Miracle-dz/UniFAR-FTUs huggingface dataset:
Biogeography and Systematics of the Genus Axyris (Amaranthaceae s.l.)

Axyris is a small genus of six species with a disjunct geographic range. Five species are present in Siberia, Central Asia, the Himalayas, and Tibet, whereas Axyris caucasica has been registered in the Central Caucasus only. Axyris species diversity is the highest in the Altai Mountains (four spp.), followed by the Tian Shan and Pamir Mountains (three spp.), and the Himalayas and Tibet (two spp.). Axyris sphaerosperma, sometimes considered endemic to Southern Siberia, in fact has a disjunct range: it is present in the lowlands of Eastern Siberia and in the Altai, Tian Shan, and Pamir Mountains. It has also been found in Mongolia and China for the first time. An updated detailed distribution of Axyris in Siberia is presented on the basis of thorough herbarium revisions. One nuclear and three plastid markers were selected for phylogenetic analysis. Divergence times were estimated using a time-calibrated Bayesian approach. Axyris shows two major clades: an Axyris amaranthoides clade and a clade including the remaining species. The latter clade consists of two subclades (A. sphaerosperma/A. caucasica and A. mira/A. prostrata + A. hybrida). The crown age for Axyris dates back to the Early Pliocene (~5.11 mya, the Zanclean). The ancestral range of Axyris covers Southern Siberia, Mongolia, NW China, and the Tian Shan/Pamir Mountains, with extensions toward Eastern Siberia, the Himalayas/Tibet, and the Caucasus. Fruit and seed characteristics of Axyris are discussed with reference to the present phylogenetic results. Closely related A. sphaerosperma and A. caucasica have the thickest seed coat among all Chenopodiaceae, and these traits have probably evolved as adaptations to extremely low winter temperatures. This reproductive peculiarity may explain the disjunct range of A. sphaerosperma, which is restricted to harsh climatic conditions.
A Study on LPG injection based speed regulator for dual fuel diesel engine

Diesel engines are popularly interested due to their great economic efficiency and the high amount of harmful emissions released. The conversion of using multi-fuel engines aims to reduce emissions, and diversifying alternative energy sources to replace diesel fuel, is a potential solution. This paper presents a method to convert the fuel system of the DI-diesel engine type Vikyno RV125 to LPG-diesel dual combustion mode and preliminarily evaluate performance characteristics operating with the LPG injection-based speed regulator. An LPG injector controller circuit was actuated to operate the engine with different load modes up to 5.0kW at corresponding engine speeds. The air intake manifold was modified to calibrate the air-mass flow to effective performance. The experimental result revealed that the changed system could operate in LPG-diesel dual combustion mode. The operating stability of the engine was recognized at speeds up to 1600rpm. A study on engine exhaust emissions will be performed in the next research stage.
The dust grain size–stellar luminosity trend in debris discs

The cross section of material in debris discs is thought to be dominated by the smallest grains that can still stay in bound orbits despite the repelling action of stellar radiation pressure. Thus the minimum (and typical) grain size $s_\text{min}$ is expected to be close to the radiation pressure blowout size $s_\text{blow}$. Yet a recent analysis of a sample of Herschel-resolved debris discs showed the ratio $s_\text{min}/s_\text{blow}$ to systematically decrease with the stellar luminosity from about ten for solar-type stars to nearly unity in the discs around the most luminous A-type stars. Here we explore this trend in more detail, checking how significant it is and seeking to find possible explanations. We show that the trend is robust to variation of the composition and porosity of dust particles. For any assumed grain properties and stellar parameters, we suggest a recipe of how to estimate the "true" radius of a spatially unresolved debris disc, based solely on its spectral energy distribution. The results of our collisional simulations are qualitatively consistent with the trend, although additional effects may also be at work. In particular, the lack of grains with small $s_\text{min}/s_\text{blow}$ for lower luminosity stars might be caused by the grain surface energy constraint that should limit the size of the smallest collisional fragments. Also, a better agreement between the data and the collisional simulations is achieved when assuming debris discs of more luminous stars to have higher dynamical excitation than those of less luminous primaries. This would imply that protoplanetary discs of more massive young stars are more efficient in forming big planetesimals or planets that act as stirrers in the debris discs at the subsequent evolutionary stage.
Silica-Filled Polyacrylonitrile Solutions: Rheology, Morphology, Coagulation, and Fiber Spinning

The fumed silica influence on the morphology, coagulation processes, and rheological properties of suspensions in dimethyl sulfoxide (DMSO) and polyacrylonitrile (PAN)–DMSO solutions has been studied for the production of composite films and fibers. It has been shown that silica–DMSO concentrated suspensions (24 wt%) form a weak gel with a yield point of about 200 Pa. At concentrations of ~5 wt% and above the dispersions, depending on the shear stress, are pseudoplastic or dilatant liquids. It has been found that the silica addition method into a PAN solution has a significant impact on the aggregates dispersibility and the rheological behavior of the obtained systems. A thixotropy appearance and a sharp increase in the relaxation time were observed for PAN solutions at a SiO2 content of more than 3−5 wt%, which indicates the formation of structures with a gel-like rheological behavior. Upon reaching the critical stress their destruction takes place and the system starts to behave like a viscoelastic liquid. Two spinning methods have been used for preparing fibers: standard wet and mechanotropic. By the mechanotropic method it is possible to achieve a higher draw ratio at spinning and to obtain fibers with better mechanical properties. It is possible to spin fibers from PAN solutions containing up to 15 wt% of silica per polymer with a tensile strength up to 600 MPa.
The Large-scale Interstellar Medium of SS 433/W50 Revisited

With new high-resolution CO and H i data, we revisited the large-scale interstellar medium (ISM) environment toward the SS 433/W50 system. We find that two interesting molecular cloud (MC) concentrations, G39.315−1.155 and G40.331−4.302, are well aligned along the precession cone of SS 433 within a smaller opening angle of ∼±7°. The kinematic features of the two MCs at ∼73–84 km s−1, as well as those of the corresponding atomic-gas counterparts, are consistent with the kinematic characteristics of SS 433. That is, the receding gas from SS 433 jet is probably responsible for the redshifted feature of G39.315−1.155 near the Galactic plane, and the approaching one may power the blueshifted gas of G40.331−4.302 toward the observer. Moreover, the H i emission at VLSR ∼ 70–90 km s−1 displays the morphological resemblance with the radio nebula W50. We suggest that the VLSR = 77 ± 5 km s−1 gas is physically associated with SS 433/W50, leading to a near kinematic distance of 4.9 ± 0.4 kpc for the system. The observed gas features, which are located outside the current radio boundaries of W50, are probably the fossil record of jet–ISM interactions at ∼105 years ago. The energetic jets of the unique microquasar have profound effects on its ISM environment, which may facilitate the formation of molecular gas on the timescale of ≲0.1 Myr for the ram pressure of ∼2 × 106 K cm−3.
Novel InGaSb/AlP Quantum Dots for Non-Volatile Memories

Non-volatile memories based on the flash architecture with self-assembled III–V quantum dots (SAQDs) used as a floating gate are one of the prospective directions for universal memories. The central goal of this field is the search for a novel SAQD with hole localization energy (Eloc) sufficient for a long charge storage (10 years). In the present work, the hole states’ energy spectrum in novel InGaSb/AlP SAQDs was analyzed theoretically with a focus on its possible application in non-volatile memories. Material intermixing and formation of strained SAQDs from a GaxAl1−xSbyP1−y, InxAl1−xSbyP1−y or an InxGa1−xSbyP1−y alloy were taken into account. Critical sizes of SAQDs, with respect to the introduction of misfit dislocation as a function of alloy composition, were estimated using the force-balancing model. A variation in SAQDs’ composition together with dot sizes allowed us to find that the optimal configuration for the non-volatile memory application is GaSbP/AlP SAQDs with the 0.55–0.65 Sb fraction and a height of 4–4.5 nm, providing the Eloc value of 1.35–1.50 eV. Additionally, the hole energy spectra in unstrained InSb/AlP and GaSb/AlP SAQDs were calculated. Eloc values up to 1.65–1.70 eV were predicted, and that makes unstrained InGaSb/AlP SAQDs a prospective object for the non-volatile memory application.
A perturbative approach to the construction of initial data on compact manifolds

We discuss the implementation of Butscher's method \cite{But06,But07} for the construction of solutions to the extended constraint equations, for the vacuum Einstein field equations, in the case of compact manifolds. The method is then applied to the construction of nonlinear perturbations of constant mean curvature initial data of constant negative sectional curvature. We prove the existence of a neighbourhood of solutions to the constraint equations around such initial data, with particular components of the extrinsic curvature and electric/magnetic parts of the spacetime Weyl curvature prescribed as free data. The space of such free data is parametrised explicitly.
The Gravitational Wave Signal from Core-collapse Supernovae

We study gravitational waves (GWs) from a set of 2D multigroup neutrino radiation hydrodynamic simulations of core-collapse supernovae (CCSNe). Our goal is to systematize the current knowledge about the post-bounce CCSN GW signal and recognize the templatable features that could be used by the ground-based laser interferometers. We demonstrate that, starting from ∼400 ms after core bounce, the dominant GW signal represents the fundamental quadrupole (l = 2) oscillation mode (f-mode) of the proto–neutron star (PNS), which can be accurately reproduced by a linear perturbation analysis of the angle-averaged PNS profile. Before that, in the time interval between ∼200 and ∼400 ms after bounce, the dominant mode has two radial nodes and represents a g-mode. We associate the high-frequency noise in the GW spectrograms above the main signal with p-modes, while below the dominant frequency there is a region with very little power. The collection of models presented here summarizes the dependence of the CCSN GW signal on the progenitor mass, equation of state, many-body corrections to the neutrino opacity, and rotation. Weak dependence of the dominant GW frequency on the progenitor mass motivates us to provide a simple fit for it as a function of time, which can be used as a prior when looking for CCSN candidates in the LIGO data.
A break in the high-redshift stellar mass Tully-Fisher relation

We investigate the stellar-mass Tully-Fisher relation (TFR) between the stellar mass and the integrated gas velocity dispersion, quantified by the kinematic estimator S_0. 5 measured from strong emission lines in spectra of galaxies at 0 3 the scatter increases and the existence of a correlation is not obvious. The high-luminosity sample exhibits a flatter slope of 1.5$\pm$0.2 at z<3 compared to the low-luminosity sample slope of 2.9$\pm$0.3, suggesting a turnover in the TFR. The combined sample is well fit with a break in the TFR at a characteristic stellar mass scale of M*~10$^{10}$ M$_{\odot}$, with no significant evolution out to z~3. We demonstrate that a break in the TFR with a steeper slope at the low-mass end is a natural consequence of galaxy models with a mass-dependent stellar to halo-mass ratio.
Patient Portal Use Among Diabetic Patients With Different Races and Ethnicities

Background Patient portal (PP) use varies among different patient populations, specifically among those with diabetes mellitus (DM). In addition, it is still uncertain whether PP use could be linked to improved clinical outcomes. Therefore, the aim of this paper was to determine PP use status for patients, recognize factors promoting PP use, and further identify the association between PP use and clinical outcome among diabetic patients of different races and ethnicities. Methods This was a single-center cross-section study. Patients were divided into non-Hispanic white (NHW), non-Hispanic black (NHB), and Hispanic/Latino groups. PP use was compared among these three groups. Multivariate logistic regressions were used to determine factors associated with PP use, serum glycemic control, and emergency department (ED) hospitalizations. Results A total of 77,977 patients were analyzed. The rate of PP use among patients of NHW (24%) was higher than those of NHB (19%) and Hispanic/Latinos (18%, P < 0.0001). The adjusted odds ratio (AOR) of insurance coverage associated with PP use was 2.12 (2.02 - 2.23, P < 0.0001), and having a primary care physician (PCP) associated with PP use was 3.89 (3.71 - 4.07, P < 0.0001). In terms of clinical outcomes, the AOR of PP use associated with serum glycemic control was 0.98 (0.90 - 1.05, P = 0.547) and ED hospitalization was 0.79 (0.73 - 0.86, P < 0.0001). Conclusion PP use disparity occurred among NHB and Hispanic/Latino patients in the ED. Having insurance coverage and PCPs seem to correlate with PP use. PP use did not seem to associate with serum glycemic control among DM patients present in the ED but could possibly reduce patient hospitalizations.
COMPARISONS OF G/G/1 QUEUES

A queueuing system (or, shortly, a queue) works as follows: there exist customers which want a service provided by some server. The service time is the time needed by the server to do its job. If a customer comes and there is at least another customer which is served, we say that the system is busy; otherwise, it is free. The discipline of the queue is the rule according to which the customers are served. The simplest is FCFS (First Come, First Served) which is also denoted by some authors by FIFO (First In, First Out). We know the queue when we know the arrival times and the service times. Let us denote by (tn)n≥1 the sequence of the arrival times and by (Sn)n the sequence of the service times. Thus tn is the moment when the n’th customer arrives in line and Sn is the time needed by the server to satisfy him. We can safely assume that the sequence (tn)n is non-decreasing and that Sn > 0 – there is no instantaneous service. We denote such a queuing system by [(Sn)n ; (tn)n] . The time when the nth customer is served will be denoted by τn. Remark that τn = tn + Wn + Sn , (1.1)
Characterization of the velocity anisotropy of accreted globular clusters

Galactic globular clusters (GCs) are believed to have formed in-situ in the Galaxy as well as in dwarf galaxies later accreted onto the Milky Way. However, to date, there is no unambiguous signature to distinguish accreted GCs. Using specifically designed $N$-body simulations of GCs evolving in a variety of time-dependent tidal fields (describing the potential of a dwarf galaxy-Milky Way merger), we analyze the effects imprinted to the internal kinematics of an accreted GC. In particular, we look at the evolution of the velocity anisotropy. Our simulations show that at early phases, the velocity anisotropy is determined by the tidal field of the dwarf galaxy and subsequently the clusters will adapt to the new tidal environment, losing any signature of their original environment in a few relaxation times. At 10 Gyr, GCs exhibit a variety of velocity anisotropy profiles, namely, isotropic velocity distribution in the inner regions and either isotropy or radial/tangential anisotropy in the intermediate and outer regions. Independently of an accreted origin, the velocity anisotropy primarily depends on the strength of the tidal field cumulatively experienced by a cluster. Tangentially anisotropic clusters correspond to systems that have experienced stronger tidal fields and are characterized by higher tidal filling factor, $r_{50}/r_j\gtrsim0.17$, higher mass loss $\gtrsim60\%$ and relaxation times $t_{rel}\lesssim10^9$ Gyr. Interestingly, we demonstrate that the presence of tidal tails can significantly contaminate the measurements of velocity anisotropy when a cluster is observed in projection. Our characterization of the velocity anisotropy profiles in different tidal environments provides a theoretical benchmark for the interpretation of the unprecedented amount of three-dimensional kinematic data progressively available for Galactic GCs.
The Planck Cold Clump G108.37-01.06: A Site of Complex Interplay between H ii Regions, Young Clusters, and Filaments

The Planck Galactic Cold Clumps (PGCCs) are possible representations of the initial conditions and very early stages of star formation. With the objective of understanding better the star and star cluster formation, we probe the molecular cloud associated with PGCC G108.37-01.06 (hereafter PG108.3), which can be traced in a velocity range of −57 to −51 km s−1. The INT Photometric Hα Survey images reveal Hα emission at various locations around PG108.3, and optical spectroscopy of the bright sources in those zones of Hα emission discloses two massive ionizing sources with spectral type O8−O9V and B1V. Using the radio continuum, we estimate ionizing gas parameters and find the dynamical ages of H ii regions associated with the massive stars in the range of 0.5–0.75 Myr. Based on the stellar surface density map constructed from the deep near-infrared Canada–France–Hawaii Telescope observations, we find two prominent star clusters in PG108.3; of these, the cluster associated with H ii region S148 is moderately massive (∼240 M⊙). A careful inspection of James Clerk Maxwell telescope 13CO (3–2) molecular data exhibits that the massive cluster is associated with a number of filamentary structures. Several embedded young stellar objects (YSOs) are also identified in PG108.3 along the length and junction of filaments. We find evidence of a velocity gradient along the length of the filaments. Along with kinematics of the filaments and the distribution of ionized, molecular gas and YSOs, we suggest that the cluster formation is most likely due to the longitudinal collapse of the most massive filament in PG108.3.
Quantum phase transition in a multicomponent anyonic Lieb-Liniger model

We study a one-dimensional multicomponent anyon model that reduces to a multicomponent Lieb-Liniger gas of impenetrable bosons (Tonks-Girardeau gas) for vanishing statistics parameter. At fixed component densities, the coordinate Bethe ansatz gives a family of quantum phase transitions at special values of the statistics parameter. We show that the ground state energy changes extensively between different phases. Special regimes are studied and a general classification for the transition points is given. An interpretation in terms of statistics of composite particles is proposed.
Calabrian Native Project: Botanical Education Applied to Conservation and Valorization of Autochthonous Woody Plants

: Calabria is a floristic hotspot just at the center of Mediterranean Sea. Unfortunately, an increasing number of alien plant species threats this natural heritage, exactly while the crucial role of botany in secondary schools of Italy has been definitely dismantled. Calabrian Native Project is an environmental education project planned by Istituto Tecnico Agrario of Catanzaro that, reintroducing some key concepts of botany and biogeography, allowing pupils to experience a botanical excursion in the close-to-the-school Mediterranean Biodiversity Park, gives them the opportunity to become acquainted with both native and alien species. Pupils are asked to collect native plant propagules and to seed or cultivate the material in the school greenhouses, and to take care of these plants until their use. The prevalent outdoor and laboratory approach to the issue of bioinvasions, make the project very effective. This feature, with the low cost and reduced technology inputs, make the project highly replicable in other contexts, just focusing appropriate target species.
Spatially Resolved 12CO(2–1)/12CO(1–0) in the Starburst Galaxy NGC 253: Assessing Optical Depth to Constrain the Molecular Mass Outflow Rate

We present Atacama Large Millimeter/submillimeter Array (ALMA) observations of 12CO(1–0) and 12CO(2–1) in the central 40″ (680 pc) of the nuclear starburst galaxy NGC 253, including its molecular outflow. We measure the ratio of brightness temperature for CO(2–1)/CO(1–0), r21, in the central starburst and outflow-related features. We discuss how r21 can be used to constrain the optical depth of the CO emission, which impacts the inferred mass of the outflow and consequently the molecular mass outflow rate. We find r21 ≲ 1 throughout, consistent with a majority of the CO emission being optically thick in the outflow, as it is in the starburst. This suggests that the molecular outflow mass is 3–6 times larger than the lower limit reported for optically thin CO emission from warm molecular gas. The implied molecular mass outflow rate is 25–50 M⊙ yr−1, assuming that the conversion factor for the outflowing gas is similar to our best estimates for the bulk of the starburst. This is a factor of 9–19 times larger than the star formation rate in NGC 253. We see tentative evidence for an extended, diffuse CO(2–1) component.
ACTIVE GALACTIC NUCLEUS OBSCURATION THROUGH DUSTY INFRARED-DOMINATED FLOWS. I. RADIATION-HYDRODYNAMICS SOLUTION FOR THE WIND

We construct a radiation-hydrodynamics model for the obscuring toroidal structure in active galactic nuclei. In this model the obscuration is produced at parsec scales by a dense, dusty wind which is supported by infrared radiation pressure on dust grains. To find the distribution of radiation pressure, we numerically solve the two-dimensional radiation transfer problem in a flux-limited diffusion approximation. We iteratively couple the solution with calculations of stationary one-dimensional models for the wind and obtain the z-component of the velocity. Our results demonstrate that for active galactic nucleus (AGN) luminosities greater than 0.1 Ledd, external illumination can support a geometrically thick obscuration via outflows driven by infrared radiation pressure. The terminal velocity of marginally Compton-thin models (0.2 < τT < 0.6) is comparable to or greater than the escape velocity. In Compton-thick models the maximum value of the vertical component of the velocity is lower than the escape velocity, suggesting that a significant part of our torus is in the form of failed wind. The results demonstrate that obscuration via normal or failed infrared-driven winds is a viable option for the AGN torus problem and AGN unification models. Such winds can also provide an important channel for AGN feedback.
STUDENTS’ PERCEPTION OF THE USE OF TED TALK VIDEOS IN PUBLIC SPEAKING CLASSS

TED Talk videos contain speakers discussing the latest thinking about education, learning, innovation, etc. The videos are made as learning media in a public speaking class. This research investigates students’ perceptions of the use of TED Talks video in public speaking class. There were tirty five students contributing as participants of this research. To gain the research data, the researcher used three research instruments: questionnaire, students and lecturer interviews. According to the data analysis, it was found that both the students and lecturer in public speaking have similar perceptions of the use of TED Talk videos. It can be inferred that the use of TED Talk videos can enhance the students’ speaking performance and give new information to them. It is recommended that EFL classes can use TED Talk videos as authentic learning media.