Miracle-dz/UniFAR-FTUs huggingface dataset:
Perturbative stability of the QCD predictions for the ratio $R=F_L/F_T$ and azimuthal asymmetry in heavy-quark leptoproduction

We analyze the perturbative and parametric stability of the QCD predictions for the Callan-Gross ratio R(x,Q2) = FL/FT and azimuthal cos(2φ) asymmetry in heavy-quark leptoproduction. Our analysis shows that large radiative corrections to the structure functions cancel each other in their ratio R(x,Q2) and azimuthal asymmetry with good accuracy. As a result, the NLO contributions to the Callan-Gross ratio and cos(2φ) asymmetry are less than 10% in a wide region of the variables x and Q2. We provide compact analytic predictions for R(x,Q2) and asymmetry in the case of low x≪ 1. Simple formulae connecting the high-energy behavior of the Callan-Gross ratio and azimuthal asymmetry with the low-x asymptotics of the gluon density in the target are derived. It is shown that the obtained hadron-level predictions for R(x,Q2) and azimuthal asymmetry are stable at x≪ 1 under the DGLAP evolution of the gluon distribution function.
The Determinants of Digital Workplace Adoption: A Conceptual Framework

Vol. No. 2022, Pg. 477 492 Abstract The digital workplace is an invaluable organizational resource that can significantly boost the productivity of knowledge workers. The reduction of barriers between people, information, and processes is one of the many benefits offered digital workplace, along with mobility, information searching, communication, and collaboration. However, the Movement Control Order caused commercial losses for more than two thirds of Malaysian SMEs (MCO). 31% of SMEs suffered delays in finishing tasks and projects, while 30% had operational interruptions. From a thorough analysis of the literature on digital workplace adoption adoption, this study presents a conceptual framework to determine the factors that influence digital workplace adoption. The conceptual framework which is based on Unified Theory of Technology Acceptance and Use (UTAUT) will be applied in this study. The proposed framework can be utilized to identify the determinant factors of digital workplace adoption among employees of Malaysian SMEs. In the meantime, Personal Knowledge Management is integrated to the framework serves as a moderator to assess worker's ability in using digital workplace tools.
EVALUATION OF BONE AUGMENTATION UNDER PERFORATED AND NON PERFORATED CERAMIC SPACE MAINTAINING DEVICE (EXPERIMENTAL STUDY)

INTRODUCTION: Alveolar bone deficiency is one of most common problems encountered with oral rehabilitation. Many bone augmentation techniques have been documented, one of them is augmentation by bone grafting and barrier membranes, ceramic membrane proved efficiency in guided bone regeneration due to enhanced properties. AIM OF THIS STUDY: Evaluation of bone surface area under perforated ceramic membrane in relation to non perforated ceramic membrane. MATERIALS AND METHODS: 14 mongrel dogs divided into two equal groups, study group used bone graft, cortical perforation and perforated ceramic membrane, control group used bone graft, cortical perforation and non perforated ceramic membrane, follow up for 12 weeks and sacrification was done retrieving ceramic mebrane with samples of new bone which histologically prepared for histomorphometric analysis. Results: By histological evaluation more cellularity and vascularity, better trabecular arrangement and lesser granulation tissues were noted under perfor ated ceramic group. By histomorphometric analysis statistically significant at p ≤ 0.05 and higher bone surface area with mean value of 40.09 ± 3.50 associated with perforated group in comparison with mean value of 19.92 ± 3.63 associated with non perforated ceramic membrane group. CONCLUSION: Perforated ceramic membrane is comparable to occlusive one in terms of higher bone surface area, reduced granulation tissues and favorable blood supply.
Drag reduction strategies

previously a description was given of an active control scheme using wall transpiration that leads to a 15% reduction in surface skin friction beneath a turbulent boundary layer, according to direct numerical simulation. In this research brief further details of that scheme and its variants are given together with some suggestions as to how sensor/actuator arrays could be configured to reduce surface drag. The research which is summarized here was performed during the first half of 1994. This research is motivated by the need to understand better how the dynamics of near-wall turbulent flow can be modified so that skin friction is reduced. The reduction of turbulent skin friction is highly desirable in many engineering applications. Experiments and direct numerical simulations have led to an increased understanding of the cycle of turbulence production and transport in the boundary layer and raised awareness of the possibility of disrupting the process with a subsequent reduction in turbulent skin friction. The implementation of active feedback control in a computational setting is a viable approach for the investigation of the modifications to the flow physics that can be achieved. Bewley et al. and Hill describe how ideas from optimal control theory are employed to give 'sub-optimal' drag reduction schemes. The objectives of the work reported here is to investigate in greater detail the assumptions implicit within such schemes and their limitations. It is also our objective to describe how an array of sensors and actuators could be arranged and interconnected to form a 'smart' surface which has low skin friction.
Spin excitations in a model of FeSe with orbital ordering

We present a theoretical study of the dynamical spin susceptibility for the intriguing Fe-based superconductor FeSe, based on a tight-binding model developed to account for the temperature-dependent band structure in this system. The model allows for orbital ordering in the $d_{xz}/d_{yz}$ channel below the structural transition and presents a strongly $C_4$ symmetry broken Fermi surface at low temperatures which accounts for the nematic properties of this material. The calculated spin excitations are peaked at wave vector $(\pi,0)$ in the 1-Fe Brillouin zone, with a broad maximum at energies of order a few meV. In this range, the occurrence of superconductivity sharpens this peak in energy, creating a $(\pi,0)$ "neutron resonance" as seen in recent experiments. With the exception of the quite low energy scale of these fluctuations, these results are roughly similar to standard behavior in Fe pnictide systems. At higher energies, however, intensity increases and shifts to wave vectors along the $(\pi,0)$ - $(\pi,\pi)$ line. We compare with existing inelastic neutron experiments and NMR data, and give predictions for further studies.
Response of Plant Immunity Markers to Early and Late Application of Extracellular DNA from Different Sources in Tomato (Solanum lycopersicum)

As a recently explored agricultural practice, the controlled elicitation of plants offers high potential in multiple crop needs as growth promotion, activation of defenses and the production of specific metabolites. Extracellular DNA has been identified as a plant immune system elicitor but some aspects of the plant response have not been explored. In the present work, five DNA treatments were applied in tomato plants and the response of catalase, superoxide dismutase, phenylalanine ammonia lyase activities, hydrogen peroxide, total phenolics and flavonoid contents in leaves were spectrophotometrically measured. Treatments differed by the source and concentration of DNA and plant phenological stage of application. Furthermore, mathematical modeling and principal component analysis were performed to explore the behavior of each variable and their interaction. The most effective treatment was the self-DNA application in young plants based on the intensity and duration of immune system activation. The information given by the measured variables correlated positively with the phenylpropanoid pathway markers and negatively with catalase and superoxide dismutase activities. Results reported here propose an easy way to evaluate plant immune response activation by DNA and any other elicitor and provide useful information for future development of controlled elicitation strategies in crop production.
FROM EXOPLANETS TO QUASARS: DETECTION OF POTENTIAL DAMPED Lyα ABSORBING GALAXIES USING ANGULAR DIFFERENTIAL IMAGING

The advantages of angular differential imaging (ADI) have been previously untested in imaging the host galaxies of damped Lyα (DLA) systems. In this pilot study, we present the first application of ADI to directly image the host galaxy of the DLA seen toward the quasar J1431+3952. K-band imaging of the field surrounding J1431+3952 was obtained on the Gemini North telescope with an adaptive optics system and a laser guide star. We computed a sensitivity curve that demonstrates the sensitivity of our observations as a function of K-band magnitude, impact parameter and DLA angular size. For an impact parameter of 0. ″5 (3.4 kpc at the redshift of the absorber) our mass sensitivity is log (M /M 9.2 and drops to ∼9.0 at separations beyond ∼6 kpc for the smallest size model galaxy. Three candidate galaxies are identified within 5″. Stellar masses were computed from the K-band photometry yielding values of log (M /M 9.9, 9.7 and 11.1 respectively. The likely identification of the absorbing galaxy is discussed, and we conclude that the galaxy with the largest impact parameter and highest stellar mass is unlikely to be the host, based on its inconsistency with the N(HI) impact parameter relation and inconsistent photometric redshift. While we cannot distinguish between the remaining two candidates as the DLA host, we note that, despite the low spin temperature and relatively high metallicity of the DLA, the host does not appear to be a particularly luminous (high-mass) galaxy.
Promising Observational Methods for Detecting the Epoch of Reionization

It has been several years since the first detection of Gunn-Peterson troughs in the z > 6 Ly-alpha forest and since the first measurement of the Thomson scattering optical depth through reionization from the cosmic microwave background (CMB). Present day CMB measurements provide a significant constraint on the mean redshift of reionization, and the Ly-alpha forest provides a lower bound on the redshift at which reionization ended. However, no observation has provided definitive information on the duration and morphology of this process. This article is intended as a short review on the most promising observational methods that aim to detect and study this cosmic phase transition, focusing on CMB anisotropies, gamma ray burst afterglows, Ly-alpha emitting galaxies, and redshifted 21cm emission.
ROCKY EXTRASOLAR PLANETARY COMPOSITIONS DERIVED FROM EXTERNALLY POLLUTED WHITE DWARFS

We report Keck High Resolution Echelle Spectrometer data and model atmosphere analysis of two helium-dominated white dwarfs, PG1225−079 and HS2253+8023, whose heavy pollutions most likely derive from the accretion of terrestrial-type planet(esimal)s. For each system, the minimum accreted mass is ∼1022 g, that of a large asteroid. In PG1225−079, Mg, Cr, Mn, Fe, and Ni have abundance ratios similar to bulk Earth values, while we measure four refractory elements, Ca, Sc, Ti, and V, all at a factor of ∼2–3 higher abundance than in the bulk Earth. For HS2253+8023 the swallowed material was compositionally similar to bulk Earth in being more than 85% by mass in the major element species, O, Mg, Si, and Fe, and with abundances in the distinctive proportions of mineral oxides—compelling evidence for an origin in a rocky parent body. Including previous studies we now know of four heavily polluted white dwarfs where the measured oxygen and hydrogen are consistent with the view that the parents' bodies formed with little ice, interior to any snow line in their nebular environments. The growing handful of polluted white dwarf systems with comprehensive abundance measurements form a baseline for characterizing rocky exoplanet compositions that can be compared with bulk Earth.
The habitat of early life:

Solar X-ray and UV radiation (0.1-320 nm) received at Earth’s surface is an important aspect of the circumstances under which life formed on Earth. The quantity that is received depends on two main variables: the emission of radiation by the young Sun and its extinction through absorption and scattering by the Earth’s early atmosphere. The spectrum emitted by the Sun when life formed, between 4 and 3.5 Ga, was modeled here, including the effects of flares and activity cycles, using a solar-like star that has the same age now as the Sun had 4-3.5 Ga. Atmospheric extinction was calculated using the Beer-Lambert law, assuming several density profiles for the atmosphere of the Archean Earth. We found that almost all radiation with a wavelength shorter than 200 nm is attenuated effectively, even by very tenuous atmospheres. Longer wavelength radiation is progressively less well attenuated, and its extinction is more sensitive to atmospheric composition. Minor atmospheric components, such as methane, ozone, water vapor, etc., have only negligible effects, but changes in CO2 concentration can cause large differences in surface flux. Differences due to variability in solar emission are small compared to this. In all cases surface radiation levels on the Archean Earth were several orders of magnitude higher in the 200-300 nm wavelength range than current levels in this range. That means that any form of life that might have been present at Earth’s surface 4-3.5 Ga, must have been exposed to much higher quantities of damaging radiation than at present.
EVIDENCE FOR WIDESPREAD COOLING IN AN ACTIVE REGION OBSERVED WITH THE SDO ATMOSPHERIC IMAGING ASSEMBLY

A well-known behavior of EUV light curves of discrete coronal loops is that the peak intensities of cooler channels or spectral lines are reached at progressively later times than hotter channels. This time lag is understood to be the result of hot coronal loop plasma cooling through these lower respective temperatures. However, loops typically comprise only a minority of the total emission in active regions (ARs). Is this cooling pattern a common property of AR coronal plasma, or does it only occur in unique circumstances, locations, and times? The new Solar Dynamics Observatory/Atmospheric Imaging Assembly (SDO/AIA) data provide a wonderful opportunity to answer this question systematically for an entire AR. We measure the time lag between pairs of SDO/AIA EUV channels using 24 hr of images of AR 11082 observed on 2010 June 19. We find that there is a time-lag signal consistent with cooling plasma, just as is usually found for loops, throughout the AR including the diffuse emission between loops for the entire 24 hr duration. The pattern persists consistently for all channel pairs and choice of window length within the 24 hr time period, giving us confidence that the plasma is cooling from temperatures of greater than 3 MK, and sometimes exceeding 7 MK, down to temperatures lower than ∼0.8 MK. This suggests that the bulk of the emitting coronal plasma in this AR is not steady; rather, it is dynamic and constantly evolving. These measurements provide crucial constraints on any model which seeks to describe coronal heating.
Characteristics of polar coronal hole jets

High spatial- and temporal-resolution images of coronal hole regions show a dynamical environment where mass flows and jets are frequently observed. These jets are believed to be important for the coronal heating and the acceleration of the fast solar wind. We studied the dynamics of two jets seen in a polar coronal hole with a combination of imaging from EIS and XRT onboard Hinode. We observed drift motions related to the evolution and formation of these small-scale jets, which we tried to model as well. We found observational evidence that supports the idea that polar jets are very likely produced by multiple small-scale reconnections occurring at different times in different locations. These eject plasma blobs that flow up and down with a motion very similar to a simple ballistic motion. The associated drift speed of the first jet is estimated to be $\approx$ 27 km s$^{-1}$. The average outward speed of the first jet is $\approx 171$ km s$^{-1}$, well below the escape speed, hence if simple ballistic motion is considered, the plasma will not escape the Sun. The second jet was observed in the south polar coronal hole with three XRT filters, namely, C$_{-}$poly, Al$_{-}$poly, and Al$_{-}$mesh filters. We observed that the second jet drifted at all altitudes along the jet with the same drift speed of $\simeq$ 7 km s$^{-1}$. The enhancement in the light curves of low-temperature EIS lines in the later phase of the jet lifetime and the shape of the jet's stack plots suggests that the jet material is falls back, and most likely cools down. To support this conclusion, the observed drifts were interpreted within a scenario where reconnection progressively shifts along a magnetic structure, leading to the sequential appearance of jets of about the same size and physical characteristics. On this basis, we also propose a simple qualitative model that mimics the observations.
K. Nadda and M. J. Kumar, “Schottky Collector Bipolar Transistor without Impurity Doped Emitter and Base: Design

In this paper, we report an alternative approach of implementing a Schottky collector bipolar transistor without doping the ultrathin SOI film. Using different metal work function electrodes, the electrons and holes are induced in an intrinsic silicon film to create the “n” emitter and the “p” base regions, respectively. Using two-dimensional device simulation, the performance of the proposed device has been evaluated. Our results demonstrate that the charge plasma based bipolar transistor with Schottky collector exhibits a high current gain and a better cut-off frequency compared to its conventional counterpart.
Discovery of VHE gamma-ray emission from the BL Lac object B3 2247+381 with the MAGIC telescopes

Aims. We study the non-thermal jet emission of the BL Lac object B3 2247+381 during a high optical state. Methods. The MAGIC telescopes observed the source during 13 nights between September 30th and October 30th 2010, collecting a total of 14.2 hours of good quality very high energy (VHE) -ray data. Simultaneous multiwavelength data was obtained with X-ray observations by the Swift satellite and optical R-band observations at the KVA-telescope. We also use high energy -ray (HE, 0.1 GeV‐100 GeV) data from the Fermi satellite. Results. The BL Lac object B3 2247+381 (z=0.119) was detected, for the first time, at VHE -rays at a statistical significance of 5.6 �. A soft VHE spectrum with a photon index of -3.2± 0.6 was determined. No significant short term flux variations were found. We model the spectral energy distribution using a one-zone SSC-model, which can successfully describe our data.
Comparison of an approximately isothermal gravitational potentials of elliptical galaxies based on X-ray and optical data

We analyze six X-ray bright elliptical galaxies, observed with Chandra and XMMNewton, and approximate their gravitational potentials by isothermal spheres φ = v 2 c log r over a range of radii from ∼0.5 to ∼ 25 kpc. We then compare the circular speed vc derived from X-ray data with the estimators available from optical data. In particular we discuss two simple and robust procedures for evaluating the circular speed of the galaxy using the observed optical surface brightness and the line-ofsight velocity dispersion profiles. The best fitting relation between the circular speeds derived from optical observations of stars and X-ray observations of hot gas is vc,opt ≃ η vc,X , where η = 1.10 − 1.15 (depending on the method), suggesting, albeit with large statistical and systematic uncertainties, that non-thermal pressure on average contributes ∼20-30% of the gas thermal pressure.
THE DISK-OUTFLOW SYSTEM IN THE S255IR AREA OF HIGH-MASS STAR FORMATION

We report the results of our observations of the S255IR area with the Submillimeter Array (SMA) at 1.3 mm in the very extended configuration and at 0.8 mm in the compact configuration as well as with the IRAM 30 m at 0.8 mm. The best achieved angular resolution is about 0.4 arcsec. The dust continuum emission and several tens of molecular spectral lines are observed. The majority of the lines is detected only toward the S255IR-SMA1 clump, which represents a rotating structure (probably a disk) around the young massive star. The achieved angular resolution is still insufficient to make any conclusions about the Keplerian or non-Keplerian character of the rotation. The temperature of the molecular gas reaches 130–180 K. The size of the clump is about 500 AU. The clump is strongly fragmented as follows from the low beam-filling factor. The mass of the hot gas is significantly lower than the mass of the central star. A strong DCN emission near the center of the hot core most probably indicates a presence of a relatively cold (≲80 K) and rather massive clump there. High-velocity emission is observed in the CO line as well as in lines of high-density tracers HCN, HCO+, CS and other molecules. The outflow morphology obtained from a combination of the SMA and IRAM 30 m data is significantly different from that derived from the SMA data alone. The CO emission detected with the SMA traces only one boundary of the outflow. The outflow is most probably driven by jet bow shocks created by episodic ejections from the center. We detected a dense high velocity clump associated apparently with one of the bow shocks. The outflow strongly affects the chemical composition of the surrounding medium.
AN INDUCTION PROBE FOR SIMULTANEOUS MEASUREMENTS OF PERMITTIVITY AND RESISTIVITY PROGETTAZIONE DI UNA SONDA AD INDUZIONE PER MISURE SIMULATANEE DI PERMITTIVITÁ E RESISITIVITÁ (Short Title-Titolo Abbreviato: RESPER PROBE)

220 221 222 223 224 225 226 227 228 229 230 231 232 233 234 235 236 237 238 239 240 241 242 243 244 245 In this paper, we propose a discussion of the theoretical design and move towards the development and engineering of an induction probe for electrical spectroscopy which performs simultaneous and non invasive measurements on the electrical RESistivity ρ and dielectric PERmittivity εr of non-saturated terrestrial ground and concretes (RESPER probe). In order to design a RESPER which measures ρ and εr with inaccuracies below a prefixed limit (10%) in a band of low frequencies (LF) (B=100kHz), the probe should be connected to an appropriate analogical digital converter (ADC), which samples in uniform or in phase and quadrature (IQ) mode, otherwise to a lock-in amplifier. The paper develops only a suitable number of numerical simulations, using Mathcad, which provide the working frequencies, the electrode-electrode distance and the optimization of the height above ground minimizing the inaccuracies of the RESPER, in galvanic or capacitive contact with terrestrial soils or concretes, of low or high resistivity. As findings of simulations, we underline that the performances of a lock-in amplifier are preferable even when compared to an IQ sampling ADC with high resolution, under the same operating conditions. As consequences in the practical applications: if the probe is connected to a data acquisition system (DAS) as an uniform or an IQ sampler, then it could be commercialized for companies of building and road paving, being employable for analyzing “in situ” only concretes; otherwise, if the DAS is a lock-in amplifier, the marketing would be for companies of geophysical prospecting, involved to analyze “in situ” even terrestrial soils.