Miracle-dz/UniFAR-FTUs huggingface dataset:
Effect of NPK levels and city compost on soil chemical and biological properties, yield and quality of wheat ( Triticum aestivum L.) under system of wheat intensification (SWI)

A field experiment was conducted on medium black calcareous soil at Junagadh (Gujarat) during rabi season of 2019-20 to study the effect of NPK levels and city compost on soil chemical and biological properties, yield and quality of wheat ( Triticum aestivum L.) under and system of wheat intensification (SWI). Total twelve treatment combinations, consisting of three system of sowing (S 1 : normal practice at 22.5 cm, S 2 : SWI at 20 cm × 20 cm and S 3 : SWI at 25 cm × 25 cm) were assigned to main plot and four fertility levels (F 1 : city compost 10 t/ha, F 2 : 50% RDF + city compost 5 t/ha, F 3 : 75% RDF + city compost 5 t/ha and F 4 : 100% RDF) were allotted to sub plots in a split plot design with three replications. The results revealed that sowing of wheat under SWI recorded significantly higher values of protein yield (562.63 kg/ha) and total fungal, bacterial as well as Azotobacter count in soil. SWI at 20 cm × 20 cm produced significantly maximum grain yield (5070 kg/ha) and straw yield (8289 kg/ha). Application of 75% RDF (90-45-45 kg N- P 2 O 5 - K 2 O/ha) + city compost 5 t/ha enhanced almost all the quality parameters viz . , protein, gluten and fiber content in grain, protein yield, available N, P and K as well as organic carbon content in soil after harvest and soil microbial population viz., total fungal, bacterial, actinomycetes, Azotobacter , PSB and KSB count in soil, and resultantly gave higher grain yield (5975 kg/ha) and straw yield (8344 kg/ha).
MAGNETOACOUSTIC WAVE ENERGY FROM NUMERICAL SIMULATIONS OF AN OBSERVED SUNSPOT UMBRA

We aim at reproducing the height dependence of sunspot wave signatures obtained from spectropolarimetric observations through three-dimensional MHD numerical simulations. A magnetostatic sunspot model based on the properties of the observed sunspot is constructed and perturbed at the photosphere, introducing the fluctuations measured with the Si i λ10827 line. The results of the simulations are compared with the oscillations observed simultaneously at different heights from the He i λ10830 line, the Ca ii H core, and the Fe i blends in the wings of the Ca ii H line. The simulations show a remarkable agreement with the observations. They reproduce the velocity maps and power spectra at the formation heights of the observed lines, as well as the phase and amplification spectra between several pairs of lines. We find that the stronger shocks at the chromosphere are accompanied with a delay between the observed signal and the simulated one at the corresponding height, indicating that shocks shift the formation height of the chromospheric lines to higher layers. Since the simulated wave propagation matches very well the properties of the observed one, we are able to use the numerical calculations to quantify the energy contribution of the magnetoacoustic waves to the chromospheric heating in sunspots. Our findings indicate that the energy supplied by these waves is too low to balance the chromospheric radiative losses. The energy contained at the formation height of the lowermost Si i λ10827 line in the form of slow magnetoacoustic waves is already insufficient to heat the higher layers, and the acoustic energy which reaches the chromosphere is around 3–9 times lower than the required amount of energy. The contribution of the magnetic energy is even lower.
Reflection Removal With NIR and RGB Image Feature Fusion

Removing undesirable reflections in photographs benefits both human perceptions and downstream computer vision tasks, but it is a highly ill-posed problem based on a single RGB image. Different from RGB images, near-infrared (NIR) images captured by an active NIR camera are less likely to be affected by reflections when glass and camera planes form certain angles, while textures on objects could “vanish” in some situations. Based on this observation, we propose a cascaded reflection removal network with an image feature fusion strategy to utilize auxiliary information in active NIR images. To tackle the insufficiency of training data, we propose a data generation pipeline to approximate perceptual properties and the reflection-suppressing nature of active NIR images. We further build a dataset with synthetic and real images to facilitate the research. Experimental results show that the proposed method outperforms state-of-the-art reflection removal methods in both quantitative metrics and visual quality.
Fermi surface in KFe2As2determined via de Haas–van Alphen oscillation measurements

We have completely determined the Fermi surface in KFe$_2$As$_2$ via de Haas-van Alphen (dHvA) measurements. Fundamental frequencies $\epsilon$, $\alpha$, $\zeta$, and $\beta$ are observed in KFe$_2$As$_2$. The first one is attributed to a hole cylinder near the X point of the Brillouin zone, while the others to hole cylinders at the $\Gamma$ point. We also observe magnetic breakdown frequencies between $\alpha$ and $\zeta$ and suggest a plausible explanation for them. The experimental frequencies show deviations from frequencies predicted by band structure calculations. Large effective masses up to 19 $m_e$ for $B \parallel c$ have been found, $m_e$ being the free electron mass. The carrier number and Sommerfeld coefficient of the specific heat are estimated to be 1.01 -- 1.03 holes per formula unit and 82 -- 94 mJmol$^{-1}$K$^{-2}$, respectively, which are consistent with the chemical stoichiometry and a direct measure of 93 mJmol$^{-1}$K$^{-2}$ [H. Fukazawa \textit{et al}. , J. Phys. Soc. Jpn. \textbf{80SA}, SA118 (2011)]. The Sommerfeld coefficient is about 9 times enhanced over a band value, suggesting the importance of low-energy spin and/or orbital fluctuations, and places KFe$_2$As$_2$ among strongly correlated metals. We have also performed dHvA measurements on Ba$_{0.07}$K$_{0.93}$Fe$_2$As$_2$ and have observed the $\alpha$ and $\beta$ frequencies.
Growth performance , carcass composition , and immunophysiological indices in juvenile great sturgeon ( Huso huso ) fed on commercial prebiotic

Growth performance, carcass composition, and immunophysiological indices in juvenile great sturgeon (Huso huso) fed on commercial prebiotic Immunoster (IS) were investigated. After a four-week acclimatization period, 270 great sturgeon juveniles weighing 95.68 ± 10.05 g were randomly distributed into 9 fiberglass tanks in three replicates and kept at a density of 30 fish per tank for a period of 8 weeks at water temperature 20.55 ± 5.11C and dissolved oxygen 6.73 ± 0.35 mg L -1 . IS was added at two levels of 1% and 3% to the basal diet in place of cellulose. At the end of the trial, blood sampling and carcass analysis were conducted. Weight, length, body weight increase (BWI), specific growth rate (SGR), feed conversion ratio (FCR), protein efficiency ratio (PER) and condition factor (CF) were significantly affected by IS 3% compared with IS 1% and the control (P<0.05). There was significant difference (P<0.05) in crude protein of carcass between the experimental groups. Mean corpuscular volume (MCV) and mean corpuscular hemoglobin (MCH) showed significantly higher levels in experimental treatments compared with the control (P<0.05). Immunoglobulin M (IgM) level and lysozyme activity in IS 1% group were higher than the control group. It can be concluded that IS can enhance growth performance and improve some immunophysiological indices of great sturgeon.
SUPERORBITAL PHASE-RESOLVED ANALYSIS OF SMC X-1

The high-mass X-ray binary SMC X-1 is an eclipsing binary with an orbital period of 3.89 days. This system exhibits a superorbital modulation with a period varying between ∼40 days and ∼65 days. The instantaneous frequency and the corresponding phase of the superorbital modulation can be obtained by a recently developed time–frequency analysis technique, the Hilbert–Huang transform (HHT). We present a phase-resolved analysis of both the spectra and the orbital profiles with the superorbital phase derived from the HHT. The X-ray spectra observed by the Proportional Counter Array on board the Rossi X-ray Timing Explorer are fitted well by a blackbody plus a Comptonized component. The plasma optical depth, which is a good indicator of the distribution of material along the line of sight, is significantly anti-correlated with the flux detected at 2.5–25 keV. However, the relationship between the plasma optical depth and the equivalent width of the iron line is not monotonic. There is no significant correlation for fluxes higher than ∼35 mCrab but clear positive correlation when the intensity is lower than ∼20 mCrab. This indicates that the iron line production is dominated by different regions of this binary system in different superorbital phases. To study the dependence of the orbital profile on the superorbital phase, we obtained the eclipse profiles by folding the All Sky Monitor light curve with the orbital period for different superorbital states. A dip feature, similar to the pre-eclipse dip in Her X-1, lying at orbital phase ∼0.6–0.85, was discovered during the superorbital transition state. This indicates that the accretion disk has a bulge that absorbs considerable X-ray emission in the stream–disk interaction region. The dip width is anti-correlated with the flux, and this relation can be interpreted by the precessing tilted accretion disk scenario.
Clinical Outcomes of Transplanted Kidneys from Deceased Donors Using Different Generic Preservation Solutions

Background and Objectives: StoreProtect Plus® is a preserving solution for cold organ storage, with a composition identical to Institute Georges Lopez (IGL-1) solution. The aim of this single center study was to compare the clinical performance of StoreProtect Plus with the generic counterpart of University of Wisconsin preservation fluid, named SPS-1®. Materials and Methods: The clinical outcomes of 168 consecutive organs preserved with StoreProtect Plus solution and 167 organs preserved with SPS-1 solution were compared. During an 18-month post-transplant follow-up period, kidney graft function, the frequency of acute rejection, post-transplant diabetes, and infectious complications, as well as patient and graft survival were analyzed. Results: There was significantly more immediate graft function (IGF) (39.3 vs. 24.0%; p < 0.01) and less slow graft function (SGF) (38.7 vs. 51.5%; p < 0.05) in the StoreProtect Plus group in comparison with the SPS-1 group, whereas the occurrence of DGF was similar in both groups. Long-term kidney graft function was comparable. Multivariate regression analysis showed that the use of StoreProtect Plus vs. SPS-1 solution (rpartial = 0.217; p < 0.001) and the amount of residual diuresis (rpartial = 0.147; p < 0.001) independently increased the occurrence of IGF, whereas Scr > 1.5 mg/dL prior to organ procurement (rpartial = −0.198; p < 0.001), longer CIT (rpartial = −0.170; p < 0.01), and CVD donor death (rpartial = −0.214; p < 0.001) were associated with SGF. Conclusions: The higher occurrence of IGF was found in kidney transplant recipients whose organs were preserved using StoreProtect Plus solution as compared with SPS-1 solution. The two groups did not differ in kidney graft function, the frequency of post-transplant complications, as well as patient and graft survival.
Generation of Functional Immortalized Human Corneal Stromal Stem Cells

In addition to their therapeutic potential in regenerative medicine, human corneal stromal stem cells (CSSCs) could serve as a powerful tool for drug discovery and development. Variations from different donors, their isolation method, and their limited life span in culture hinder the utility of primary human CSSCs. To address these limitations, this study aims to establish and characterize immortalized CSSC lines (imCSSC) generated from primary human CSSCs. Primary CSSCs (pCSSC), isolated from human adult corneoscleral tissue, were transduced with ectopic expression of hTERT, c-MYC, or the large T antigen of the Simian virus 40 (SV40T) to generate imCSSC. Cellular morphology, proliferation capacity, and expression of CSSCs specific surface markers were investigated in all cell lines, including TNFAIP6 gene expression levels in vitro, a known biomarker of in vivo anti-inflammatory efficacy. SV40T-overexpressing imCSSC successfully extended the lifespan of pCSSC while retaining a similar morphology, proliferative capacity, multilineage differentiation potential, and anti-inflammatory properties. The current study serves as a proof-of-concept that immortalization of CSSCs could enable a large-scale source of CSSC for use in regenerative medicine.
Reconstructing WIMP properties through an interplay of signal measurements in direct detection, Fermi-LAT, and CTA searches for dark matter

We examine the projected ability to reconstruct the mass, scattering, and annihilation cross section of dark matter in the new generation of large underground detectors, XENON-1T, SuperCDMS, and DarkSide-G2, in combination with diffuse gamma radiation from expected 15 years of data from Fermi-LAT observation of 46 local spiral dwarf galaxies and projected CTA sensitivity to a signal from the Galactic Center. To this end we consider several benchmark points spanning a wide range of WIMP mass, different annihilation final states, and large enough event rates to warrant detection in one or more experiments. As previously shown, below some 100 GeV only direct detection experiments will in principle be able to reconstruct WIMP mass well. This may, in case a signal at Fermi-LAT is also detected, additionally help restricting σv and the allowed decay branching rates. In the intermediate range between some 100 GeV and up a few hundred GeV, direct and indirect detection experiments can be used in complementarity to ameliorate the respective determinations, which in individual experiments can at best be rather poor, thus making the WIMP reconstruction in this mass range very challenging. At large WIMP mass, ∼ 1 TeV, CTA will have the ability to reconstruct mass, annihilation cross section, and the allowed decay branching rates to very good precision for the τ+τ− or purely leptonic final state, good for the W+W− case, and rather poor for bb̄. A substantial improvement can potentially be achieved by reducing the systematic uncertainties, increasing exposure, or by an additional measurement at Fermi-LAT that would help reconstruct the annihilation cross section and the allowed branching fractions to different final states.
An ultraviolet study of B[e] stars: evidence for pulsations, luminous blue variable type variations and processes in envelopes

Stars that exhibit a B[e] phenomenon comprise a very diverse group of objects in a different evolutionary status. These objects show common spectral characteristics, including the presence of Balmer lines in emission, forbidden lines and strong infrared excess due to dust. Observations of emission lines indicate illumination by an ultraviolet ionizing source, which is key to understanding the elusive nature of these objects. We study the ultraviolet variability of many B[e] stars to specify the geometry of the circumstellar environment and its variability. We analyse massive hot B[e] stars from our Galaxy and from the Magellanic Clouds. We study the ultraviolet broad-band variability derived from the flux-calibrated data. We determine variations of individual lines and the correlation with the total flux variability. We detected variability of the spectral energy distribution and of the line profiles. The variability has several sources of origin, including light absorption by the disc, pulsations, luminous blue variable type variations, and eclipses in the case of binaries. The stellar radiation of most of B[e] stars is heavily obscured by circumstellar material. This suggests that the circumstellar material is present not only in the disc but also above its plane. The flux and line variability is consistent with a two-component model of a circumstellar environment composed of a dense disc and an ionized envelope. Observations of B[e] supergiants show that many of these stars have nearly the same luminosity, about 1.9 x 10^5 Lo, and similar effective temperatures.
Sensitivities to charged-current nonstandard neutrino interactions at DUNE

We investigate the effects of charged-current (CC) nonstandard neutrino interactions (NSIs) at the source and at the detector in the simulated data for the planned Deep Underground Neutrino Experiment (DUNE), while neglecting the neutral-current NSIs at the propagation due to the fact that several solutions have been proposed to resolve the degeneracies posed by neutral-current NSIs while no solution exists for the degeneracies due to the CC NSIs. We study the effects of CC NSIs on the simultaneous measurements of $\theta_{23}$ and $\delta_{CP}$ in DUNE. The analysis reveals that 3$\sigma $ C.L. measurement of the correct octant of $\theta_{23}$ in the standard mixing scenario is spoiled if the CC NSIs are taken into account. Likewise, the CC NSIs can deteriorate the uncertainty of the $\delta_{CP}$ measurement by a factor of two relative to that in the standard oscillation scenario. We also show that the source and the detector CC NSIs can induce a significant amount of fake CP-violation and the CP-conserving case can be excluded by more than 80\% C.L. in the presence of fake CP-violation. We further find the potential of DUNE to constrain the relevant CC NSI parameters from the single parameter fits for both neutrino and antineutrino appearance and disappearance channels at both the near and far detectors. The results show that there could be improvement in the current bounds by at least one order of magnitude at the near and far detector of DUNE except a few parameters which remain weaker at the far detector.
ESO 243-49 HLX-1: scaling of X-ray spectral properties and black hole mass determination

We report the results of Swift/XRT observations (2008-2015) of a hyper-luminous X-ray source, ESO 243-49 HLX-1. We found a strong observational evidence that ESO 243-49 HLX-1 underwent spectral transitions from the low/hard state to the high/soft state during these observations. The spectra of ESO 243-49 HLX-1 are well fitted by the so-{called} bulk motion Comptonization model for all spectral states. We have established the photon index Gamma saturation level, Gamma_{sat}$=3.0+/-0.1, in the correlation of Gamma versus mass accretion rate dot M. This Gamma-dot M correlation allows us to estimate the black hole (BH) mass in ESO 243-49 HLX-1 to be M_{BH}~ 7x 10^4 solar masses, assuming the distance to ESO 243-49 of 95 Mpc. For the BH mass estimate we used the scaling method, taking Galactic BHs XTE~J1550-564, H~1743-322 and 4U~1630-472, and an extragalactic BH source, M101 ULX-1 as reference sources. The Gamma-dot M correlation revealed in ESO 243-49 HLX-1 is similar to those in a number of Galactic and extragalactic BHs and it clearly shows the correlation along with the strong Gamma saturation at ~ 3. This is a reliable observational evidence of a BH in ESO 243-49 HLX-1. We also found that the seed (disk) photon temperatures are quite low, of order of 50-140 eV which are consistent with a high BH mass in ESO 243-49 HLX-1.
Dynamical Organization around Turbulent Bursts

It is well-known from experiments and numerical simulations that intermittency in turbulent flows produces corrections both to the classical Kolmogorov —5/3 scaling law of the energy spectrum but also for other moments in the inertial range [1, 2]. Still very little is known about the structure of the intermittent bursts which arise in turbulent flows. This work presents an analysis of the intermittent bursts in the turbulent GOY shell model, inspired by work of Dombre and Gilson [3]. Shell models are formed by various truncation techniques of the Naiver-Stokes equations and have become paradigm models for the study of turbulence at very high Reynolds numbers [4, 5, 6, 7, 8, 9, 10]. In the GOY model wave-number space is divided it into N separate shells with characteristic wavenumber k n ~ λ n (λ = 2) where n = 1, …, N. Each shell is assigned a complex amplitude u n which can be imagined as the velocity gradient on a scale l n = 1/k n . By assuming conservation of phase space, energy and helicity and interactions among the nearest and next nearest neighbor shells, one arrives at the following evolution equations [6, 8, 9] $$ \left( {\frac{d}{{dt}} + vk_n^2} \right){u_n} = i{k_n}\left( {u_{n + 1}^*u_{n + 2}^* - \frac{1}{4}u_{n - 1}^*u_{n + 1}^* - \frac{1}{8}u_{n - 2}^*u_{n - 1}^*} \right) + f{\delta _{n,4}} $$ (1)
Sinking Satellites and Tilting Disk Galaxies

We perform fully self-consistent N-body simulations of a system of disk, halo, and satellite to investigate three different dynamical responses of a disk to an infalling satellite: tilting, warping, and thickening. Our model is characterized by two cosmologically significant improvements. First, the satellites start at a distance more than 3 times the radius of the optical disk, which ensures a realistic interaction among the satellite, the disk, and the halo in the course of the satellite infall. Second, we allow evolution of the structure and velocity ellipsoid of the disk due to internal heating. We study the commonly arising case of low-density satellites in contrast to that of compact satellites considered in previous work. We find that disks are mainly tilted rather than heated by infalling satellites. Satellites of 10%, 20%, and 30% of the disk mass tilt the disk by angles of 2. °9 ± 0. °3, 6. °3 ± 0. °1, and 10. °6 ± 0. °2. However, only 3.4%, 6.9%, and 11.1% of the orbital angular momentum is transferred to the parent galaxy. The kinetic energy associated with vertical motion in the initial coordinate frame of the disk is respectively increased by (6 ± 3)%, (26 ± 3)%, and (51 ± 5)%, whereas the corresponding thermal energy associated with the vertical random motion in the tilted coordinate frame is only increased by (4 ± 3)%, (6 ± 2)%, and (10 ± 2)%, respectively. The satellites cause warps that are substantially damped over 30 disk rotations. Given our choice of initial conditions, satellites are mainly accreted to the parent halos. Satellites having up to 20% of the disk mass produce no observable thickening, whereas a satellite with 30% of the disk mass produces little observable thickening inside the half-mass radius but great damage beyond this radius. Hence, high cosmological accretion and thin disks can coexist if most infalling satellites have densities comparable to that of the parent galaxy.
Time correlators from deferred measurements

Repeated measurements that typically occur in two-time or multitime correlators rely on von Neumann's projection postulate, telling how to restart the system after an intermediate measurement. We invoke the principle of deferred measurement to describe an alternative procedure in which coevolving quantum memories extract system information through entanglement, combined with a final readout of the memories described by Born's rule. Our approach to repeated quantum measurements respects the unitary evolution of quantum mechanics during intermediate times, unifies the treatment of strong and weak measurements, and reproduces the projected and (anti) symmetrized correlators in the two limits. As an illustration, we apply our formalism to the calculation of the electron charge correlator in a mesoscopic physics setting, where single electron pulses assume the role of flying memory qubits. We propose an experimental setup that reduces the measurement of the time correlator to the measurement of currents and noise, exploiting the (pulsed) injection of electrons to cope with the challenge of performing short-time measurements.