Miracle-dz/UniFAR-FTUs huggingface dataset:
WIYN OPEN CLUSTER STUDY. XLVIII. THE HARD-BINARY POPULATION OF NGC 188

We present an in-depth study of the hard-binary population of the old (7 Gyr) open cluster NGC 188. Utilizing 85 spectroscopic binary orbits out of a complete sample of 129 detected binary members, we study the cluster binary frequency and the distributions of binary orbital elements among the main-sequence (MS), giant, and blue straggler (BS) populations. The results are derived from our ongoing radial velocity survey of the cluster, which spans in magnitude from the brightest stars in the cluster to V = 16.5 (about 1.1–0.9 M☉), and extends to a projected radius of 17 pc (∼13 core radii). Our detectable binaries have periods ranging from a few days to of order 104 days, and thus are hard binaries that dynamically power the cluster. The MS solar-type hard binaries in NGC 188 are nearly indistinguishable from similar binaries in the Galactic field. We observe a global solar-type MS hard-binary frequency in NGC 188 of 23% ± 2%, which when corrected for incompleteness results in a frequency of 29% ± 3% for binaries with periods less than 104 days. For MS hard binaries in the cluster, we observe a log-period distribution that rises toward our detection limit, a roughly Gaussian eccentricity distribution centered on e = 0.35 (for binaries with periods longer than the circularization period), and a secondary-mass distribution that rises toward lower-mass companions. Importantly, the NGC 188 BS binaries show significantly different characteristics than the solar-type MS binaries in NGC 188. We observe a BS hard-binary frequency of 76% ± 19%, three times that of the MS. The excess of this binary frequency over the normal MS binary frequency is valid at the >99% confidence level. Furthermore, the BS binary eccentricity−log-period distribution is distinct from that of the MS at the 99% confidence level, with the majority of the BS binaries having periods of order 1000 days and lower eccentricities. The secondary-mass distribution for these long-period BS binaries is narrow and peaked with a mean value of about 0.5 M☉. Predictions for mass-transfer products are most closely consistent with the binary properties of these NGC 188 BSs, which comprise two-thirds of the BS population. Additionally, we compare the NGC 188 binaries to those evolved within the sophisticated Hurley et al. (2005) N-body open cluster simulation. The MS hard-binary population predicted by the simulation is significantly different from the MS hard-binary population observed in NGC 188, in frequency and distributions of period and eccentricity. Many of these differences result from the adopted initial binary population, while others reflect on the physics used in the simulation (e.g., tidal circularization). Additional simulations with initial conditions that are better motivated by observations are necessary to properly investigate the dynamical evolution of a rich binary population in open clusters like NGC 188.
Chiral Magnetic Effect at Weak Coupling with Relaxation Dynamics

We provide a resolution of an old issue in weak coupling computation of the Chiral Magnetic Effect (CME) current, where a free chiral fermion theory gives two different results depending on the order of the two limits, $\omega\rightarrow 0$ (frequency) and $k\rightarrow 0$ (spatial momentum). We first argue based on hydrodynamics that in any reasonable interacting theory of chiral fermions the non-commutativity between the two limits should be absent, and we demonstrate this at weak coupling regime in two different frameworks: kinetic theory in the relaxation time approximation, and diagrammatic computation with resummation of damping rate. In the latter computation, we also show that the "pinch" singularity, which would make the summation of ladder diagrams necessary as in the P-even correlation function, is absent in the relevant P-odd correlation function. The correct value of CME current is reproduced even in the presence of relaxation dynamics in both computations.
CARING for xAI

Over the last few years, Artificial Intelligence (AI) has pervaded our lives. As a result, automated tools that “reason” on different scenarios have become more and more common. As this trend continues to grow, it has become necessary to ensure that newly developed tools and technologies can be safely adopted, as demonstrated by the numerous EU regulations. This is especially true when the concept of AI is intertwined with the field of medicine, where every decision may be critical. That is why, in this work, we decided to tackle the problem of automated interpretation of Computed Tomography (CT) scans using an explainable approach. In fact, while several methods based on Machine Learning (ML) are currently available, these are still outperformed by medical doctors and provide answers that cannot be traced back to a logical deduction. This paper presents CARING, a new methodology based on Answer Set Programming (ASP), which returns reliable, easy-to-program and explainable interpretations of CT scans. In particular, CARING makes use of transparent technologies in order to handle medical knowledge provided either by experts or by verified ontologies. This proof of concept shows that Logic Programming is a mature technology that can match the newest challenges in the xAI field.
S0031182022000774jra 1381..1396

Wild mammals, especially rodents, can participate in the life cycle of Schistosoma mansoni; however, the impact of these parasite strains on the severity of schistosomiasis remains unclear. The aim of this study was to comparatively evaluate the parasitological and immunopathological alterations induced by an S. mansoni strain isolated from the wild rodent Holochilus sciureus (HS strain) and a parasite strain isolated from a human (LE strain) in experimentally infected mice. Male BALB/c mice were subcutaneously infected with 50 cercariae/mouse of either the HS or the LE strain and were evaluated for 12 weeks. In the experimental groups, the parasite burden was estimated by worm and egg (feces and tissues) count, and immunopathological alterations were evaluated in the liver and intestines. Compared to experimental infection with the LE parasite strain, HS-infected mice showed reduced number of parasite worms but higher fecundity rate, significant reduction in IL-5, IL-10 and IL-13 concentrations, lower EPO-activity in liver homogenate and higher concentrations of TNFα, IFN-γ, IL-12 and IL-17 in the small intestine homogenate. Moreover, HS infection resulted in higher concentrations of NO end-products in both the liver and intestine, suggesting a predominance of the Th1/Th17 immune response. HS-infected mice also showed higher plasma transaminase levels, formed larger granulomas, and had a higher mortality rate in comparison with LE-infected mice. Data indicate that BALB/c mice infected with the HS strain of S. mansoni showed reduced susceptibility to the parasite but stronger tissue inflammation and high disease severity.
Case Report Peroneal Nerve Palsy Caused by Proximal Fibular Solitary Osteochondroma: Case Report and Literature Review

Osteochondroma is a relatively common benign tumor of the bone, and compressive neuropathies due to osteochondroma are comparatively rare. Here, we present a rare case of osteochondroma of the ﬁ bular head that caused peroneal nerve palsy in an 8-year-old girl. Physical examination revealed 0/5 tibialis anterior, 1/5 extensor hallucis longus, and 1/5 peroneal brevis muscle power — according to the manual muscle testing grading system, as well as numbness on the lateral side of the right leg and the back of the foot. Radiological examination and ultrasound revealed a bone tumor in the head of the right ﬁ bula. Magnetic resonance imaging ruled out spinal nerve root compression. It was discovered that the bone tumor in the ﬁ bular head had compressed and displaced the common peroneal nerve. The patient underwent surgical decompression of the right peroneal nerve. A bone region measuring 22 × 14 × 8 mm was removed. Three months postoperatively, the preoperative neurological de ﬁ cits were found to be nearly resolved. The patient presented with a foot drop for 1 year, but symptoms resolved 3 months after surgery. Conventional wisdom states that surgery should be performed within 3 months, but we recommend that surgery be performed as soon as diagnosis is made even in cases with a long history, as it may improve patient symptoms and outcomes.
Acta Polytechnica

This work reports the construction of constants of motion for a family of time-dependent mass oscillators, achieved by implementing the formalism of form-preserving point transformations. The latter allows obtaining a spectral problem for each constant of motion, one of which leads to a non-orthogonal set of eigensolutions that are, in turn, coherent states. That is, eigensolutions whose wavepacket follows a classical trajectory and saturate, in this case, the Schrödinger-Robertson uncertainty relationship. Results obtained in this form are relatively general, and some particular examples are considered to illustrate the results further. Notably, a regularized Caldirola-Kanai mass term is introduced in an attempt to amend some of the unusual features found in the conventional Caldirola-Kanai case.
POLARIZATION SIGNATURES OF RELATIVISTIC MAGNETOHYDRODYNAMIC SHOCKS IN THE BLAZAR EMISSION REGION. I. FORCE-FREE HELICAL MAGNETIC FIELDS

The optical radiation and polarization signatures in blazars are known to be highly variable during flaring activities. It is frequently argued that shocks are the main driver of the flaring events. However, the spectral variability modelings generally lack detailed considerations of the self-consistent magnetic field evolution modeling; thus, so far the associated optical polarization signatures are poorly understood. We present the first simultaneous modeling of the optical radiation and polarization signatures based on 3D magnetohydrodynamic simulations of relativistic shocks in the blazar emission environment, with the simplest physical assumptions. By comparing the results with observations, we find that shocks in a weakly magnetized environment will largely lead to significant changes in the optical polarization signatures, which are seldom seen in observations. Hence an emission region with relatively strong magnetization is preferred. In such an environment, slow shocks may produce minor flares with either erratic polarization fluctuations or considerable polarization variations, depending on the parameters; fast shocks can produce major flares with smooth polarization angle rotations. In addition, the magnetic fields in both cases are observed to actively revert to the original topology after the shocks. All these features are consistent with observations. Future observations of the radiation and polarization signatures will further constrain the flaring mechanism and the blazar emission environment.
D=5 maximally supersymmetric Yang-Mills theory diverges at six loops

The connection of maximally supersymmetric Yang-Mills theory to the (2,0) theory in six dimensions has raised the possibility that it might be perturbatively ultraviolet finite in five dimensions. We test this hypothesis by computing the coefficient of the first potential ultraviolet divergence of planar (large Nc) maximally supersymmetric Yang-Mills theory in D = 5, which occurs at six loops. We show that the coefficient is nonvanishing. Furthermore, the numerical value of the divergence falls very close to an approximate exponential formula based on the coefficients of the divergences through five loops. This formulapredicts the approximate values of the ultraviolet divergence at loop orders L > 6 in the critical dimension D = 4 + 6/L. To obtain the six-loop divergence we first construct the planar six-loop four-point amplitude integrand using generalized unitarity. The ultraviolet divergence follows from a set of vacuum integrals, which are obtained by expanding the integrand in the external momenta. The vacuum integrals are integrated via sector decomposition, using a modified version of the FIESTA program.
THE “NESSIE” NEBULA: CLUSTER FORMATION IN A FILAMENTARY INFRARED DARK CLOUD

The “Nessie” Nebula is a filamentary infrared dark cloud (IRDC) with a large aspect ratio of over 150:1 (1.°5 × 0.°01 or 80 pc × 0.5 pc at a kinematic distance of 3.1 kpc). Maps of HNC (1–0) emission, a tracer of dense molecular gas, made with the Australia Telescope National Facility Mopra telescope, show an excellent morphological match to the mid-IR extinction. Moreover, because the molecular line emission from the entire nebula has the same radial velocity to within ±3.4 km s−1, the nebula is a single, coherent cloud and not the chance alignment of multiple unrelated clouds along the line of sight. The Nessie Nebula contains a number of compact, dense molecular cores which have a characteristic projected spacing of ∼4.5 pc along the filament. The theory of gravitationally bound gaseous cylinders predicts the existence of such cores, which, due to the “sausage” or “varicose” fluid instability, fragment from the cylinder at a characteristic length scale. If turbulent pressure dominates over thermal pressure in Nessie, then the observed core spacing matches theoretical predictions. We speculate that the formation of high-mass stars and massive star clusters arises from the fragmentation of filamentary IRDCs caused by the “sausage” fluid instability that leads to the formation of massive, dense molecular cores. The filamentary molecular gas clouds often found near high-mass star-forming regions (e.g., Orion, NGC 6334, etc.) may represent a later stage of IRDC evolution.
On semigroups, semirings, and rings of quotients

There are many theorems known about the imbedding of algebraic structures in quotient structures, that is, structures with all the properties of the original ones in which suitable candidates (cancellable elements) become invertible, and such that every element of the larger structure is a quotient of elements of the original structure. The best-known classical theorem of this sort asserts that an integral domain may be imbedded in a field of quotients. The construction of such a field, using equivalence classes of ordered pairs, has been adapted to prove a number of generalizations, such as those of Ore [1(Γ] and Asano [1J for rings and Vandiver [14] for semigroups and semirings. In a negative direction, we have the theorem of Malcev \ΊΓ\ that not every ring without zero divisors can be imbedded in a division ring. On the other hand, if one is willing to give up associativity, such an imbedding can always be accomplished (Neumann H9H). We will confine our attention to associative structures. In [2J, Asano generalized his own work with a different kind of construction of quotients using partial endomorphisms (which he called simply "operators"). This in turn was extensively generalized by Findlay and Lambek [3]. In recent years there have been many papers devoted to the subject of rings of quotients: see, for example, [7, 113 a n d references listed in these. For the purposes of ring theory, constructions via partial homomorphisms and related ideas are surely more elegant and efficient than the old-fashioned, but more concrete, constructions via equivalence classes of ordered pairs. For example, the verifications of associativity and distributivity are trivial when one uses mappings as elements of the quotient structure. However, the student is usually introduced first (perhaps solely) to the more concrete construction. Thus it is of interest to see this construction in perhaps its most general form, where only the essential ideas are present at each step. In the process, it becomes clear that for purposes of extending a multiplicative structure to include quotients, the accompanying additive structure (if any) is of little or no consequence. Hence imbedding theorems
Absorptive Capacity and ERP Implementation in Indian Medium-Sized Firms

Whilst absorptive capacity has been identified as an important contributor to the effective implementation of IT systems, previous studies have failed to explicitly consider the contribution of individual and organizational knowledge processes. Nine case studies of Enterprise Resource Planning ERP implementation were undertaken. The case studies were all undertaken in SMEs in a developing country since this is an important but under researched area for the application of the concept of absorptive capacity. A particular implication of the findings is that firms lacking knowledge of IT implementation cannot simply seek this from external sources but must develop internal organizational knowledge processes if their implementations of IT systems are to be effective. This finding is particularly pertinent to the developing country and SME context of this study, where low levels of experience within the firm and the loss of experienced staff are found to impact on the development of absorptive capacity.
Economic Impact Payments and Household Spending during the Pandemic

ABSTRACT:Households spent only a small fraction of their 2020 Economic Impact Payments (EIPs) within a month or two of arrival, consistent with pandemic constraints on spending, other pandemic programs and social insurance, and the broader disbursement of the EIPs compared to the economic losses during the early stages of the pandemic. While these EIPs did not fill an urgent economic need for most households, the first round of EIPs did provide timely pandemic insurance to some households that were more exposed to the economic losses from the pandemic. Households with lower liquid wealth entering the pandemic and those less able to earn while working from home raised consumption more following receipt of their EIP. While our measurement for later EIPs is not as reliable, our estimates suggest even less spending on average to the second and third rounds of EIPs. Our point estimates imply less short-term spending on average than in response to economic stimulus payments in 2001 or 2008. While our analysis lacks the power to measure longer-term spending effects, the lack of short-term spending contributed to strong household balance sheets as the direct economic effects of the pandemic on households waned.
Mechanics of porous continua

Description of the Deformation and Kinematics of a Saturated Porous Medium, Mass Conservation. Momentum Balance, Stress Tensor. Thermodynamics of Open Continua. Linear Thermoporoelastic Behaviour. Poroplastic Behaviour. Hereditary Behaviours. Surfaces of Discontinuity. Linearized Quasistatic Evolutions in Thermoporoelasticity, Direct Methods of Resolution. Quasistatic Evolutions, Uniqueness of Solution, Numerical Methods of Resolution. Reactive Partially Saturated Porous Media. References. Index.
ALBEDO PROPERTIES OF MAIN BELT ASTEROIDS BASED ON THE ALL-SKY SURVEY OF THE INFRARED ASTRONOMICAL SATELLITE AKARI

We present an analysis of the albedo properties of main belt asteroids (MBAs) detected by the All-Sky Survey of the infrared astronomical satellite AKARI. The characteristics of 5120 asteroids detected by the survey, including their sizes and albedos, were cataloged in the Asteroid Catalog Using AKARI (AcuA). Size and albedo measurements were based on the standard thermal model, using inputs of infrared fluxes and absolute magnitudes measured at optical wavelengths. MBAs, which account for 4722 of the 5120 AcuA asteroids, have semimajor axes of 2.06–3.27 AU, except for the near-Earth asteroids. AcuA provides a complete data set of all MBAs brighter than the absolute magnitude of H < 10.3, which corresponds to the diameter of d > 20 km. We confirmed that the albedo distribution of the MBAs is strongly bimodal as was already known from the past observations, and that the bimodal distribution occurs not only in the total population, but also within inner, middle, and outer regions of the main belt. The bimodal distribution in each group consists of low-albedo components in C-type asteroids and high-albedo components in S-type asteroids. We found that the small asteroids have much more variety in albedo than the large asteroids. In spite of the albedo transition process like space weathering, the heliocentric distribution of the mean albedo of asteroids in each taxonomic type is nearly flat. The mean albedo of the total, on the other hand, gradually decreases with an increase in semimajor axis. This can be explained by the compositional ratio of taxonomic types; that is, the proportion of dark asteroids such as C- and D-types increases, while that of bright asteroids such as S-type decreases, with increasing heliocentric distance. The heliocentric distributions of X-subclasses: E-, M-, and P-types, which can be divided based on albedo values, are also examined. P-types, which are the major component in X-types, are distributed throughout the main belt regions, and the abundance of P-types increases beyond 3 AU. This distribution is similar to that of C- or D-types.
The solar neighbourhood in angle coordinates: the Hyades moving group

I investigate the suggestion that the Hyades moving group in the solar neighbourhood is the result of a recent inner Lindblad resonance. I use dynamical ‘torus’ models of the Galaxy to understand the expected distribution of solar neighbourhood stars in angle coordinates for phase-mixed models and models which include a resonant component. I show that attempts to find the signatures of resonances in angle coordinates are strongly influenced by selection effects, including rather subtle effects associated with the relationship between action and angle for stars at a given point. These effects mean that one cannot use simple tests to determine whether substructures seen in the solar neighbourhood are associated with any given resonance.
THE MEGAMASER COSMOLOGY PROJECT. VIII. A GEOMETRIC DISTANCE TO NGC 5765b

As part of the Megamaser Cosmology Project, here we present a new geometric distance measurement to the megamaser galaxy NGC 5765b. Through a series of very long baseline interferometry observations, we have confirmed the water masers trace a thin, sub-parsec Keplerian disk around the nucleus, implying an enclosed mass of 4.55 ± 0.40 × 107 M⊙. Meanwhile, from single-dish monitoring of the maser spectra over two years, we measured the secular drifts of maser features near the systemic velocity of the galaxy with rates between 0.5 and 1.2 km s−1 yr−1. Fitting a warped, thin-disk model to these measurements, we determine a Hubble Constant H0 of 66.0 ± 6.0 km s−1 Mpc−1 with an angular-diameter distance to NGC 5765b of 126.3 ± 11.6 Mpc. Apart from the distance measurement, we also investigate some physical properties related to the maser disk in NGC 5765b. The high-velocity features are spatially distributed into several clumps, which may indicate the existence of a spiral density wave associated with the accretion disk. For the redshifted features, the envelope defined by the peak maser intensities increases with radius. The profile of the systemic masers in NGC 5765b is smooth and shows almost no structural changes over the two years of monitoring time, which differs from the more variable case of NGC 4258.
Shock acceleration of electrons in the presence of synchrotron losses – I. Test-particle theory

We discuss a semi-analytical solution of the transport equation for electrons at a non-relativistic shock in the presence of synchrotron energy losses. We calculate the spectrum of accelerated (test) particles at any point upstream and downstream of the shock for an arbitrary diffusion coefficient, and we specialize the results to three cases: (1) diffusion constant in momentum [D(p) = D 0 ], (2) Bohm diffusion [D(p) ∝ p] and (3) Kolmogorov diffusion [D(p) ∝ p 1/3 ]. Of special importance is the determination of the shape of the cut-off in the electron spectrum which depends on the diffusion properties felt by particles in the shock region. The formalism can be generalized to the case of a shock with an upstream precursor induced by the dynamical reaction of accelerated particles.