bluuebunny/crossref_metadata_2025_split huggingface dataset:
A replication and extension of adverse and benevolent childhood experiences along with contemporaneous social support and sociodemographic stress for perinatal mental health problems
Authors: Merrick Jillian S. , Narayan Angela J. 
Published: August 2024

Abstract
This study replicated and extended Narayan and colleagues’ (2018) original benevolent childhood experiences (BCEs) study. We examined associations between adverse and positive childhood experiences and mental health problems in a second sample of low-income, ethnically diverse pregnant individuals (replication). We also examined effects of childhood experiences on perinatal mental health problems while accounting for contemporaneous support and stress (extension). Participants were 175 pregnant individuals (M = 28.07 years, SD = 5.68, range = 18–40; 38.9% White, 25.7% Latina, 16.6% Black, 12.0% biracial/multiracial, 6.8% other) who completed standardized instruments on BCEs, childhood maltreatment and exposure to family dysfunction, sociodemographic stress, and perinatal depression and post-traumatic stress disorder (PTSD) symptoms. They completed the Five-Minute Speech Sample at pregnancy and postpartum to assess social support from the other biological parent. Higher family dysfunction predicted higher prenatal depression symptoms, while higher BCEs and prenatal social support predicted lower prenatal PTSD symptoms. Prenatal depression and prenatal PTSD symptoms were the most robust predictors of postnatal depression and PTSD symptoms, respectively, although higher postnatal social support also predicted lower postnatal PTSD symptoms. Findings replicated many patterns found in the original BCEs study and indicated that contemporaneous experiences are also associated with perinatal mental health problems.
Preliminary investigation on the impact of salty and sugary former foods on pig liver and plasma profiles using OMICS approaches
Authors: Manoni Michele , Altomare Alessandra , Nonnis Simona , Ferrario Giulio , Mazzoleni Sharon , Tretola Marco , Bee Giuseppe , Tedeschi Gabriella , Aldini Giancarlo , Pinotti Luciano 
Published: August 2024

AbstractReplacing cereals with food leftovers could reduce feed-food competition and keep nutrients and energy in the food chain. Former food products (FFPs) are industrial food leftovers no more intended for human but still suitable as alternative and sustainable feedstuffs for monogastric. In this study, omics approaches were applied to evaluate the impact of dietary FFPs on pig liver proteome and plasma peptidome. Thirty-six Swiss Large White male castrated pigs were randomly assigned to three dietary treatments [control (CTR), 30% CTR replaced with salty FFP (SA), 30% CTR replaced with sugary FFP (SU)] from the start of the growing phase (22.4 ± 1.7 kg) until slaughtering (110 ± 3 kg). The low number of differentially regulated proteins in each comparison matrix (SA/SU vs. CTR) and the lack of metabolic interaction indicated a marginal impact on hepatic lipid metabolism. The plasma peptidomics investigation showed low variability between the peptidome of the three dietary groups and identified three possible bioactive peptides in the SA group associated with anti-hypertension and vascular homeostasis regulation. To conclude, the limited modulation of liver proteome and plasma peptidome by the SA and SU diets strenghtened the idea of reusing FFPs as feed ingredients to make pig production more sustainable.
Emerging targets for positron emission tomography imaging in proteinopathies
Authors: Chassé Melissa , Vasdev Neil 
Published: August 2024

AbstractPositron emission tomography (PET) imaging of neurodegenerative disease has historically focused on a small number of established targets. The development of selective PET radiotracers for novel biological targets enables new ways to interrogate the neuropathology of proteinopathies and will advance our understanding of neurodegeneration. This perspective aims to highlight recent PET radiotracers developed for five emerging targets in proteinopathies (i.e., mHTT, BACE1, TDP-43, OGA, and CH24H).
Genetic association of serum calcium, phosphate, vitamin D, parathyroid hormone, and FGF23 with the risk of aortic stenosis
Authors: Zhao Qinghao , Nie Wenchang , Dong Jiaming , Zhang Bowen , Tang Gongzheng , Hong Shenda , Liu Jian 
Published: August 2024

AbstractDisorders of mineral metabolism, including elevated levels of serum calcium, phosphate, 25-hydroxyvitamin D (25OH-VitD), parathyroid hormone (PTH), and fibroblast growth factor 23 (FGF23), have been reported in patients with calcific aortic valve stenosis (CAVS). However, evidence of the causal role of mineral metabolism in CAVS is still lacking. In this study, we employed a systematic pipeline combining Mendelian randomization (MR), Steiger directionality test, colocalization analysis, protein-protein network, and enrichment analysis to investigate the causal effect of mineral metabolism on CAVS. Genome-wide association study (GWAS) and protein quantitative trait loci data for mineral metabolism markers were extracted from large-scale meta-analyses. Summary statistics for CAVS were obtained from two independent GWAS datasets as discovery and replication cohorts (n = 374,277 and 653,867). In MR analysis, genetic mimicry of serum FGF23 elevation was associated with increased CAVS risk [ORdiscovery = 3.081 (1.649–5.760), Pdiscovery = 4.21 × 10−4; ORreplication = 2.280 (1.461 – 3.558), Preplication = 2.82 × 10−4] without evidence of reverse causation (Psteiger= 7.21 × 10−98). Strong colocalisation association with CAVS was observed for FGF23 expression in the blood (PP.H4 = 0.96). Additionally, we identified some protein-protein interactions between FGF23 and known CAVS-associated genes. Serum calcium, phosphate, 25OH-VitD, and PTH failed to show causal effects on CAVS at Bonferroni-corrected significance (all P > 0.05/5 = 0.01). In conclusion, elevated serum FGF23 level may act as a causal risk factor for CAVS, and its mechanism of action in CAVS development may be independent of its function in regulating mineral metabolism. Hence, FGF23 may serve as a circulating marker and a promising preventive target for CAVS, warranting further investigation.
An adaptive block‐wise prediction error‐based (AdaBPE) reversible data hiding in encrypted images for medical image transmission
Authors: Panchikkil Shaiju , Manikandan Vazhora Malayil , Pratim Roy Partha , Wang Shuihua , Zhang Yudong 
Published: August 2024

AbstractLife expectancy has improved with new‐age technologies and advancements in the healthcare sector. Though artificial intelligence (AI) and the Internet of Things (IoT) are revolutionising smart healthcare systems, security of the healthcare data is always a concern. Reversible data hiding (RDH) is widely explored in the healthcare domain for secure data transmission and in areas like cloud computing, satellite image transmission, etc. Medical image transmission plays an important role in the smart health sector. In the case of medical images, a minute error in the reconstructed medical image can mislead the doctor, posing a threat to the patient’s health. Many RDH schemes have been proposed, but very few address from the view of medical images, and that too on high‐quality DICOM images. The proposed AdaBPE RDH scheme is a solution for secure transmission of the patient’s health report (PHR) and other sensitive information with medical specialists. The scheme put forward a technique that maintains a good trade‐off between the smooth pixels for maximum embedding in a block and a lossless recovery. Here, the cover medium employed to hide the patient’s sensitive information is an encrypted 16‐bit DICOM image. The scheme processes the cover image as disjoint blocks of equal size, embedding the information adaptively within the encrypted blocks pertaining to the nature of the actual pixel values in the block through MSB prediction error methodology. The outcomes are evaluated on both the 16‐bit DICOM images and 8‐bit natural images, and the scheme is well poised with RDH goal of BER = 0, PSNR = ∞, and SSIM = 1, achieving an average embedding of 5.7067 bpp on high‐quality medical images and 1.6769 bpp on natural images. The experimental results prove advantageous and are better than other similar state‐of‐the‐art schemes.
Wind power generation forecasting based on multi‐model fusion via blending ensemble learning architecture
Authors: Wang Jian , Hou Yanpeng , Ma Zhiqi , Qi Jianming 
Published: August 2024

AbstractBecause of the intermittency and randomness of wind power generation, constructing an accurate wind power generation forecasting model is of great necessity for stable operation and optimal scheduling of modern power systems. Considering the unsatisfied performance of the single learner model and the diverse learning abilities of different machine learning algorithms, XGBoost model, KNN algorithm, SVM algorithm, and CNN‐BiLSTM‐Attention neural network are integrated via blending ensemble architecture to construct the multi‐model fusion short‐term wind power forecasting model. Pearson correlation analysis is applied to reveal the interrelation between meteorological factors and wind power. Additionally, the training samples of base learners are reconstructed for ensuring all data can be utilized. The advantages of each learner are combined co‐ordinately via blending ensemble learning framework. Prediction results of ensemble learning model and single learner model are compared in the same scenario. Simulation results indicate that the ensemble learning model can effectively extract potential features of input information and realize higher prediction accuracy.
Disturbance observer‐based finite‐time control of a photovoltaic‐battery hybrid power system
Authors: Esmaeili Fatemeh , Koofigar Hamid Reza 
Published: August 2024

AbstractHerein, the load power control of the stand‐alone photovoltaic‐battery hybrid power system (HPS) has been investigated. The underlying HPS consists of a boost DC‐DC converter, a non‐isolated bidirectional half‐bridge converter, a photovoltaic (PV) panel, and a battery pack. On the PV side, a disturbance observer‐based finite‐time terminal sliding mode control (FTSMC) is used to regulate the DC bus to the desired voltage, in the presence of irradiation variation and load changes. On the battery side, the load power control system is constructed, based on a model predictive control (MPC) algorithm, with constraints on state‐of‐charge (SOC) and maximum current value of the battery to improve the battery life cycle and high reliability of the system. To highlight the benefits of the closed‐loop system, the analytical proofs and numerical analysis are presented from a comparative viewpoint. The experimentally derived results, by implementation on TMS320F28335 digital signal processing (DSP), are also presented and discussed for practical justification.
Connecting stellar and galactic scales: Energetic feedback from stellar wind bubbles to supernova remnants
Authors: Fichtner Yvonne A. , Mackey Jonathan , Grassitelli Luca , Romano-Díaz Emilio , Porciani Cristiano 
Published: August 2024

Context. Energy and momentum feedback from stars is a key element in models of galaxy formation and interstellar medium (ISM) dynamics, but resolving the relevant length scales in order to directly include this feedback remains beyond the reach of current-generation simulations.
Aims. We aim to constrain the energy feedback of winds, photoionisation, and supernovae (SNe) from massive stars.
Methods. We measure the thermal and kinetic energy imparted to the ISM on various length scales, which we calculate from high-resolution 1D radiation-hydrodynamics simulations. Our grid of simulations covers a broad range of densities, metallicities, and state-of-the-art evolutionary models of single and binary stars.
Results. A single star or binary system can carve a cavity of tens of parsecs (pc) in size into the surrounding medium. During the pre-SN phase, post-main sequence stellar winds and photoionisation dominate. While SN explosions dominate the total energy budget, the pre-SN feedback is of great importance by reducing the circumstellar gas density and delaying the onset of radiative losses in the SN remnant. Contrary to expectations, the metallicity dependence of the stellar wind has little effect on the cumulative energy imparted by feedback to the ISM; the only requirement is the existence of a sufficient level of pre-SN radiative and mechanical feedback. The ambient medium density determines how much and when feedback energy reaches distances of ≳10–20 pc and affects the division between kinetic and thermal feedback.
Conclusions. Our results can be used as a subgrid model for feedback in large-scale simulations of galaxies. The results reinforce that the uncertain mapping of stellar evolution sequences to SN explosion energy is very important for determining the overall feedback energy from a stellar population.
Numerical challenges for energy conservation inN-body simulations of collapsing self-interacting dark matter halos
Authors: Fischer Moritz S. , Dolag Klaus , Yu Hai-Bo 
Published: August 2024

Context.Dark matter (DM) halos can be subject to gravothermal collapse if the DM is not collisionless, but engaged in strong self-interactions instead. When the scattering is able to efficiently transfer heat from the centre to the outskirts, the central region of the halo collapses and reaches densities much higher than those for collisionless DM. This phenomenon is potentially observable in studies of strong lensing. Current theoretical efforts are motivated by observations of surprisingly dense substructures. However, a comparison with observations requires accurate predictions. One method to obtain such predictions is to useN-body simulations. Collapsed halos are extreme systems that pose severe challenges when applying state-of-the-art codes to model self-interacting dark matter (SIDM).Aims.In this work, we investigate the root of such problems, with a focus on energy non-conservation. Moreover, we discuss possible strategies to avoid them.Methods.We ranN-body simulations, both with and without SIDM, of an isolated DM-only halo and we adjusted the numerical parameters to check the accuracy of the simulation.Results.We find that not only the numerical scheme for SIDM can lead to energy non-conservation, but also the modelling of gravitational interaction and the time integration are problematic. The main issues we find are: (a) particles changing their time step in a non-time-reversible manner; (b) the asymmetry in the tree-based gravitational force evaluation; and (c) SIDM velocity kicks breaking the time symmetry.Conclusions.Tuning the parameters of the simulation to achieve a high level of accuracy allows us to conserve energy not only at early stages of the evolution, but also later on. However, the cost of the simulations becomes prohibitively large as a result. Some of the problems that make the simulations of the gravothermal collapse phase inaccurate can be overcome by choosing appropriate numerical schemes. However, other issues still pose a challenge. Our findings motivate further works on addressing the challenges in simulating strong DM self-interactions.
Accretion flares from stellar collisions in galactic nuclei
Authors: Hu B. X. , Loeb A. 
Published: August 2024

Context. The strong tidal force in a supermassive black hole’s (SMBH) vicinity, coupled with a higher stellar density at the center of a galaxy, make it an ideal location to study the interaction between stars and black holes. Two stars moving near the SMBH could collide at a very high speed, which can result in a high energy flare. The resulting debris can then accrete onto the SMBH, which could be observed as a separate event.
Aims. We simulate the light curves resulting from the fallback accretion in the aftermath of a stellar collision near a SMBH. We investigate how it varies with physical parameters of the system.
Methods. Light curves are calculated by simulating post-collision ejecta as N particles moving along individual orbits which are determined by each particle’s angular momentum, and assuming that all particles start from the distance from the black hole at which the two stars collided. We calculate how long it takes for each particle to reach its distance of closest approach to the SMBH, and from there we add to it the viscous accretion timescale as described by the alpha-disk model for accretion disks. Given a timestamp for each particle to accrete, this can be translated into into a luminosity for a given radiative efficiency.
Results. With all other physical parameters of the system held constant, the direction of the relative velocity vector at time of impact plays a large role in determining the overall form of the light curve. One distinctive light curve we notice is characterized by a sustained increase in the luminosity some time after accretion has started. We compare this form to the light curves of some candidate tidal disruption events (TDEs).
Conclusions. Stellar collision accretion flares can take on unique appearances that would allow them to be easily distinguished, as well as elucidate underlying physical parameters of the system. There exist several ways to distinguish these events from TDEs, including the much wider range of SMBH masses stellar collisions may exist around. The beginning of the Vera Rubin Observatory Legacy Survey of Space and Time will greatly improve survey abilities and facilitate in the identification of more stellar collision events, particularly in higher-mass SMBH systems.
Disentangling the dust and gas contributions of the JWST/MIRI spectrum of Sz 28
Authors: Kaeufer T. , Woitke P. , Kamp I. , Kanwar J. , Min M. 
Published: August 2024

Context. Recent spectra of protoplanetary disks around very low-mass stars (VLMS), captured by the Mid-InfraRed Instrument (MIRI) on board the James Webb Space Telescope (JWST), reveal a rich carbon chemistry. Current interpretations of these spectra are based on 0D slab models and provide valuable estimates for molecular emission temperatures and column densities in the innermost disk (radius ≲ 1 au). However, the established fitting procedures and simplified models are challenged by the many overlapping gas features.
Aims. We aim to simultaneously determine the molecular and the dust composition of the disk around the VLMS Sz 28 in a Bayesian way.
Methods. We modelled the JWST/MIRI spectrum of Sz 28 up to 17 μm using the Dust Continuum Kit with Line emission from Gas (DuCKLinG). Systematically excluding different molecules from the Bayesian analysis allowed for an evidence determination of all investigated molecules and isotopologues. We continued by examining the emission conditions and locations of all molecules, analysing the differences to previous 0D slab fitting, and analysing the dust composition.
Results. We find very strong Bayesian evidence for the presence of C2H2, HCN, C6H6, CO2, HC3N, C2H6, C3H4, C4H2, and CH4 in the JWST/MIRI spectrum of Sz 28. Additionally, we identify CH3 and find tentative indications for NH3. There is no evidence for water in the spectrum. However, we show that column densities of up to 2 × 1017 cm−2 could be hidden in the observational noise if assuming similar emission conditions of water as the detected hydrocarbons. Contrary to previous 0D slab results, a C4H2 quasi-continuum is robustly identified. We confirm previous conclusions that the dust in Sz 28 is highly evolved, with large grains (5 μm) and a high crystallinity fraction being retrieved. We expect some of the stated differences to previous 0D slab fitting results to arise from an updated data reduction of the spectrum, but also due to the different modelling process. The latter reason underpins the need for more advanced models and fitting procedures.
Gas dynamics around a Jupiter-mass planet
Authors: Lega E. , Benisty M. , Cridland A. , Morbidelli A. , Schulik M. , Lambrechts M. 
Published: August 2024

Context. Giant planets grow and acquire their gas envelope during the disk phase. At the time of the discovery of giant planets in their host disk, it is important to understand the interplay between the host disk and the envelope and circum-planetary disk properties of the planet.
Aims. Our aim is to investigate the dynamical and physical structure of the gas in the vicinity of a Jupiter-mass planet and study how protoplanetary disk properties, such as disk mass and viscosity, determine the planetary system as well as the accretion rate inside the planet’s Hill sphere.
Methods. We ran global 3D simulations with the grid-based code fargOCA, using a fully radiative equation of state and a dust-to-gas ratio of 0.01. We built a consistent disk structure starting from vertical thermal equilibrium obtained by including stellar irradiation. We then let a gap open with a sequence of phases, whereby we deepened the potential and increased the resolution in the planet’s neighbourhood. We explored three models. The nominal one features a disk with surface density, ∑, corresponding to the minimum mass solar nebula at the planet’s location (5.2 au), characterised by an α viscosity value of 4 10−3 at the planet’s location. The second model has a surface density that is ten times smaller than the nominal one and the same viscosity. In the third model, we also reduced the viscosity value by a factor of 10.
Results. During gap formation, giant planets accrete gas inside the Hill sphere from the local reservoir. Gas is heated by compression and cools according to opacity, density, and temperature values. This process determine the thermal energy budget inside the Hill sphere. In the analysis of our disks, we find that the gas flowing into the Hill sphere is approximately scaled as the product ∑ν, as expected from viscous transport. The accretion rate of the planetary system (envelope plus circum-planetary disk) is instead scaled as √Σv, with its efficiency depending on the thermal energy budget inside the Hill sphere.
Conclusions. Previous studies have shown that pressure-supported or rotationally supported structures are formed around giant planets, depending on the equation of state (EoS) or on the opacity; namely, on the dust content within the Hill sphere. In the case of a fully radiative EoS and a constant dust to gas ratio of 0.01, we find that low-mass and low-viscosity circum-stellar disks favour the formation of a rotationally supported circum-planetary disk. Gas accretion leading to the doubling time of the planetary system of > 105 years has only been found in the case of a low-viscosity disk.