bluuebunny/crossref_metadata_2025_split huggingface dataset:
Assessment of Sacculocollic and Vestibulomasseteric Reflex Pathways in Individuals With Migraine and Vestibular Migraine
Authors: Sreedharan Sanitha Adithya , Sinha Sujeet Kumar 
Published: October 2024

Purpose:
The study's objective was to evaluate the functioning of sacculocollic and vestibulomasseteric reflex pathways in individuals with vestibular migraine and migraine.

Method:
Seventy-five participants aged 18–50 years were selected for the study. Participants were divided into three groups. Group 1 consisted of 25 healthy individuals, Group 2 consisted of 25 migraine individuals, and Group 3 consisted of 25 individuals with vestibular migraine. Cervical vestibular-evoked myogenic potential (cVEMP) and masseter vestibular-evoked myogenic potential (mVEMP) were recorded using a 500-Hz tone burst stimulus presented at 125 dB peSPL for all participants.

Results:

The cVEMP test results showed a delayed p13 and n23 latency for both migraine and vestibular migraine individuals when compared to healthy individuals. Also, the amplitude of the p13-n23 peak was reduced compared to healthy individuals in both migraine and vestibular migraine. Similarly, the mVEMP test results showed a delayed p11 and n21 latency for both migraine and vestibular migraine individuals. No difference was observed in the amplitude of the p11-n21 peak complex between the three groups. Spearman's rho correlation revealed no significant (
p
> .05) correlation between cervical and masseter VEMP latency and amplitude parameters between healthy, migraine, and vestibular migraine individuals.

Conclusions:
The results of the study are suggestive of the pathology of the sacullocollic and vestibulomasseteric reflex pathways in individuals with migraine and vestibular migraine. Individuals with migraine and vestibular migraine should undergo a detailed vestibular evaluation.
Fractional order slide mode droop control for simultaneous voltage and frequency regulation of AC microgrid
Authors: Ibraheem Mohamad Issa , Edrisi Mehdi , Alhelou Hassan Haes , Gholipour Mehdi 
Published: October 2024

AbstractThis research proposes the application of fractional‐order sliding mode control (FOSMC) at the primary controller level to improve the stability of an islanded microgrid by adjusting its voltage and frequency. The control strategies used in the microgrid are performed in two levels (primary and secondary) in the islanded mode. Practically, most previous studies have worked to improve the primary controller. Droop control is one of the most commonly used methods at the primary level and is adopted in this study as well. The sliding mode control (SMC) strategy is normally used to control linear equations. Thus, the non‐linear microgrid equations were transformed into some linear ones using the input‐output feedback linearization technique. Further, a fractional sliding surface was acquainted. The sliding surface and FOSMC were designed to reject system uncertainties and organize the voltage and frequency. Design parameters were chosen using the Lyapunov stability theorem. The validation of the proposed method using Simulink‐MATLAB confirms its effectiveness in enhancing level power sharing, regulating frequency, and maintaining voltage stability across the system.
LBM-DEM modeling of particle-fluid interactions on active small solar bodies
Authors: Wang Qiujun , Cheng Bin , Baoyin Hexi , Piao Ying 
Published: October 2024

Context. Aeolian-like surface features observed on small Solar System bodies have piqued interest in their underlying formation mechanisms. Understanding the evolution of fluid-solid interactions is crucial for elucidating the nature of cometary activity.
Aims. We established a resolved fluid-particle simulation approach and implemented it into our self-developed DEMBody and LBM-Coupler codes to simulate the wind erosion process on comet 67P.
Methods. We developed this novel framework by applying the lattice Boltzmann method-discrete element method (LBM-DEM) in a low-gravity and rarefied atmosphere environment. The inter-particle forces were modeled using the Hertz contact model, friction, and cohesion. The fluid field was calculated by solving the lattice Boltzmann equations, which use the distribution function as the variable. The fluid-particle forces were modeled using the partially saturated cells method, in which the force is calculated based on the populations of the fluid cells occupied by the solid phase. We conducted 2D and 3D validation simulations and a series of simulations of a regolith layer as a preliminary application to validate the framework.
Results. The validation results of the drag coefficient under 2D and 3D conditions are in good agreement with previous theoretical and numerical estimates. Additionally, the wind erosion process on the surface of comet 67P is reproduced using the presented approach. This preliminary application show that the threshold velocity to initiate grain motion on comet 67P is about 25 m/s, which is consistent with the observations that sediment transport driven by winds frequently occurs near the perihelion of comet 67P.
Conclusions. The proposed LBM-DEM framework can be successively applied to simulate the fluid-solid interaction on small solar bodies that have extremely low-gravity and rarefied atmosphere environments. Future works based on this tool and focused on aeolian geologic landforms, such as sand dunes, can help us understand the dynamics of cometary activity.
X-ray reverberation modelling of the continuum, optical/UV time-lags in quasars
Authors: Langis D. A. , Papadakis I. E. , Kammoun E. , Panagiotou C. , Dovčiak M. 
Published: October 2024

Context. Extensive, multi-wavelength monitoring campaigns of nearby and higher redshift active galactic nuclei (AGN) have shown that the UV/optical variations are well correlated with time delays which increase with increasing wavelength. Such behaviour is expected in the context of the X-ray thermal reverberation of the accretion disc in AGN.
Aims. Our main objective is to use time-lag measurements of luminous AGN and fit them with sophisticated X-ray reverberation time-lags models. In this way we can investigate whether X-ray reverberation can indeed explain the observed continuum time lags, and whether time-lag measurements can be used to measure physical parameters such as the X-ray corona height and the spin of the black hole (BH) in these systems.
Methods. We use archival time-lag measurements for quasars from different surveys, and we compute their rest frame, mean time-lags spectrum. We fit the data with analytical X-ray reverberation models, using χ2 statistics, and fitting for both maximal and non spinning BHs, for various colour correction values and X-ray corona heights.
Results. We found that X-ray reverberation can explain very well the observed time lags, assuming the measured BH mass, accretion rate and X-ray luminosity of the quasars in the sample. The model agrees well with the data both for non-rotating and maximally rotating BHs, as long as the corona height is larger than ∼40 gravitational radii. This is in agreement with previous results which showed that X-ray reverberation can also explain the disc radius in micro-lensed quasars, for the same corona heights. The corona height we measure depends on the model assumption of a perfectly flat disc. More realistic disc models may result in lower heights for the X-ray corona.
Proton ingestion in asymptotic giant branch stars as a possible explanation for J-type stars and AB2 grains
Authors: Choplin A. , Siess L. , Goriely S. 
Published: October 2024

Context. J-type stars are a subclass of carbon stars that are generally Li-rich, not enriched in s-elements, and have low 12C/13C ratios. They were suggested to be the manufacturers of the pre-solar grains of type AB2 (having low 12C/13C and supersolar 14N/15N).
Aims. In this Letter, we investigate the possibility that J-type stars are early asymptotic giant branch (AGB) stars that experienced a proton ingestion event (PIE).
Methods. We used the stellar evolution code STAREVOL to compute AGB stellar models with initial masses of 1, 2, and 3M⊙ and metallicities [Fe/H] = − 0.5 and 0.0. We included overshooting above the thermal pulse and used a network of 1160 nuclei coupled to the transport equations. The outputs of these models were compared to observations of J-type stars and AB2 grains.
Results. In solar-metallicity AGB stars, PIEs can be triggered if a sufficiently high overshoot is considered. These events lead to low 12C/13C ratios, high Li abundances, and no enrichment in s-elements. We find that the 2 − 3 M⊙ AGB models experiencing a PIE can account for most of the observational features of J-type stars and AB2 grains. The remaining tensions between models and observations are (1) the low 14N/15N ratio of some AB2 grains and of 2 out of 13 J-type stars, (2) the high 26Al/27Al of some AB2 grains, and (3) the J-type stars with A(Li) < 2. Extra mixing mechanisms can alleviate some of these tensions, such as thermohaline or rotation.
Conclusions. This work highlights a possible match between AGB stellar models that undergo a PIE and J-type stars and AB2 grains. To account for other types of carbon stars, such as N-type stars, PIEs should only develop in a fraction of solar-metallicity AGB stars. Additional work is needed to assess how the occurrence of PIEs depends on mixing parameters and initial conditions, and therefore to further confirm or exclude the proposed scenario.
Failed supernova explosions increase the duration of star formation in globular clusters
Authors: Wirth Henriette , Haas Jaroslav , Šubr Ladislav , Jerabkova Tereza , Yan Zhiqiang , Kroupa Pavel 
Published: October 2024

Context. The duration of star formation (SF) in globular clusters (GCs) is an essential aspect for understanding their formation. Contrary to previous presumptions that all stars above 8 M⊙ explode as core-collapse supernovae (CCSNe), recent evidence suggests a more complex scenario.
Aims. We analyse iron spread observations from 55 GCs to estimate the number of CCSNe explosions before SF termination, thereby determining the SF duration. This work for the first time takes the possibility of failed CCSNe into account, when estimating the SF duration.
Methods. Two scenarios are considered: one where all stars explode as CCSNe and another where only stars below 20 M⊙ lead to CCSNe, as most CCSN models predict that no failed CCSNe happen below 20 M⊙ .
Results. This establishes a lower (≈3.5 Myr) and an upper (≈10.5 Myr) limit for the duration of SF. Extending the findings of our previous paper, this study indicates a significant difference in SF duration based on CCSN outcomes, with failed CCSNe extending SF by up to a factor of three. Additionally, a new code is introduced to compute the SF duration for a given CCSN model.
Conclusions. The extended SF has important implications on GC formation, including enhanced pollution from stellar winds and increased binary star encounters. These results underscore the need for a refined understanding of CCSNe in estimating SF durations and the formation of multiple stellar populations in GCs.
MEGS: Morphological Evaluation of Galactic Structure
Authors: Çakir U. , Buck T. 
Published: October 2024

Context. Understanding the morphology of galaxies is a critical aspect of astrophysics research, providing insight into the formation, evolution, and physical properties of these vast cosmic structures. Various observational and computational methods have been developed to quantify galaxy morphology, and with the advent of large galaxy simulations, the need for automated and effective classification methods has become increasingly important.
Aims. This paper investigates the use of principal component analysis (PCA) as an interpretable dimensionality reduction algorithm for galaxy morphology using the IllustrisTNG cosmological simulation dataset with the aim of developing a generative model for galaxies.
Methods. We first generate a dataset of 2D images and 3D cubes of galaxies from the IllustrisTNG simulation, focusing on the mass, metallicity, and stellar age distribution of each galaxy. PCA is then applied to this data, transforming it into a lower-dimensional image space, where closeness of data points corresponds to morphological similarity.
Results. We find that PCA can effectively capture the key morphological features of galaxies, with a significant proportion of the variance in the data being explained by a small number of components. With our method we achieve a dimensionality reduction by a factor of ~200 for 2D images and ~3650 for 3D cubes at a reconstruction accuracy below 5%.
Conclusions. Our results illustrate the potential of PCA in compressing large cosmological simulations into an interpretable generative model for galaxies that can easily be used in various downstreaming tasks such as galaxy classification and analysis.
Stable case BB/BC mass transfer to form GW190425-like massive binary neutron star mergers
Authors: Qin Ying , Zhu Jin-Ping , Meynet Georges , Zhang Bing , Wang Fa-Yin , Shu Xin-Wen , Song Han-Feng , Wang Yuan-Zhu , Yuan Liang , Wang Zhen-Han-Tao , Hu Rui-Chong , Wu Dong-Hong , Yi Shuang-Xi , Tang Qing-Wen , Wei Jun-Jie , Wu Xue-Feng , Liang En-Wei 
Published: October 2024

Context. On April 25, 2019, the LIGO-Virgo Collaboration discovered a gravitational-wave (GW) signal from a binary neutron star (BNS) merger, that is, GW190425. Due to the inferred large total mass, the origin of GW190425 remains unclear.
Aims. Assuming GW190425 originated from the standard isolated binary evolution channel, its immediate progenitor is considered to be a close binary system, consisting of a He-rich star and a NS just after the common envelope phase. We aim to study the formation of GW190425 in a solar-like environment by using the detailed binary evolution code MESA.
Methods. We perform detailed stellar structure and binary evolution calculations that take into account mass loss, internal differential rotation, and tidal interactions between a He-rich star and a NS companion. We explore the parameter space of the initial binary properties, including initial NS and He-rich masses and initial orbital period.
Results. We find that the immediate post-common-envelope progenitor system, consisting of a primary ∼2.0 M⊙ (∼1.7 M⊙) NS and a secondary He-rich star with an initial mass of ∼3.0 − 5.5 M⊙ (∼5.5 − 6.0 M⊙) in a close binary with an initial period of ∼0.08 − 0.5 days (∼0.08 − 0.4 days), that experiences stable Case BB/BC mass transfer (MT) during binary evolution, can reproduce the formation of GW190425-like BNS events. Our studies reveal that the secondary He-rich star of the GW190425’s progenitor before its core collapse can be efficiently spun up through tidal interaction, finally remaining as a NS with rotational energy even reaching ∼1052 erg, which is always much higher than the neutrino-driven energy of the supernova (SN) explosion. If the newborn secondary NS is a magnetar, we expect that GW190425 can be the remnant of a magnetar-driven SN, namely a magnetar-driven ultra-stripped SN, a superluminous SN, or a broad-line Type Ic SN.
Conclusions. Our results show that GW190425 could be formed through the isolated binary evolution, which involves a stable Case BB/BC MT just after the common envelope phase. On top of that, we show the He-rich star can be tidally spun up, potentially forming a spinning magnetized NS (magnetar) during the second SN explosion.
eDIG-CHANGES
Authors: Lu Li-Yuan , Li Jiang-Tao , Vargas Carlos J. , Fang Taotao , Benjamin Robert A. , Bregman Joel N. , Dettmar Ralf-Jürgen , English Jayanne , Heald George H. , Jiang Yan , Daniel Wang Q. , Yang Yang 
Published: October 2024

Context. The kinematic information of the extraplanar diffuse ionized gas (eDIG) around galaxies provides clues to the origin of the gas.
Aims. The eDIG-CHANGES project studies the physical and kinematic properties of the eDIG around the CHANG-ES sample of nearby edge-on disk galaxies.
Methods. We use a novel multi-slit narrow-band spectroscopy technique to obtain the spatial distribution of the spectral properties of the ionized gas around NGC 891, which is often regarded as an analogue of the Milky Way. We developed specific data reduction procedures for the multi-slit narrow-band spectroscopy data taken with the MDM 2.4 m telescope. The data presented in this paper cover the Hα and [N II]λλ6548, 6583 Å emission lines.
Results. The eDIG traced by the Hα and [N II] lines shows an obvious asymmetric morphology, being brighter in the northeastern part of the galactic disk and extending a few kiloparsecs above and below the disk. Global variations in the [N II]/Hα line ratio suggest additional heating mechanisms for the eDIG at large heights beyond photoionization. We also construct position-velocity (PV) diagrams of the eDIG based on our optical multi-slit spectroscopy data and compare them to similar PV diagrams constructed with the H I data. The dynamics of the two gas phases are generally consistent with each other. Modelling the rotation curves at different heights from the galactic mid-plane suggests a vertical negative gradient in turnover radius and maximum rotation velocity, with magnitudes of approximately 3 kpc kpc−1 and 22 − 25 km s−1 kpc−1, respectively.
Conclusions. Our measured vertical gradients of the rotation curve parameters suggest significant differential rotation of the ionized gas in the halo, often referred to as the lagging eDIG. Systematic study of the lagging eDIG, using the multi-slit narrow-band spectroscopy technique developed in our eDIG-CHANGES project, will help us to better understand the dynamics of the ionized gas in the halo.
A multi-instrument study of UV bursts and associated surges in AR 12957
Authors: Nelson C. J. , Calchetti D. , Gandorfer A. , Hirzberger J. , Sinjan J. , Solanki S. K. , Berghmans D. , Strecker H. , Blanco J. 
Published: October 2024

Context. The relationship between UV bursts and solar surges is complex, with these events sometimes being observed together and sometimes being observed independently. Why this sporadic association exists is unknown; however, it likely relates to the physical conditions at the site of the energy release that drives these events.
Aims. Here, we aim to better understand the relationship between UV bursts and solar surges through a multi-instrument analysis of several associated events that occurred around the trailing sunspot in AR 12957.
Methods. We used data from Solar Orbiter, the Solar Dynamics Observatory (SDO), and the Interface Region Imaging Spectrograph (IRIS) to achieve our aims. These data were sampled on 3 March 2022 between 09:30:30 UT and 11:00:00 UT, during which time a coordinated observing campaign associated with the Slow Solar Wind Connection Solar Orbiter Observing Plan (SOOP) took place.
Results. Numerous small-scale negative polarity magnetic magnetic features (MMFs) were observed to move quickly (potentially up to 3.3 km s−1) away from a sunspot until they collided with a more stable positive polarity plage region around 7 Mm away. Several UV bursts were identified in IRIS slit-jaw imager (SJI) 1400 Å data co-spatial to where these opposite polarity fields interacted, with spatial scales (< 2 Mm) and lifetimes (< 20 minutes) larger than typical values for such events. Two surges were also observed to occur at these locations, with one being short (5 Mm) and hot (bright in the IRIS SJI images), whilst the other was a cooler (dark in coronal imaging channels), longer surge that appeared to fill an active region loop.
Conclusions. Magnetic reconnection between the negative polarity MMFs around the sunspot and the positive polarity plage region appears to be the driver of these events. Both the speed of the MMFs and the locally open magnetic topology of the plage region could possibly have been important for forming the surges.
Diagnostic des systèmes de production de pommier face aux changements climatiques : cas de M’semrir, Haut Atlas, Maroc
Authors: Lozzi Assia , Chakroun Rim , Hakimi Fatiha , Maatala Nassreddine , Bounadi Imane , Lahrech Taha , Bekkar Younes , Bouaziz Ahmed 
Published: October 2024

Les systèmes de production pomicole dans les zones montagneuses du Haut Atlas, au Maroc, sont confrontés à des contraintes techniques et environnementales, exacerbées par les effets croissants du changement climatique. Cette étude vise à diagnostiquer les systèmes de production de pommier dans la commune de M’semrir, tout en analysant l’impact des variations climatiques locales, afin d’identifier des stratégies d’amélioration pour renforcer la durabilité et la résilience des exploitations. Les conditions climatiques arides à semi-arides donnent un rôle crucial à l’irrigation et à la gestion des ressources en eau. Trois catégories d’exploitations ont été distinguées : moyennes, petites, et micro-exploitations. Au sein de chacun de ces groupes, deux niveaux de performance ont été dégagés, principalement basés sur les rendements, la productivité de l’eau, et la productivité de l’azote. Les principaux défis rencontrés dans la majorité de ces exploitations sont des rendements modestes, une faible productivité de l’eau et une faible productivité partielle de l’engrais azoté, ce qui souligne la nécessité de stratégies d’optimisation pour améliorer l’efficacité des intrants. Une gestion plus efficace de l’irrigation, orientée vers des méthodes économes en eau, pourrait jouer un rôle clé dans la résilience des exploitations. Enfin, des stratégies proactives pour anticiper et atténuer les effets de la sécheresse apparaissent essentielles pour assurer la durabilité de ces systèmes agricoles dans un contexte climatique de plus en plus contraignant.
Frequency-resolved measurement of two-color air plasma terahertz emission
Authors: Hase Eiji , Degert Jérôme , Freysz Eric , Yasui Takeshi , Abraham Emmanuel 
Published: October 2024

We investigated the far-field terahertz beam profile generated from an air plasma induced by two-color femtosecond laser pulses. Under our experimental conditions (filament length shorter than the dephasing length between the two-color pulses), using electro-optic sampling in both ZnTe (0.2–2.2 THz) and GaP (0.4–6.8 THz) crystals, and ultra-broadband ABCD technique (1–17.5 THz), we determined that the THz beam exhibits a unimodal beam pattern below 4 THz and a conical one above 6 THz. This experimental finding is consistent with theoretical studies based on the unidirectional pulse propagation equation, which predict the transition of THz emission from a flat-top profile to a conical one due to the destructive interference of THz waves emitted from the plasma filament. Our results also underscore the importance of accounting for experimental artifacts, such as photo-excited losses in silicon resulting in on-axis THz absorption along with the influence of drilled mirrors, in characterizing the complex spatial and frequency-dependent behavior of two-color plasma-induced terahertz emission.
Naturheilverfahren und Komplementärmedizin: alles im Goldrahmen?
Authors: Stange Rainer 
Published: October 2024

SummaryDie Komplementärmedizin sowie Naturheilverfahren sind bei Patienten in Deutschland stark nachgefragt. Auch gibt es eine große Zahl an Ärzten und medizinisch Tätigen, die diese Leistungen anbieten. Dennoch mangelt es in vielen Bereichen an Anerkennung der Komplementärmedizin von Seiten öffentlicher Einrichtungen und Institutionen wie der gesetzlichen Krankenversicherung. Rechtliche Rahmenbedingungen sowie gute qualifizierende Weiterbildungsangebote sind wichtige Faktoren, um die Rolle der Komplementärmedizin zu stärken.