bluuebunny/crossref_metadata_2025_split huggingface dataset:
Speech Production Errors in Children With Cleft Palate With or Without Cleft Lip
Authors: Lien Kari M. , Scherer Nancy J. , Cordero Kelly Nett , Sitzman Thomas J. 
Published: August 2024

Purpose:
The purpose of this study was to describe the frequency of speech production errors in children with cleft palate with or without cleft lip (CP±L) and explore characteristics related to speech production errors.

Method:
Fifty-six children with nonsyndromic CP±L between the ages of 4;0 and 7;11 (years;months) were included in this study. The children's audio-recorded production of a sentence repetition task was transcribed using narrow transcription and coded for speech error type.

Results:
Children used, on average, 18 speech errors during the sentence repetition task that sampled 59 phoneme targets. On average, phonological errors were used most frequently, with nine errors per sample, followed by anterior oral speech errors at four errors per sample, and non-oral compensatory errors at three errors per sample. Individual-level characteristics including age and cleft type were related to frequency of phonological errors and anterior oral speech errors, respectively. One treatment-level characteristic, hypernasality, was related to use of non-oral compensatory errors and passive speech errors.

Conclusions:
This study identified the most frequent speech production errors as phonological errors, followed by anterior oral speech errors and non-oral compensatory errors. Individual-level and treatment-level characteristics were related to speech production errors. Future research should explore additional characteristics that may influence use of speech production errors. Clinically, this study adds information regarding speech error types that should be monitored throughout cleft care, including phonological errors that were most prevalent among this sample.

Supplemental Material:

https://doi.org/10.23641/asha.22044095
Observer‐based adaptive control of vehicle platoon with uncertainty and input constraints
Authors: Lin Shengping , Liu Lei 
Published: August 2024

AbstractThis study focuses on the highway platoon driving mode and proposes a distributed adaptive control algorithm based on an observer. Firstly, the adaptive observer is designed to compensate for the effect of unknown driving resistance and thus enhance the adaptation ability of the system to uncertainty. Secondly, an auxiliary system is introduced to specifically address actuator saturation constraints, ensuring the stability of the platoon driving in extreme conditions. Lastly, combining an event‐triggered mechanism, a control strategy is designed to achieve the stability of the entire platoon while maximizing the conservation of communication resources. The algorithm's viability and efficiency are confirmed through simulation outcomes.
Impact analysis on distribution network due to coordinated electric ferry charging
Authors: Roy Rajib Baran , Alahakoon Sanath , Rensburg Piet Janse Van , Arachchillage Shantha Jayasinghe 
Published: August 2024

AbstractThe maritime industry is a significant emitter of greenhouse gases in marine ecosystems, prompting a global shift towards renewable‐powered electric vessels, where energy storage is pivotal. The authors examine the potential ramifications of coordinating the charging of Electric Ferries (EFs) on local distribution networks, with Gladstone Marina in Queensland, Australia, serving as a case study. Employing OpenDSS software for power flow analysis, the authors utilise actual load data and simulate a network with four Battery Energy Storage Systems (BESSs) representing proposed charging stations. The authors discuss the impact on bus voltage, load current, and power flow by integrating a storage controller to optimise BESS charging and discharging dynamics. The Dynamic Link Library (DLL) of MATLAB Simulink‐based BESS's dynamic model is linked with OpenDSS environment to replicate the actual electric ferry storage. Additionally, a user‐written DLL in Python regulates BESS charging and discharging by the storage controller according to load demand and BESS State of Charge for ensuring efficient operation within the network. The power flow results without inclusion of BESSs to the network, referred to as the base case, are used for relative comparison with the results in the coordinated mode. The power flow analysis suggests that bus voltages rise by approximately 1%–1.5%, while load current consumption decreases by around 2%–2.5% compared to the base case with variable load. Selected lines and transformers maintain consistent power flows. Notably, a reduction in total power consumption and losses is observed, particularly under an 80% load demand increase. These findings indicate that the coordinated mode with a storage controller effectively manages BESS charging and discharging according to demand. Moreover, the storage controller ensures system parameters remain within permissible limits. The support of real and reactive power by BESSs during peak hours validates their role as peak shavers for the test network, suggesting that EFs can operate in either Grid to Ferry mode during charging and Ferry to Grid mode during discharging.
A family of interleaved isolated three‐level DC/DC converters
Authors: Ai Jian , Yang Xianbin , Shen Yehao , Ni Hanjie , Bi Kaitao , Fan Qigao 
Published: August 2024

AbstractThis paper proposes a family of bipolar step‐up cells (BSUCs). Additionally, a family of interleaved parallel isolated high‐gain DC/DC converters with bipolar outputs based on the BSUCs is proposed. Using one of these converters as an example, it is demonstrated that the converter inherits the advantages of DC three‐level characteristics, resulting in low component voltage stress and low output voltage ripple. Moreover, the converter features a low input current ripple, electrical isolation, bipolar outputs, high voltage gain and operates both switches and diodes in a soft‐switching state. Furthermore, the neutral point of the bipolar outputs in this converter possesses self‐balancing characteristics, effectively mitigating the impact of parasitic parameters on voltage balance. Even with a significant deviation of the duty cycles in the main switches, the influence on the neutral point voltage balance remains very slight. Besides, to address the difficulty of accurately calculating output voltage ripple using traditional methods, a voltage ripple calculation method based on linearizing the charging of the output capacitor is proposed, characterized by its high accuracy and simplicity in the calculation process. Finally, an experimental prototype is established to verify the performance of the proposed converter.
Capacity market in the decarbonization era: Adequacy, flexibility, and environmental revenue
Authors: Li Chaojie , Jiang Youquan , Dai Jiang , Guo Ruyue , Zhang Ying , Tian Shijin , Peng Siran 
Published: August 2024

AbstractWith the increasing penetration rate of renewable energy in the power system, it becomes increasingly important to coordinate adequacy, flexibility, and environmental protection. The development of the power market provides diverse signals for power investors and plays an increasingly significant role in the decarbonization of the power system. However, due to the interdependent operations of various power markets, measuring the multifaceted value of power generation within traditional market mechanisms poses considerable challenges. Herein, a bi‐level optimization model is proposed to integrate the capacity remuneration mechanism (CRM), energy market (EM), and carbon emission trading (CET). The adequacy, flexibility, and environmental revenue expectations of different generation resources through synergistic transactions are derived using Lagrange multipliers. Furthermore, the bilevel optimization model is converted to its equivalent single‐level scheme based on the Karush–Kuhn–Tucker optimality conditions. Finally, several case studies are conducted to demonstrate the effectiveness of the proposed model, along with comparisons and sensitivity analyses to study the principles behind synergistic transactions and the impact of some key parameters.
Spin-orbit alignment in very low mass tight binaries: results for the 2MASS J0746425+200032AB and 2MASS J1314203+132001AB systems using spectroscopic and optically derived rotational estimates
Authors: Dulaimi S. , Boyle R. P. , Fitzgerald K. , Butler R. F. , Golden A. 
Published: August 2024

Context. Constraining the coplanarity status of very low mass (VLM) tight binary systems provides valuable information towards understanding the dominant mechanisms in star and planetary formation at the lower end of the initial mass function.
Aims. We sought to constrain the v sin i degeneracies of two nearby tight VLM binary systems, 2MASS J0746+20AB and 2MASS J1314+13AB, by independently determining each companion’s rotational period and so characterize each system’s spin-orbit alignment.
Methods. Long observational baseline high cadence I band photometry data were obtained for both systems using the Galway Ultra Fast Imager (GUFI) on the Mount Graham International Observatory’s Vatican Advanced Technology Telescope. Previously known rotational periods determined in other passbands were used as a basis for recovering additional periodic modulations in the time-series data.
Results. Using the known rotational period of 3.32 hours for 2MASS J0746425+200032A, we recovered an underlying periodic modulation of 2.14 ± 0.11 hours, which we associate with 2MASS J0746425+200032B. Breaking each components’ v sin i corresponds to equatorial inclination angles of 32 ± 4 degrees and 37 ± 4 degrees for components A & B respectively. We recover a weaker 2.06 ± 0.05 hours modulation separate from the known 3.79 hour signature for J1314203+132001B, which we associate with J1314203+132001A. We place a lower limit on J1314203+132001A’s equatorial inclination angle to be in the range of 24.5−3+3.5 degrees, which deviates from the system’s orbital plane previously determined to be 49.34−0.23+0.28 degrees.
Conclusions. We confirm long term, consistent periodic modulations from both binary systems and report the first definitive rotational period for J1314203+132001A of 2.06 ± 0.05 hours, in addition to coplanarity to within 10 degrees in the spin-orbit alignment of the 2MASS J0746425+200032AB system. The lack of separate v sin i values for the 2MASS J1314203+132001AB system limits a definitive assessment but best estimates suggest coplanarity to be unlikely.
Exploring the links between quasar winds and radio emission along the main sequence at high redshift
Authors: Deconto-Machado A. , del Olmo A. , Marziani P. 
Published: August 2024

Context. Despite the increasing prevalence of radio-loud (RL) sources at cosmic noon, our understanding of the underlying physics that governs the accretion disc outflows in these particular sources and its dissimilarity with radio-quiet (RQ) quasars remains somewhat limited.
Aims. Disentangling the real impact of the radio-loudness and accretion on the outflow parameters remains a challenge to this day. We present ten new spectra of high-redshift and high-luminosity quasars and combine these with previous data at both high and low redshift with the aim being to evaluate the role of the feedback from RL and RQ AGN. The final high-redshift (1.5 ≲ z ≲ 3.9), high-luminosity (47.1 ≤ log(L) ≤ 48.5) sample consists of a combination of 60 quasars from our ISAAC and the Hamburg-ESO surveys. The low-redshift (z ≤ 0.8) sample has 84 quasars that have been analyzed in the optical and with the Faint Object Spectrograph (FOS) data in the UV.
Methods. We perform a multicomponent analysis of optical and UV emission line profiles along the quasar main sequence, and provide a relation that can be used to estimate the main outflow parameters (mass rate, thrust, and kinetic power) in both the BLR and NLR through the analysis of the [O III]λ5007 and C IVλ1549 emission lines.
Results. Spectrophotometric properties and line profile measurements are presented for Hβ+[O III]λλ4959,5007, Si IVλ1397+O IV]λ1402, C IVλ1549+He IIλ1640, and the 1900 Å blend. High-ionization lines, such as C IVλ1549 and [O III]λ5007, usually present a significant asymmetry toward the blue, especially in radio-quiet sources. This is strong evidence of outflow motions. In the ISAAC sample, 72% of the quasars where [O III] is clearly detected present significant outflows, with centroid velocity at half intensity blueshifted to values of greater than ∼250 km s−1. Radio-loud quasars tend to present slightly more modest blueshifted components in both the UV and optical ranges. The behavior of [O III]λ5007 mirrors that of C IVλ1549, with blueshift amplitudes between the two lines showing a high degree of correlation, which appears unaffected by the presence of radio emission.
Conclusions. In contrast to the situation at low redshift, both RL and RQ AGN outflow parameters at high luminosity appear in the range needed to provide feedback effects on their host galaxies. Both high- and low-z RL quasars exhibit smaller outflows compared to RQ quasars, suggesting a potential role of radio-loudness in mitigating outflow effects. Nevertheless, the radio-loudness effect on AGN feedback is much less significant than the effect of accretion, with this latter emerging as the main driver of nuclear outflows.
Protostellar spin-up and fast rotator formation through binary star formation
Authors: Kuruwita Rajika L. , Federrath Christoph , Kounkel Marina 
Published: August 2024

Context. Many fast-rotating stars (rotation periods of < 2 days) are found to be unresolved binaries with separations of tens of AU. This correlation between fast rotators and binarity leads to the question of whether the formation of binary stars inherently produces fast rotators.
Aims. Our goal is to understand the spin evolution of protostars and whether the formation of companions plays a role in spinning up stars.
Methods. We used magneto-hydrodynamic simulations to study the formation of multiple star systems from turbulent and non-turbulent protostellar cores. We tracked the angular momentum accreted by individual star and inner disc systems by using a sink (star) particle technique. We ran a resolution study to extrapolate protostellar properties.
Results. We find in all simulations that the primary star can experience a spin-up event correlated with the formation of companions, namely fragmentation into binaries or higher-order systems. The primary star can spin up by up to 84% of its pre-fragmentation angular momentum and by up to 18% of its pre-fragmentation mass-specific angular momentum. The mechanism for the spin-up is gravitational disc instabilities in the circumstellar disc around the primary star, which leads to the accretion of material with high specific angular momentum. The simulations that experience the strongest disc instabilities fragment to form companions. Simulations with weaker spin-up events experience disc instabilities triggered by a companion flyby, and the disc instability in these cases typically does not produce further fragments (i.e. they remain binary systems).
Conclusions. The primary star in multiple star systems can end up with a higher spin than single stars. This is because gravitational instabilities in the circumstellar disc around the primary star can trigger a spin-up event. In the strongest spin-up events, the instability is likely to cause disc fragmentation and the formation of companions. This spin-up mechanism, coupled with shorter disc lifetimes due to truncated circumstellar discs (and thus short spin-down times), may help produce fast rotators.
The AMBRE Project: Lead abundance in Galactic stars
Authors: Contursi G. , de Laverny P. , Recio-Blanco A. , Molero M. , Spitoni E. , Matteucci F. , Cristallo S. 
Published: August 2024

Context. The chemical evolution of neutron capture elements in the Milky Way is still a matter of debate. Although more and more studies investigate their chemical behaviour, there is still a lack of a significant large sample of abundances of a key heavy element: lead.
Aims. Lead is the final product of the s-process nucleosynthesis channel and is one of the most stable heavy elements. The goal of this article is to present the largest catalogue of homogeneous Pb abundances, in particular for metallicities higher than −1.0 dex, and then to study the lead content of the Milky Way.
Methods. We analysed high-resolution spectra from the ESO UVES and FEROS archives. Atmospheric parameters were taken from the AMBRE parametrisation. We used the automated abundance method GAUGUIN to derive lead abundances in 653 slow-rotating FGK-type stars from the 368.34 nm Pb I line.
Results. We present the largest catalogue of Local Thermodynamic Equilibrium (LTE) and non-LTE lead abundances ever published with metallicities ranging from −2.9 to 0.6 dex and [Pb/Fe] from −0.7 to 3.3 dex. Within this sample, no lead-enhanced Asymptotic Giant Branch (AGB) stars were found, but nine lead-enhanced metal-poor stars ([Pb/Fe] > 1.5) were detected. Most of them were already identified as carbon-enhanced metal-poor stars with enrichments in other s-process species. The lead abundance of 13 Gaia Benchmark Stars are also provided. We then investigated the Pb content of the Milky Way disc by computing vertical and radial gradients and found a slightly decreasing [Pb/Fe] radial trend with metallicity. This trend together with other related ratios ([Pb/Eu], [Pb/Ba], and [Pb/α]) are interpreted thanks to chemical evolution models. The two-infall model closely reproduces the observed trends with respect to the metallicity. It is also found that the AGB contribution to the Pb Galactic enrichment has to be strongly reduced. Moreover, the contribution of massive stars with rather high rotational velocities should be favoured in the low-metallicity regime.
X-ray photo-desorption of NH3 and N2 from ammonia ices: Mechanisms and yields in protoplanetary disks
Authors: Torres-Díaz D. , Basalgète R. , Amiaud L. , Philippe L. , Michaut X. , Fillion J.-H. , Lafosse A. , Bertin M. 
Published: August 2024

Context. Ammonia is detected both in the gas phase and in the ices of protoplanetary disks. However, its gas phase abundances are still difficult to reproduce via chemical modelling when only the thermal-, UV photon-, and cosmic ray-induced processes are considered. Among other non-thermal mechanisms, X-ray photo-desorption is a relevant pathway to maintaining a budget of molecules in the gas of disks. However, no quantitative data are available to constrain its efficiency in the case of ammonia-containing ices.
Aims. We studied the desorption induced by soft X-rays from ammonia ices to determine the photo-desorption yields of neutral molecules that can be applied to the conditions of protoplanetary disks. We also aim to identify the desorption mechanisms at play.
Methods. Pure ammonia ices were deposited at 23 or 75 K and irradiated between 395 and 435 eV, with monochromatic synchrotron light. Desorption of neutral molecules and fragments was detected using a quadrupole mass spectrometer, calibrated to obtain des-orption yields. These values were extrapolated and the spectrum of a protoplanetary disk was used to extract average astrophysical desorption yields.
Results. Photo-desorption from NH3 ices is dominated by the desorption of neutral NH3 and N2 molecules. The desorption mechanism mostly involves the thermalisation of Auger electrons in the ice, although resonant phenomena also contribute near the N 1s ionisation edge. The NH3 photo-desorption is independent of ice morphology and irradiation temperature. Contrary to NH3 desorption, N2 desorption is sensitive to the photon fluence received by the ice. Average photo-desorption yields derived using the TW Hya X-ray spectrum reveal that the NH3 photo-desorption would be four to six times more efficient than that of H2O. This could be at the origin of unexplained high NH3/H2O abundance ratios predicted in the disk around TW Hya. This result ought to be confirmed by the study of mixed water-ammonia ices.
Soft X-ray emission from the classical nova AT 2018bej
Authors: Tavleev A. , Ducci L. , Suleimanov V. F. , Maitra C. , Werner K. , Santangelo A. , Doroshenko V. 
Published: August 2024

Context. Classical novae are known to demonstrate a supersoft X-ray source (SSS) state following outbursts. This state is associated with residual thermonuclear burning on the white dwarf (WD) surface. During its all-sky survey (eRASS1), the eROSITA telescope on board the Spectrum-Roentgen-Gamma observatory discovered a bright new SSS, whose position is consistent with the known classical nova AT 2018bej in the Large Magellanic Cloud. There were two eROSITA spectra obtained during the eRASS1 and eRASS2 monitoring epochs and one XMM-Newton grating spectrum close to the eRASS1 epoch.
Aims. We aim to describe the eROSITA and follow-up XMM-Newton spectra of AT 2018bej with our local thermodynamic equilibrium (LTE) atmosphere models. We focussed on the evolution of the hot WD properties between the eRASS1 and eRASS2 epochs, especially with respect to the change in carbon abundance.
Methods. A grid of LTE model atmosphere spectra was calculated for different values of the effective temperature (from Teff = 525 to 700 kK in steps of 25 kK), surface gravity (six values), and chemical composition, assuming approximately equal hydrogen and helium number fractions, and five different values of carbon and nitrogen abundances.
Results. Both eRASS1 and XMM 0.3–0.6 keV spectral analyses yield a temperature of the WD of Teff~ 600 kK and a WD radius of 8000–8700 km. A simultaneous fitting of the eROSITA spectra for two epochs (eRASS1 and eRASS2) with a common WD mass parameter demonstrates a decrease in Teff, accompanied by an increase in the WD radius and a decrease in the carbon abundance. However, these changes are marginal and remain within the errors. The derived WD mass is estimated to be 1.05–1.15 M⊙.
Conclusions. We traced a minor evolution of the source on a half-year timescale accompanied by a decrease in the carbon abundance and concluded that LTE model atmospheres can be used to analyse the available X-ray spectra of classical novae during their SSS state.