Miracle-dz/UniFAR-FTUs huggingface dataset:
Surface waves in protoplanetary disks induced by outbursts: Concentric rings in scattered light

Context. Vertically hydrostatic protoplanetary disk models are based on the assumption that the main heating source, stellar irradiation, does not vary much with time. However, it is known that accreting young stars are variable sources of radiation. This is particularly evident for outbursting sources such as EX Lupi and FU Orionis stars. Aims. We investigate how such outbursts affect the vertical structure of the outer regions of the protoplanetary disk, in particular their appearance in scattered light at optical and near-infrared wavelengths. Methods. We employ the 3D FARGOCA radiation-hydrodynamics code, in polar coordinates, to compute the time-dependent behavior of the axisymmetric disk structure. The temperature is computed self-consistently and time-dependently from the irradiation flux using a two-stage radiative transfer method: first the direct illumination is computed; then the diffuse radiation is treated with the flux-limited diffusion method. The outbursting inner disk region is not included explicitly. Instead, its luminosity is added to the stellar luminosity and is thus included in the irradiation of the outer disk regions. For time snapshots of interest we insert the density structure into the RADMC-3D radiative transfer code and compute the appearance of the disk at optical/near-infrared wavelengths, where we observe stellar light that is scattered off the surface of the disk. Results. We find that, depending on the amplitude of the outbursts, the vertical structure of the disk can become highly dynamic, featuring circular surface waves of considerable amplitude. These “hills” and “valleys” on the disk’s surface show up in the scattered light images as bright and dark concentric rings. Initially these rings are small and act as standing waves, but they subsequently lead to outward propagating waves, like the waves produced by a stone thrown into a pond. These waves continue long after the actual outburst has died out. Conclusions. Single, periodic, or quasiperiodic outbursts of the innermost regions of protoplanetary disks will necessarily lead to wavy structures on the surface of these disks at all radii. We propose that some of the multi-ringed structures seen in optical/infrared images of several protoplanetary disks may have their origin in outbursts that occurred decades or centuries ago. However, the multiple rings seen at (sub-)millimeter wavelengths in HL Tau and several other disks are not expected to be related to such waves.
Towards improving challenging stochastic defect detection in SEM images based on improved YOLOv5

With the progression of deep learning algorithms in computer vision, a lot of research is taking place in the semiconductor industry towards improving real-time defect detection and classification analysis. An Automated Defect Classification and Detection (ADCD) framework not only enables rapid measurement of dimensions and classification of defects, but also helps minimize production costs, engineering time as well as tool cycle time associated with the defect inspection process. As we continue to shrink the pitch (below 36nm), defect characterization at wafer scale becomes a key issue as it demands rapid measurement but without losing accuracy and repeatability. Also, in the context of high NA lithography (thin resist), accurate metrology becomes difficult with very noisy as well as low contrast images (No BKM exists till now). Human eyes generally demonstrate close to the Bayesian Error limit in detecting smaller objects (for example, extracting contextual information instantaneously from nanoscale defects in SEM images). However, for most One-stage and Two-stage object detectors, this is still a very challenging task due to variable image resolution and SEM (scanning electron microscope) image quality (low SNR). In this research work, we have experimented with different modified YOLOv5 object detectors to improve challenging stochastic defect detection precision. In this work, we have proposed an ensemble strategy by empirically combining multiple custom-trained models (YOLOv5n, YOLOv5s, YOLOv5m, YOLOv5l, and YOLOv5x) together at the test and inference time. We have noticed four YOLOv5 architecture variants are outperforming against our previous Ensemble ResNets model with improvements of the average precision metric (AP) of the most difficult defect classes as p gap and microbridges as well as overall mAP accuracy. With Ensemble YOLOv5, the p gap AP and microbridge AP metrices have been improved by 35% and 25.33%, respectively, whereas the overall mAP has been improved by 6.25%. The proposed Automated Defect Classification and Detection (ADCD) framework can also be used for high resolution and high-speed metrology, providing rapid identification of defects with improved certainty and further root cause investigation.
Comaneci-Assisted Coiling of Wide-Necked Intracranial Aneurysm: A Single-Center Preliminary Experience

Background: Wide-necked aneurysms remain challenging for both coiling and microsurgical clipping. They often require additional techniques to prevent coil prolapse into the parent artery, such as balloon- and stent-assisted coiling. Comaneci is an expandable and removable stent that acts as a bridging device and does not interfere with the blood flow of the parent artery. Methods: We retrospectively reviewed our institutional radiological and clinical chart of patients treated for saccular intracranial aneurysm via endovascular Comaneci-assisted coiling. The aim of the study was to report our preliminary experience in Comaneci-assisted coiling of wide-necked intracranial aneurysms. Results: We included 14 patients in the study. Of these, 11 had a ruptured intracranial aneurysm and were treated with Comaneci-assisted coiling. We registered five minor intraprocedural complications and two intraprocedural failures of the device. At one-year follow-up, a satisfying aneurysm occlusion was observed in 85% of the cases. Conclusions: Though long-term follow-up data and larger case series are needed, this preliminary study showed the feasibility of the Comaneci-assisted coiling method for both ruptured and unruptured wide-neck intracranial aneurysms, with similar occlusion rates as balloon-assisted coiling. However, we registered high incidence of thromboembolic complications; these were probably related to the lack of heparin administration. The main advantageous application of this technique is likely in cases of ruptured intracranial aneurysms, as there is no need for post-procedural antiplatelet therapy.
Going Abroad and Going Green: The Effects of Top Management Teams’ Overseas Experience on Green Innovation in the Digital Era

Green innovation has become one of the most important approaches to achieving sustainable development in modern business. Top management team (TMT)’s overseas experience, as one type of unique resources, constitutes the cognitive basis of the team and thus influences firms’ strategic decision-making. Based on the upper echelon theory, this study aims to investigate the effect of TMT’s overseas experiences on green innovation performances. By utilizing a panel dataset of Chinese listed firms, this study shows that TMTs’ overseas experience indeed promotes firms’ green innovation performance and that both firms’ digital transformation and regions’ digital economy development positively moderate the relationship between TMTs’ overseas experience and green innovation. These findings not only help managers better organize the TMT and green innovation strategy but also draw policymakers’ attention to the importance of the digital economy and sustainable development.
The Tsallis distribution in proton?proton collisions at $\sqrt{s}$ = 0.9 TeV at the LHC

The Tsallis distribution has been used recently to fit the transverse momentum distributions of identified particles by the STAR (Abelev et al (STAR Collaboration) 2007 Phys. Rev. C 75 064901) and PHENIX (Adare et al (PHENIX Collaboration) 2011 Phys. Rev. C 83 064903) collaborations at the Relativistic Heavy Ion Collider and by the ALICE (Aamodt et al (ALICE Collaboration) 2011 Eur. Phys. J. C 71 1655) and CMS (Khachatryan et al (CMS Collaboration) 2011 J. High Energy Phys. JHEP05(2011)064) collaborations at the Large Hadron Collider. Theoretical issues are clarified concerning the thermodynamic consistency of the Tsallis distribution in the particular case of relativistic high-energy quantum distributions. An improved form is proposed for describing the transverse momentum distribution and fits are presented together with estimates of the parameter q and the temperature T.
SUBSTELLAR OBJECTS IN NEARBY YOUNG CLUSTERS (SONYC). VI. THE PLANETARY-MASS DOMAIN OF NGC 1333

Within the SONYC (Substellar Objects in Nearby Young Clusters) survey, we investigate the frequency of free-floating planetary-mass objects (planemos) in the young cluster NGC 1333. Building upon our extensive previous work, we present spectra for 12 of the faintest candidates from our deep multi-band imaging, plus seven random objects in the same fields, using MOIRCS on Subaru. We confirm seven new sources as young very low mass objects (VLMOs), with Teff of 2400–3100 K and mid-M to early-L spectral types. These objects add to the growing census of VLMOs in NGC 1333, now totaling 58. Three confirmed objects (one found in this study) have masses below 15 MJup, according to evolutionary models, thus are likely planemos. We estimate the total planemo population with 5–15 MJup in NGC 1333 is ≲ 8. The mass spectrum in this cluster is well approximated by dN/dM ∝ M−α, with a single value of α = 0.6 ± 0.1 for M < 0.6 M☉, consistent with other nearby star-forming regions, and requires α ≲ 0.6 in the planemo domain. Our results in NGC 1333, as well as findings in several other clusters by ourselves and others, confirm that the star formation process extends into the planetary-mass domain, at least down to 6 MJup. However, given that planemos are 20–50 times less numerous than stars, their contribution to the object number and mass budget in young clusters is negligible. Our findings disagree strongly with the recent claim from a microlensing study that free-floating planetary-mass objects are twice as common as stars—if the microlensing result is confirmed, those isolated Jupiter-mass objects must have a different origin from brown dwarfs and planemos observed in young clusters.
Long-Term Effect on Health-Related Quality of Life in Patients With COVID-19 Requiring Hospitalization Compared to Non-hospitalized COVID-19 Patients and Healthy Controls

Background In this study, we aimed to evaluate the health-related quality of life (HRQL) in patients with severe coronavirus disease 2019 (COVID-19) six months after their hospitalization and compare it to that of non-hospitalized patients with mild COVID-19 and healthy controls. Methodology Participants were enrolled between September 2021 and April 2022 and included hospitalized COVID-19 patients at General Hospital of Athens “Hippocration” who had been discharged at least six months prior to enrollment, non-hospitalized patients with COVID-19, and healthy controls. Collected data included demographics, disease severity, medication history, and comorbidities. Participants completed a EuroQol 5 Dimensions 5Levels (EQ5D5L), a Short Form 36 version 2 (SF36v2), a Functional Assessment of Chronic Illness Therapy-Fatigue (FACIT-F), and a Post-COVID-19 Functional Status Scale (PCFSS) regarding HRQL before and six months after infection with severe acute respiratory syndrome coronavirus 2. In the case of healthy controls, two sets of questionnaires were completed at least six months apart. Statistical analysis was performed using the SPSS version 25 software (IBM Corp., Armonk, NY, USA). Results A total of 151 participants were enrolled. Hospitalized patients with COVID-19 demonstrated a statistically significant deterioration in most parameters of SF36v2 as well as both parameters of the EQ5D5L and FACIT-F questionnaires. Hospitalized patients exhibited worse results in SF36v2 and EQ5D5L when compared to both healthy controls as well as those with mild COVID-19 (p < 0.05). Hospitalized women, in particular, were shown to fare worse than other women in parameters associated with both mental/psychological and physical health (p < 0.05). Hospitalized patients between 41 and 60 years old demonstrated a statistically significant drop in the scores of all three main questionnaires compared to their previous health status (p < 0.05). Hospitalized patients between 61 and 80 years old exhibited a similar trend, but statistical significance was achieved in fewer parameters. HRQL decline was greater in both age groups compared to that of healthy and milder disease counterparts. There was a significant correlation between the results from the three main questionnaires. Similarly, PCFS scale values were shown to correlate with disease severity (hospitalization or not) and age. Conclusions HRQL remained noticeably impacted six months after hospitalization due to COVID-19. The physical and mental/psychological stress of severe COVID-19 translated into lasting health deterioration, especially for women and those aged 41-60 years old. The use of questionnaires, such as those implemented in this study, might help in the early detection of patients who could benefit from rehabilitation programs. Psychological, as well as physical and social, support is crucial to alleviate the burden of post-COVID-19 symptomatology and expedite the recovery of this group of patients.
The MUSIC of Galaxy Clusters II: X-ray global properties and scaling relations

We present the X-ray properties and scaling relations of a large sample of clusters extracted from the Marenostrum MUltidark SImulations of galaxy Clusters (MUSIC) dataset. We focus on a sub-sample of 179 clusters at redshift z � 0.11, with 3.2 × 10 14 h −1 M⊙ < Mvir < 2 × 10 15 h −1 M⊙, complete in mass. We employed the X-ray photon simulator PHOX to obtain synthetic Chandra observations and derive observable-like global properties of the intracluster medium (ICM), as X-ray temperature (TX) and luminosity (LX). TX is found to slightly under-estimate the true mass-weighted temperature, although tracing fairly well the cluster total mass. We also study the effects of TX on scaling relations with cluster intrinsic properties: total (M500 and gas Mg,500 mass; integrated Compton parameter (YSZ) of the Sunyaev-Zel’dovich (SZ) thermal effect; YX = Mg,500 TX. We confirm that YX is a very good mass proxy, with a scatter on M500 YX and YSZ YX lower than 5%. The study of scaling relations among X-ray, intrinsic and SZ properties indicates that simulated MUSIC clusters reasonably resemble the self-similar prediction, especially for correlations involving TX. The observational approach also allows for a more direct comparison with real clusters, from which we find deviations mainly due to the physical description of the ICM, affecting TX and, particularly, LX.
Mercury's Magnetic Field in the MESSENGER Era

MESSENGER magnetometer data show that Mercury's magnetic field is not only exceptionally weak but also has a unique geometry. The internal field resembles an axial dipole that is offset to the North by 20% of the planetary radius. This implies that the axial quadrupol is particularly strong while the dipole tilt is likely below 0.8 degree. The close proximity to the sun in combination with the weak internal field results in a very small and highly dynamic Hermean magnetosphere. We review the current understanding of Mercury's internal and external magnetic field and discuss possible explanations. Classical convection driven core dynamos have a hard time to reproduce the observations. Strong quadrupol contributions can be promoted by different measures, but they always go along with a large dipole tilt and generally rather small scale fields. A stably stratified outer core region seems required to explain not only the particular geometry but also the weakness of the Hermean magnetic field. New interior models suggest that Mercury's core likely hosts an iron snow zone underneath the core-mantle boundary. The positive radial sulfur gradient likely to develop in such a zone would indeed promote stable stratification. However, even dynamo models that include the stable layer show Mercury-like magnetic fields only for a fraction of the total simulation time. Large scale variations in the core-mantle boundary heat flux promise to yield more persistent results but are not compatible with the current understanding of Mercury's lower mantle.
GLOBAL SIMULATIONS OF MAGNETOROTATIONAL INSTABILITY IN THE COLLAPSED CORE OF A MASSIVE STAR

We performed the first global numerical simulations of magnetorotational instability from a sub-magnetar-class seed magnetic field in core-collapse supernovae. As a result of axisymmetric ideal MHD simulations, we found that the magnetic field is greatly amplified to magnetar-class strength. In the saturation phase, a substantial part of the core is dominated by turbulence, and the magnetic field possesses dominant large-scale components, comparable to the size of a proto-neutron star. A pattern of coherent channel flows, which generally appears during the exponential growth phase in previous local simulations, is not observed in our global simulations. While the approximate convergence in the exponential growth rate is attained by increasing spatial resolution, that of the saturation magnetic field is not achieved due to still large numerical diffusion. Although the effect of the magnetic field on the dynamics is found to be mild, a simulation with a high enough resolution might result in a larger impact.
The Planet Formation Potential around a 45 Myr Old Accreting M Dwarf

Debris disk detections around M dwarfs are rare, and so far no gas emission has been detected from an M dwarf debris disk. This makes the 45 Myr old M dwarf WISE J080822.18-644357.3 a bit of a curiosity; it has a strong infrared excess at an age beyond the lifetime of a typical planet-forming disk, and also exhibits broad Hα emission consistent with active accretion from a gaseous disk. To better understand the cold gas and dust properties of this system, we obtained ALMA observations of the 1.3 mm continuum and the CO/13CO/C18O J = 2–1 emission lines. No cold CO gas is detected from this system, ruling out a gas-rich protoplanetary disk. Unresolved dust continuum emission is detected at a flux of 198 ± 15 μJy, consistent with 0.057 ± 0.006 M⊕ worth of optically thin dust, and consistent with being generated through a collisional cascade induced by large bodies at radii <16 au. With a sufficiently strong stellar wind, dust grains released in the outer disk can migrate inward via PR drag, potentially serving as a source of grains for the strong infrared excess.
FORMATION OF BLACK WIDOWS AND REDBACKS—TWO DISTINCT POPULATIONS OF ECLIPSING BINARY MILLISECOND PULSARS

Eclipsing binary millisecond pulsars (MSPs; the so-called black widows and redbacks) can provide important information about accretion history, pulsar irradiation of their companion stars, and the evolutionary link between accreting X-ray pulsars and isolated MSPs. However, the formation of such systems is not well understood, nor the difference in progenitor evolution between the two populations of black widows and redbacks. Whereas both populations have orbital periods between 0.1 and 1.0 days, their companion masses differ by an order of magnitude. In this paper, we investigate the formation of these systems via the evolution of converging low-mass X-ray binaries by employing the MESA stellar evolution code. Our results confirm that one can explain the formation of most of these eclipsing binary MSPs using this scenario. More notably, we find that the determining factor for producing either black widows or redbacks is the efficiency of the irradiation process, such that the redbacks absorb a larger fraction of the emitted spin-down energy of the radio pulsar (resulting in more efficient mass loss via evaporation) compared to that of the black widow systems. We argue that geometric effects (beaming) are responsible for the strong bimodality of these two populations. Finally, we conclude that redback systems do not evolve into black widow systems with time.
THE INNER STRUCTURE OF THE TW HYA DISK AS REVEALED IN SCATTERED LIGHT

We observe a significant change in the TW Hya disk interior to 40 au via archival unpolarized multi-wavelength Hubble Space Telescope/STIS and NICMOS images with an inner working angle of 0. ″4 (22 au). Our images show the outer edge of a clearing at every wavelength with similar behavior, demonstrating that the feature is structural, rather than due to some property of polarized light in the disk. We compare our observations to those taken by Akiyama et al. and Rapson et al., and discuss the spectral evolution of the disk interior to 80 au. We construct a model with two gaps: one at 30 au and one at 80 au that fit the observed surface brightness profile but overpredicts the absolute brightness of the disk. Our models require an additional dimming to be consistent with observations, which we tentatively ascribe to shadowing. The gap structures seen in scattered light are spatially coincident with sub-millimeter detections of CO and N2H+, and are near expected condensation fronts of these molecular species, providing tentative evidence that the structures seen in scattered light may be correlated with chemical changes in the disk.
A Generational Divide? Coping With Ethnic Prejudice and Inequality Among Romanian Roma Transnational Returnees

Roma people are likely Europe’s most discriminated and marginalized minority. In the past years, increasing attention has been paid to their migration to Western Europe and their limited social mobility in their countries of destination. Our article focuses on the “post‐return” experiences of Roma and the changes generated by return migration in their communities of origin, a topic largely neglected so far. We build on recent debates around post‐return positionality, asking how adult and old Roma returnees experience return. We thus contribute to the growing literature on return migration and lifecourse that distinguishes between the return migration of children and youth, that of adults, and that of older migrants. Focusing on Roma returnees, we employ an understanding of migration not just as a means of generating resources, but also as a learning process where the Roma population acquires new ideas and a sense of agency and dignity. Informed by long‐term fieldwork in ethnically mixed localities in Romania (including participant observation and 76 semi‐structured interviews), we inquire into the ethnic relations and negotiations between Roma and non‐Roma populations. Migration results in a weakening of the economic dependency of the Roma on the non‐Roma. In this new context, which is still marred by ethnic prejudice and inequality, we analysed how local interethnic relations were reshaped by the returned Roma’s new consumption practices, new modes of communication, and new claims for equality. While adult Roma tend to demand equality and decent treatment, setting in motion a process of ethnic change, older returned Roma tend to maintain more submissive practices.