated electrons with a few thermal speeds are more complex than those with significantly higher speeds. To better describe the energetic electrons after injection, a model considering energy diffusion and thermalization effects in flare conditions (the warm-target model) has recently been developed for spectral analysis of hard X-rays. This model has demonstrated how the low-energy cutoff, which can hardly be constrained in cold-target modeling, can be determined. However, the power-law form may not be the most suitable representation of injected electrons. The kappa distribution, which is proposed as a physical consequence of electron acceleration, has been applied successfully in RHESSI spectral analysis. In this study, we employ the kappa-form injected electrons in the warm-target model to analyze two M-class flares, observed by RHESSI and the Spectrometer/Telescope for Imaging X-rays, respectively. The best-fit results show that the kappa-form energetic electron spectrum generates lower nonthermal energy than the power-law form when producing a similar photon spectrum in the fit range. We also demonstrated that the fit parameters associated with the kappa-form electron spectrum can be well determined with small uncertainty. Further, the kappa distribution, which covers the entire electron energy range, enables the determination of key electron properties such as total electron number density and average energy at the flare site, providing valuable information on electron acceleration processes.
Exploring Filament Galaxies Using AstroSat/UVIT
Authors: Pandey Divya , Saha Kanak , Pradhan Ananta C.
Published: October 2024

We present results from our deep far-ultraviolet (FUV) survey using AstroSat/UVIT of a filamentary structure at z ∼0.072. A total of four filaments comprising 58 galaxies were probed in our study. We detect 18 filament galaxies in our FUV observation. All filament galaxies are further classified based on their photometric color, nuclear activity, and morphology. The filaments contain galaxies with mixed stellar population types and structures. We do not detect galaxies in our UVIT survey up to a distance of 0.4 Mpc h
−1 from the filament axis, implying a lack of recent star formation in the inner region of filaments. The FUV star formation rate (SFR) for star-forming galaxies agrees well with the SFR144MHz calculated using Low-Frequency Array radio-continuum observations. We witness an increase in the FUV specific-SFR (sSFR) of filament galaxies with increasing distance from the filament spine (D
fil). The intermediate-to-high stellar mass filament galaxies were more star-forming than cluster galaxies in a fixed stellar mass bin. The FUV morphology of some filament galaxies detected in the filament outskirts (D
fil ≳ 0.7 Mpc h
−1) is comparable to or slightly extended than their optical counterpart. The mass assembly of galaxies examined by estimating (FUV − r) color gradients shows that more “red-cored’ galaxies reside in the outer region of the filaments. Our results prove that the likelihood of merger interaction and gas starvation increases when approaching the filament spine. We report a definitive and inhomogeneous impact of filaments on the galaxies residing inside them.
A Framework for Incorporating Binding Energy Distribution in Gas-ice Astrochemical Models
Authors: Furuya Kenji
Published: October 2024

One of the most serious limitations of current astrochemical models with the rate equation (RE) approach is that only a single type of binding site is considered in grain surface chemistry, although laboratory and quantum chemical studies have found that surfaces contain various binding sites with different potential energy depths. When various sites exist, adsorbed species can be trapped in deep potential sites, increasing the resident time on the surface. On the other hand, adsorbed species can be populated in shallow sites, activating thermal hopping and thus two-body reactions even at low temperatures, where the thermal hopping from deeper sites is not activated. Such behavior cannot be described by the conventional RE approach. In this work, I present a framework for incorporating various binding sites (i.e., binding energy distribution) in gas-ice astrochemical models as an extension of the conventional RE approach. I propose a simple method to estimate the probability density function (pdf) for the occupation of various sites by adsorbed species, assuming a quasi-steady state. By using thermal desorption and hopping rates weighted by the pdfs, the effect of binding energy distribution is incorporated into the RE approach without increasing the number of ordinary differential equations to be solved. This method is found to be accurate and computationally efficient, and enables us to consider binding energy distribution even for a large gas-ice chemical network which contains hundreds of icy species. The impact of the binding energy distribution on interstellar ice composition is discussed quantitatively for the first time.
Host Galaxy Properties of Gamma-Ray Bursts Involving Neutron Star Binary Mergers and Their Impact on Kilonovae Rates
Authors: Jeong Mankeun , Im Myungshin
Published: October 2024

In the upcoming gravitational-wave (GW) observing runs, identifying host galaxies is crucial as it provides essential redshift information and enables the use of GW events as standard sirens. However, pinpointing host galaxies remains challenging due to the large localization uncertainties and the rapidly fading nature of their optical counterparts. Analyzing the host galaxies of short gamma-ray bursts (sGRBs) offers an alternative approach to deepen our understanding of the environments where binary neutron stars (BNS) primarily merge. This study compiles archival photometric data for the host galaxies of 76 sGRBs and four hybrid GRBs that are long GRBs accompanied by kilonova-like signals. We use this data to evaluate their physical properties through spectral energy distribution fitting. To assess the characteristics of the host galaxies, we utilized a volume-limited sample (z < 0.5) from the COSMOS field as a control group. Contrary to expectations that the BNS merger rate is proportional to host stellar mass, the short and hybrid GRB population appears less massive than the mass-weighted distribution of the control sample. Instead, we propose a formulation for the expected BNS merger rate from a galaxy as

log
(

n
BNS

Gyr

-
1

)
=
0.86
×
log
(

M
*

/

M
⊙

)

+

0.44
×
log
(
sSFR

yr

-
1

)
+
0.857

, which optimally explains the deviation between the stellar mass distributions of the GRB host galaxies and the control sample. These insights provide a strategic framework for targeted GW follow-ups and enhance our ability to identify potential host galaxies for future GW events.
CHARA Near-infrared Imaging of the Yellow Hypergiant Star ρ Cassiopeiae: Convection Cells and Circumstellar Envelope
Authors: Anugu Narsireddy , Baron Fabien , Monnier John D. , Gies Douglas R. , Roettenbacher Rachael M. , Schaefer Gail H. , Montargès Miguel , Kraus Stefan , Le Bouquin Jean-Baptiste , Anderson Matthew D. , ten Brummelaar Theo , Codron Isabelle , Farrington Christopher D. , Gardner Tyler , Gutierrez Mayra , Köhler Rainer , Lanthermann Cyprien , Norris Ryan , Scott Nicholas J. , Setterholm Benjamin R. , Vargas Norman L.
Published: October 2024

Massive evolved stars such as red supergiants and hypergiants are potential progenitors of Type II supernovae, and they are known for ejecting substantial amounts of matter, up to half their initial mass, during their final evolutionary phases. The rate and mechanism of this mass loss play a crucial role in determining their ultimate fate and the likelihood of their progression to supernovae. However, the exact mechanisms driving this mass ejection have long been a subject of research. Recent observations, such as the Great Dimming of Betelgeuse, have suggested that the activity of large convective cells, combined with pulsation, could be a plausible explanation for such mass-loss events. In this context, we conducted interferometric observations of the famous yellow hypergiant, ρ Cassiopeiae using the CHARA Array in H- and K-band wavelengths. ρ Cas is well known for its recurrent eruptions, characterized by periods of visual dimming (∼1.5–2 mag) followed by recovery. From our observations, we derived the diameter of the limb-darkened disk and found that this star has a radius of 1.04 ± 0.01 mas, or 564–700 R
⊙. We performed image reconstructions with three different image reconstruction software packages, and they unveiled the presence of giant hot and cold spots on the stellar surface. We interpret these prominent hot spots as giant convection cells, suggesting a possible connection to mass ejections from the star’s envelope. Furthermore, we detected spectral CO emission lines in the K band (λ = 2.31–2.38 μm), and the image reconstructions in these spectral lines revealed an extended circumstellar envelope with a radius of 1.45 ± 0.10 mas.
Magnetic Field of the Quasar 1604+159 from Parsec to Kiloparsec Scale
Authors: Hu Xu-Zhi , Hong Xiaoyu , Zhao Wei , Chen Liang , Wang Wei-Yang , Wu Linhui
Published: October 2024

We present a multifrequency polarimetric study for the quasar 1604+159. The source was observed at the L band with the American Very Long Baseline Array and the L, X, and U bands with the Very Large Array. These observations provide different resolutions from mas to arcsec, enabling us to probe the morphology and magnetic field from tens of parsec to hundreds of kiloparsec scale. We detect a symmetrical Fanaroff–Riley Class I–like structure. The source has several lobes and bulges, forming a cocoon shape. The polarization is normal to the edges of the structure with high fractional polarization up to ∼60%. Two hotspots are observed at the eastern and western sides of the source, located symmetrically relative to the core. The flux density ratio (>1.5) between the two hotspots suggests the Doppler beaming effect exists at a large scale. The polarized emission in the hotspots also shows a symmetrical structure with an oblique direction from the jet direction. In general, the jet propagates in a collimating structure with several bends. Polarization is also detected perpendicular to the local jet from ∼100 mas to ∼1″. The jet shows strong polarized intensity and high fractional polarization at the bending edges. We discuss the possible origins of the observed structure and magnetic field.
The Time Evolution of Fast Flavor Crossings in Postmerger Disks around a Black Hole Remnant
Authors: Mukhopadhyay Payel , Miller Jonah , McLaughlin Gail C.
Published: October 2024

We postprocess a three-dimensional, general relativistic, full transport neutrino radiation magnetohydrodynamics simulation of the black-hole-accretion disk-wind system thought to be a potential outcome of the GW170817 merger to investigate the presence of electron lepton number (ELN-XLN) crossings in the neutrino angular distribution. Neutrinos are evolved with an explicit Monte Carlo method and can interact with matter via emission, absorption, or scattering. Within the postprocessing framework, we find ubiquitous occurrence of ELN-XLN crossings at early times (∼11 ms), but this does not hold for later times in the simulation. At postmerger times of ∼60 ms and beyond, ELN-XLN crossings are only present near the equator. We provide a detailed analysis of the neutrino radiation field to investigate the origin and time evolution of these crossings. Previous reports have suggested ubiquitous flavor crossings persisting throughout the simulation lifetime, albeit for different sets of conditions for the merger remnant, the treatment of hydrodynamics, and neutrino transport. Even though we do not perform a direct comparison with other published works, we qualitatively assess the reasons for the difference with our results. The geometric structure and evolution of the ELN-XLN crossings found in our analysis, and by extension, fast flavor instabilities, have important implications for heavy element nucleosynthesis in neutron star mergers.
The Active Optics System on the Vera C. Rubin Observatory: Optimal Control of Degeneracy among the Large Number of Degrees of Freedom
Authors: Megias Homar Guillem , Kahn Steven M. , Meyers Joshua M. , Crenshaw John Franklin , Thomas Sandrine J.
Published: October 2024

The Vera C. Rubin Observatory is a unique facility for survey astronomy that will soon be commissioned and begin operations. Crucial to many of its scientific goals is the achievement of sustained high image quality, limited only by the seeing at the site. This will be maintained through an active optics system that controls optical element misalignments and corrects mirror figure error to minimize aberrations caused by both thermal and gravitational effects. However, the large number of adjustment degrees of freedom available on the Rubin Observatory introduces a range of degeneracies, including many that are induced by noise due to imperfect measurement of the wave-front errors. We present a structured methodology for identifying these degeneracies through an analysis of image noise level. We also present a novel scaling strategy based on truncated singular value decomposition that mitigates the degeneracy and optimally distributes the adjustment over the available degrees of freedom. Our approach ensures the attainment of optimal image quality, while avoiding excursions around the noise-induced subspace of degeneracies, marking a significant improvement over the previous techniques adopted for Rubin, which were based on an optimal integral controller. This new approach is likely to also yield significant benefits for all telescopes that incorporate large numbers of degrees of freedom of adjustment.
Radiation Hydrodynamic Simulations of Massive Stars in Gas-rich Environments: Accretion of AGN Stars Suppressed by Thermal Feedback
Authors: Chen 陈 Yi-Xian 逸贤 , Jiang 姜 Yan-Fei 燕飞 , Goodman Jeremy , Lin 林 Douglas N. C. 潮
Published: October 2024

Massive stars may form in or be captured into active galactic nuclei (AGN) disks. Recent 1D studies employing stellar-evolution codes have demonstrated the potential for rapid growth of such stars through accretion up to a few hundred solar masses. We perform 3D radiation hydrodynamic simulations of moderately massive stars’ envelopes in order to determine the rate and critical radius R
crit of their accretion process in an isotropic gas-rich environment in the absence of luminosity-driven mass loss. We find that in the “fast-diffusion” regime where characteristic radiative diffusion speed c/τ is faster than the gas sound speed c

s
, the accretion rate is suppressed by feedback from gravitational and radiative advection energy flux, in addition to the stellar luminosity. Alternatively, in the “slow-diffusion” regime where c/τ < c

s
, due to adiabatic accretion, the stellar envelope expands quickly to become hydrostatic and further net accretion occurs on thermal timescales in the absence of self-gravity. When the radiation entropy of the medium is less than that of the star, however, this hydrostatic envelope can become more massive than the star itself. Within this subregime, the self-gravity of the envelope excites runaway growth. Applying our results to realistic environments, moderately massive stars (≲100M
⊙) embedded in AGN disks typically accrete in the fast-diffusion regime, leading to a reduction of steady-state accretion rate 1–2 orders of magnitudes lower than expected by previous 1D calculations and R
crit smaller than the disk scale height, except in the opacity window at temperature T ∼ 2000 K. Accretion in slow diffusion regime occurs in regions with very high density ρ ≳ 10−9 g cm−3, and needs to be treated with caution in 1D long-term calculations.
On the Origin of High-velocity Clouds in the Galaxy
Authors: Lucchini Scott , Han Jiwon Jesse , Hernquist Lars , Conroy Charlie
Published: October 2024

The origin of our Galaxy’s high-velocity clouds (HVCs) remains a mystery after many decades of effort. In this paper, we use the TNG50 simulation of the IllustrisTNG project to identify cool, dense clouds that match observations of Galactic H i HVCs. We track these clouds back in time to determine their origin. For a TNG50 Milky Way−like galaxy, we find that only 17% of HVCs can be tracked directly to the disk and 21% to material stripped out of satellites. The majority of HVCs (62%) arise from warm and hot circumgalactic gas that cools through thermal instability. They then obtain their anomalous velocities through interactions with the turbulent circumgalactic medium. At TNG50 resolution, we do not see evidence for HVCs forming out of very low metallicity intergalactic material. Instead, low-metallicity HVCs are most likely associated with satellites. These results suggest that Galactic HVCs are highly heterogeneous in their origin and can provide insight into the physical processes that shape the circumgalactic medium, such as disk outflows, satellite accretion, and thermal instabilities.
Comparison of the On-disk Apparent Current Sheets with the Limb Ones
Authors: Ding Tao , Zhang Jun
Published: October 2024

Based on observations from the Solar Dynamics Observatory (SDO) and the Solar and Heliospheric Observatory (SOHO), we investigate 30 apparent current sheets during 1999–2021, including 10 on-disk and 8 limb ones from the SDO, as well as 12 limb ones from the SOHO. Each on-disk current sheet is formed among an X-type configuration consisting of two sets of atmospheric structures, and each limb one is involved in a flare–coronal mass ejection event. During magnetic reconnection period, the on-disk apparent current sheet evolves from a bright point to an elongated line-like structure, and the structure becomes thin in the late stage of the reconnection. Subsequently, the plasma distribution within the current sheet manifests as a plasmoid chain. For the limb apparent current sheet, the length elongation is faster than that of the on-disk one, and the thinning process is also detected. Although the aspect ratios of the limb cases are comparable to the value for the occurrence of tearing mode instability from simulation research, no obvious plasmoid chain is detected within these limb current sheets, and the density distribution is locally uniform. We suggest that due to the rapid extension of limb cases, the tearing mode instability is very fast, resulting in the formation of tiny plasmoids that are smaller than the instrument resolution. Moreover, there is another possible scenario. The observed limb apparent current sheet is just a bright ray, and the actual current sheet is only a small segment of the ray.
KM UMa: An Active Short-period Detached Eclipsing Binary in a Hierarchical Quadruple System
Authors: Meng Fangbin , Zhu Liying , Liu Nianping , Li Ping , Zhang Jia , Li Linjia , Matekov Azizbek
Published: October 2024

The first detailed photometric and spectroscopic analysis of the G-type eclipsing binary KM UMa is presented, which indicates that the system is a short-period detached eclipsing binary. The radial velocity curves were calculated using the cross-correlation function method based on Large Sky Area Multi-Object Fiber Spectroscopic Telescope, Sloan Digital Sky Survey, and our observations, which determined the mass ratio as q = 0.45 (±0.04). Based on the light curves from the Transiting Exoplanet Survey Satellite, other survey data, and our multiband observations, the positive and negative O’Connell effects have been detected evolving gradually and alternately over the last 20 yr, which can be explained by the presence of spots on the primary component. A superflare event was detected in the SuperWASP data on 2007 February 28, further indicating that KM UMa is a very active system. We calculated its energy to be 5 × 1034 erg by assuming it occurred on the primary star. Utilizing hundreds of medium-resolution spectra and one low-resolution spectrum, the equivalent width variations of the H

α
line were calculated, indicating the presence of a 5.21 (±0.67) yr magnetic activity cycle. The orbital period variations were analyzed using the O–C method, detecting a long-term decrease superimposed with a periodic variation. The amplitude of the cyclic variation is 0.01124 (±0.00004) day, with a period of 33.66 (±0.0012) yr, which exceeds the 5.21 yr activity cycle, suggesting that this is more likely attributable to the light travel time effect of a third body. Simultaneously, a visual companion has been detected based on the Gaia astrometric data, indicating that KM UMa is actually in a 2+1+1 hierarchical quadruple system.
Hints of Planet Formation Signatures in a Large-cavity Disk Studied in the AGE-PRO ALMA Large Program
Authors: Sierra Anibal , Pérez Laura M. , Agurto-Gangas Carolina , Miley James , Zhang Ke , Pinilla Paola , Pascucci Ilaria , Trapman Leon , Kurtovic Nicolas , Vioque Miguel , Deng Dingshan , Anania Rossella , Carpenter John , Cieza Lucas A. , González-Ruilova Camilo , Hogerheijde Michiel , Kuznetsova Aleksandra , Rosotti Giovanni P. , Ruiz-Rodriguez Dary A. , Schwarz Kamber , Tabone Benoît , TorresVillanueva Estephani E.
Published: October 2024

Detecting planet signatures in protoplanetary disks is fundamental to understanding how and where planets form. In this work, we report dust and gas observational hints of planet formation in the disk around 2MASS J16120668-301027, as part of the Atacama Large Millimeter/submillimeter Array (ALMA) Large Program “AGE-PRO: ALMA survey of Gas Evolution in Protoplanetary disks.” The disk was imaged with the ALMA at Band 6 (1.3 mm) in dust continuum emission and four molecular lines: 12CO(J = 2–1), 13CO(J = 2–1), C18O(J = 2–1), and H2CO(J = 3(3,0)–2(2,0)). Resolved observations of the dust continuum emission (angular resolution of ∼150 mas, 20 au) show a ring-like structure with a peak at 0.″57 (75 au), a deep gap with a minimum at 0.″24 (31 au), an inner disk, a bridge connecting the inner disk and the outer ring, along with a spiral arm structure, and a tentative detection (to 3σ) of a compact emission at the center of the disk gap, with an estimated dust mass of ∼2.7−12.9 Lunar masses. We also detected a kinematic kink (not coincident with any dust substructure) through several 12CO channel maps (angular resolution ∼200 mas, 30 au), located at a radius of ∼0.″875 (115.6 au). After modeling the 12CO velocity rotation around the protostar, we identified a purple tentative rotating-like structure at the kink location with a geometry similar to that of the disk. We discuss potential explanations for the dust and gas substructures observed in the disk and their potential connection to signatures of planet formation.
A Comparison of the X-Ray Polarimetric Properties of Stellar and Supermassive Black Holes
Authors: Saade M. Lynne , Kaaret Philip , Liodakis Ioannis , Ehlert Steven R.
Published: October 2024

X-ray polarization provides a new way to probe accretion geometry in black hole systems. If the accretion geometry of black holes is similar regardless of mass, we should expect the same to be true of their polarization properties. We compare the polarimetric properties of all nonblazar black holes observed with the Imaging X-ray Polarimetry Explorer. We find that their polarization properties are very similar, particularly in the hard state, where the corona dominates. This tentatively supports the idea that stellar and supermassive black holes share a common coronal geometry.
Partial Disruption of a Planet around a White Dwarf: The Effect of Perturbations from the Remnant Planet on the Accretion
Authors: Kurban Abdusattar , Zhou Xia , Wang Na , Huang Yong-Feng , Wang Yu-Bin , Nurmamat Nurimangul
Published: October 2024

About 25%–50% of white dwarfs (WDs) are found to be polluted by heavy elements. It has been argued that the pollution could be caused by the tidal disruption of an approaching planet around the WD, during which a large number of clumps would be produced and would finally fall onto the WD. The reason that the planet approaches the WD is usually believed to be due to gravitational perturbations from another distant planet or stellar companion. However, the dynamics of the perturbations and the detailed partial disruption process are still poorly understood. In this study, we present an in-depth investigation of these issues. A triple system composed of a WD, an inner orbit planet, and an outer orbit planet is considered. The inner planet would be partially disrupted periodically over its long-term evolution. Fragments generated in the process are affected by gravitational perturbations from the remnant planet, facilitating their fall toward the WD. The mass-loss rate of the inner planet depends on both its internal structure and also on the orbital configuration of the planetary system.
Astrometric Binary Classification via Artificial Neural Networks
Authors: Smith Joe
Published: October 2024

With nearly two billion stars observed and their corresponding astrometric parameters evaluated in the recent Gaia mission, the number of astrometric binary candidates has risen significantly. Due to the surplus of astrometric data, the current computational methods employed to inspect these astrometric binary candidates are both computationally expensive and cannot be executed in a reasonable time frame. In light of this, a machine learning (ML) technique to automatically classify whether a set of stars belongs to an astrometric binary pair via an artificial neural network (ANN) is proposed. Using data from Gaia Data Release 3, the ANN was trained and tested on 1.5 million highly probable true and visual binaries, considering the proper motions, parallaxes, and angular and physical separations as features. The ANN achieves high classification scores, with an accuracy of 99.3%, a precision rate of 0.988, a recall rate of 0.991, and an area under the curve of 0.999, indicating that the utilized ML technique is a highly effective method for classifying astrometric binaries. Thus, the proposed ANN is a promising alternative to the existing methods for the classification of astrometric binaries.
The Use of Participatory Modelling Methods in Agri-Environmental Research – A Systematic Mapping Dataset
Authors: Klemm Toni
Published: October 2024

Participatory modelling (PM) is a transdisciplinary research approach that involves stakeholder in a modelling process to develop or improve qualitative or quantitative models. To better understand the potential uses of PM in the emerging field of agroecology living lab research, I conducted a systematic search of the peer-reviewed literature and describe 78 participatory agri-environmental case studies in this dataset. Bibliographic data are included and each case study is described in terms of main goal(s), PM method(s) used, involved stakeholders and their contributions and the level of stakeholder participation in the project. I also extracted key metadata (if available), such as publication type and year, study location (country), funding source, project duration and outcomes beyond publications. This dataset adds value by revealing clusters and associations of methods and goals, by showing the dominating role of researchers in this type of participatory research, by pointing out the absence of PM in certain areas of agricultural production, such as hydroponic farming or viticulture and by providing a comprehensive foundation for the related research article. It also contained data not used in the related research article that could provide a basis for future research, such as linking methods, goals and stakeholder involvement with other metadata or comparing this agri-environmental research and other areas.
Yersinochloa nianheana (Poaceae, Bambusoideae), a new species from southern Vietnam
Authors: Van Duy Nong , Vinh Tran Thai , Cong Vu Kim , Hoi Quach Van , Tham Dang Thi , Hang Nguyen Thi Thanh , Khiem Dinh Van , Truong Hoang Thanh , Nghia Nguyen Hoang , Minh Nguyen Thi Ai , Tien Tran Van
Published: October 2024

Yersinochloa nianheanasp. nov. from Vietnam is described and illustrated. It is found in southern Vietnam, where it occurs at an elevation of 1400–1500 m in Voi Mountain, Duc Trong District, Lam Dong Province. This new species is distinguished from a similar species, Yersinochloa dalatensis, by culm nodes with a thick swollen patella, culm leaf blades erect, auricles conspicuous, margins bearing long hairs, palea dorsal view showing rachilla extension and rudimentary floret at the apex and lodicules purple gradually towards the top. Besides that, the species is distinguished from Yersinochloa nghiana by the leaf blades without being swollen at the base, the prophyllate bud 2-keeled, lodicules purple at ½ upper parts and unbifid at the base.
Temporal consistency and spatial variability in detection: implications for monitoring of macroinvertebrates from shallow groundwater aquifers
Authors: Knüsel Mara , Alther Roman , Couton Marjorie , Altermatt Florian
Published: October 2024

Implementing and optimizing biodiversity monitoring is crucial given the current, worldwide biodiversity decline. Compared to other ecosystems, monitoring of biodiversity is lagging behind in groundwater ecosystems, both because of sparse taxonomic knowledge and methodological constraints. We here assessed temporal variation in the occurrence and abundance of macroinvertebrates collected systematically from shallow groundwater aquifers of Switzerland to establish general principles on seasonality and repeatability of assessment outcomes. We found no seasonal abundance pattern for obligate groundwater amphipods and isopods, indicating temporal consistency. In contrast, other macroinvertebrates (predominantly stygophiles and stygoxenes) showed pronounced seasonality in their detection rate. However, we found variability in detection rates across groundwater amphipod species and especially across sampling sites. For groundwater communities, characterized by narrowly-distributed and rare species, our results highlight the need for tailored and extensive sampling strategies. When setting up monitoring programs on groundwater fauna, detection probability, temporal autocorrelation, and standardization of sampling effort should be carefully considered. Applying novel, systematic approaches, can offer promising methodologies for understanding and conserving groundwater ecosystems.
Improving production sequencing in the age of Industry 4.0: A mathematical launching model approach
Authors: Azemi Fatmir , Lujic Roberto , Šimunovic Goran , Šimunovic Katica , Ahmeti Faruk
Published: October 2024

Purpose: To enhance enterprise efficiency, this study examines the pivotal role of operations management in optimizing the use of materials, technology, equipment, and personnel, especially within the transformative framework of Industry 4.0.Design/methodology/approach: This article investigates operational preparation in the context of Industry 4.0. Through questionnaires and interviews with stakeholders, problems related to operational preparation were identified. To address these problems, a launching model was developed for production systems. The model considers several parameters important for the production process, including business goals, customer needs, and environmental conditions that impact enterprise performance and profit.Findings: The model determines the importance of jobs to be performed in a certain order to optimize production sequence. The proposed parameters are included in a mathematical-algorithmic launching model based on categorical levels related to the production process, such as profit, delivery times, processing times, total number of technological operations, product types, materials, required quality, product complexity, and resource use. The model was developed based on observations and investigations conducted in Kosovo's enterprises on operations research, and it has the potential to significantly improve production efficiency and profitability in the Industry 4.0 era.Practical implications: The findings of this study have practical implications for operations management within the Industry 4.0 framework, proposing a launching model designed to optimize production processes and enhance efficiency.Originality/value: The originality and value of this research lie in the development of a mathematical-algorithmic launching model that addresses operational preparation in the Industry 4.0 context, taking into account various crucial parameters.
Evaluating Obesity: The “Why” Behind the American Academy of Pediatrics' Obesity Treatment Clinical Practice Guideline
Authors: Rausch John C. , Bolling Christopher F.
Published: October 2024

The 2023 American Academy of Pediatrics' “Clinical Practice Guideline for the Evaluation and Treatment of Children and Adolescents with Obesity (Obesity CPG)” is a comprehensive document that addresses the evaluation and treatment of pediatric obesity. Much attention has been focused on the use of medications and surgery to treat severe obesity, but the document also thoroughly reviews the evaluation of obesity and its comorbidities through key action statements and consensus recommendations. The majority of these evaluation guidelines are well within the scope of the general pediatrician and an understanding of and implementation of them can lead to improved obesity care in the primary care setting. The goal of this article is to guide the reader in the evaluation of obesity and its comorbidities in the primary care setting through a chronic disease model lens as a basis for all future care.

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Pediatr Ann
. 2024;53(10):e378–e385.]
Trauma-Informed Positive Parenting in Primary Care as a Tool to Support Child and Family Well-Being
Authors: Keown M. Kathleen , Vargas-Haskins Wanda , Harford Laura , Maletz Beth , Hoffman Liora , Berger-Jenkins Evelyn
Published: October 2024

Factors affecting caregiver health and wellbeing, such as trauma and stress, can have significant negative impact on parenting behaviors and on subsequent child physical and mental health. Trauma-informed positive parenting (TIPP) is an effective tool that acknowledges and addresses a family's unique journey and needs, while promoting both nurturing caregiver-child interactions and appropriate limit setting. Primary care practices are in unique positions to provide such interventions, due to their long-standing and trusted involvement with families. Therefore, we propose that TIPP can feasibly be incorporated into the pediatric primary care setting to support overall family health and well-being.

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Pediatr Ann
. 2024;53(10):e360–e365.]
Impact of a spherical interface on a concentrical spherical droplet
Authors: Salem Ahmed G. , Alharbi Turki D. , Alharbi Abdulaziz H. , Aldhafeeri Anwar Ali
Published: October 2024

In this paper, an analytical and numerical technique are examined in order to analyse the Stokes flow determination problem due to a viscous sphere droplet moving at a concentric instantaneous position inside a spherical interface separating finite and semi-infinite immiscible fluid phases. Here, when only one of the three phases of the fluid (micropolar fluid) has a microstructure, attention is focused on this case. The motion is considered when Reynolds- and capillary-numbers are low, and the droplet surface and the fluid-fluid interface have insignificant deformation. A general solution is obtained in a spherical coordinate system based on a concentric position to analyse the slow axisymmetric movement of the micropolar fluid, considering microrotation and velocity components. Boundary conditions are initially fulfilled at the fluid-fluid interface and subsequently at the droplet surface. The normalised hydrodynamic drag force applying to a moving viscous droplet appears to be a function of the droplet-to-interface radius ratio, which increases monotonically and becomes unbounded when the droplet surface touches the fluid-fluid interface. The numerical outcomes of the normalised drag force acting on the viscous droplet are derived for different values of the parameters, and are presented in a tabular and graphical framework. A comparison was made between our numerical outcomes for the drag force and the pertinent data for the special cases found in the literature.
The Good, the Bad and the Ugly: How the Three Revolts Against Igor Bensen's Popular Rotorcraft Association During 1962-1976 Failed to Change the Popular Rotorcraft Movement in America
Authors:   Hofstra University, Charnov Bruce
Published: October 2024

During the 1962 - 1982 time period there were three distinct revolts against Igor Bensen's Popular Rotorcraft Association: members of the PRA who saw the PRA as an "association of Bensen dealers"; Ken Brock of California whose attempts to standardize and industrialize the Bensen B8M kit, which were not intended as a challenge, ended up forcing Bensen's withdrawal from formal PRA leadership in early 1973; and the International Gyroplane movement of Martin Hollmann of the mid-1970s which boldly challenged the Bensen heritage even after Bensen's presidency. The irony of each of these revolts is to be found in their genesis and eventual impact: the members' revolt was seemingly ineffective, yet analysis reveals it had a long-lasting impact; the Brock revolt appeared to be the most successful, yet it occasioned little change on the American popular rotorcraft movement; while the International Gyroplane Association, correctly perceiving that the PRA under the leadership of Ken Brock was, in many significant ways, actually a continuation of Bensen's PRA, mounted a vigorous challenge that was seemingly the least effective of the three revolts. But historical analysis reveals that the International Gyroplane revolt of Martin Hollmann, while deemed an utter failure, had the real potential of changing the American Popular Rotorcraft. That Hollmann's revolt did not have a significant impact was largely due to his vitriolic personality and animosity towards Bensen and Brock, and the Popular Rotorcraft movement is poorer for it.
Historical Contributions to Vertical Flight at the NASA Langley Research Center
Authors:   Retired, Hodges Todd ,   NASA Langley Research Ctr., Gorton Susan , Jackson Karen
Published: October 2024

The NASA Langley Research Center has had a long and distinguished history in powered lift technology development. This research has formed the foundation of knowledge for the powered lift community worldwide. From aerodynamics to structures, aeromechanics, powered lift, acoustics, materials, stability & control, structural dynamics and human factors, Langley has made significant contributions to the advancement of vertical lift technologies. This research has encompassed basic phenomenological studies through subscale laboratory testing, analytical tool development, applied demonstrations and full scale flight-testing. Since the dedication of Langley in 1920, it has contributed to the understanding, design, analysis, and flight test development of experimental and production V/STOL configurations. This paper will chronicle significant areas of research through the decades from 1920 to 2015 with historical photographs and references.
Advancing Vertical Flight: A Historical Perspective on AHS International and its Times
Authors:   M.E. Rhett Flater & Associates, Flater M.E. , Smith L.
Published: October 2024

This paper describes AHS's vital role in the development of the rotorcraft industry, with particular emphasis on events since 1990. It includes first-hand accounts of the formation of the Society, how it matured and evolved, and the particular influences that compelled change. It describes key events which occurred during various stages of the Society's growth, including the formation of its technical committees, the evolution of the AHS Annual Forum and technical specialists' meetings, and the creation and evolution of the Society's publications. Featured prominently are accounts of AHS's role in pursuing a combined government, industry and academia approach to rotorcraft science and technology. Also featured is the creation in 1965 of the Army-NASA Agreement for Joint Participation in Aeronautics Technology, the establishment of the U.S. Army Rotorcraft Centers of Excellence, the National Rotorcraft Technology Center (NRTC), the inauguration of the Congressional Rotorcraft Caucus and its support for the U.S. defense industrial base for rotorcraft, the battle for the survival of NASA aeronautics and critical NASA subsonic ground test facilities, and the launching of the International Helicopter Safety Team (IHST).