Miracle-dz/UniFAR-FTUs huggingface dataset:
Nonprofit Organizations, Social Media, and Trust: How Self-Congruence Can Help Organizations Choose the Right Social Media Endorsers

ABSTRACT Nonprofit organizations have been increasingly professionalizing their presence on social media to influence potential donors’ perceptions and behaviors. Thus, an increasing number of organizations have started to partner with social media endorsers (i.e., influencers and celebrities). In doing so, organizations face the question of whether they should partner with endorsers who represent the potential donors’ ideal self or with endorsers who reflect the potential donors’ actual self . To examine this question, the present study is based on a cross-sectional survey with 419 social media users. Data are analyzed based on a structural equation model. Findings demonstrate that matching potential donors’ ideal self-concept positively affects competence belief, while aligning with potential donors’ actual self-concept positively increases benevolence/integrity belief. In addition, the results show that both competence belief and benevolence/integrity belief are of vital importance, as both factors positively influence attention to a social media post, which affects behavioral outcomes.
Automatic Recognition and Geolocation of Vertical Traffic Signs Based on Artificial Intelligence Using a Low-Cost Mapping Mobile System

Road maintenance is a key aspect of road safety and resilience. Traffic signs are an important asset of the road network, providing information that enhances safety and driver awareness. This paper presents a method for the recognition and geolocation of vertical traffic signs based on artificial intelligence and the use of a low-cost mobile mapping system. The approach developed includes three steps: First, traffic signals are detected and recognized from imagery using a deep learning architecture with YOLOV3 and ResNet-152. Next, LiDAR point clouds are used to provide metric capabilities and cartographic coordinates. Finally, a WebGIS viewer was developed based on Potree architecture to visualize the results. The experimental results were validated on a regional road in Avila (Spain) demonstrating that the proposed method obtains promising, accurate and reliable results.
Stable accessibility is C1 dense

— We prove that in the space of ail Cr (r ^ 1) partially hyperbolic diffeomorphisms, there is a C1 open and dense set of accessible diffeomorphisms. This settles the C1 case of a conjecture of Pugh and Shub. The same resuit holds in the space of volume preserving or symplectic partially hyperbolic diffeomorphisms. Combining this theorem with results in [Br], [Ar] and [PugSh3], we obtain several corollaries. The first states that in the space of volume preserving or symplectic partially hyperbolic diffeomorphisms, topological transitivity holds on an open and dense set. Further, on a symplectic n-manifold (n $C 4) the C1-closure of the stably transitive symplectomorphisms is precisely the closure of the partially hyperbolic symplectomorphisms. Finally, stable ergodicity is C1 open and dense among the volume preserving, partially hyperbolic diffeomorphisms satisfying the additional technical hypothèses of [PugSh3]. Introduction This paper is about the accessibility property of partially hyperbolic diffeomorphisms. We show that accessibility holds for a C1 open and dense set in the space of ail partially hyperbolic diffeomorphisms, thus settling the C1 version of a conjecture of Pugh and Shub [PugShl]. Partially hyperbolic diffeomorphisms are similar to Anosov diffeomorphisms, in that they possess invariant hyperbolic directions, but unlike Anosov diffeomorphisms, they can also possess invariant directions of nonhyper bolic behavior. Accessibility means that the hyperbolic directions fill up the manifold on a macroscopic scale. Accessibility often provides enough hyperbolicity for a variety of chaotic properties, such as topological transitivity [Br] and ergodicity 2000 Mathematics Subject Classification. — Primary 37D30, 37C20.
N-body description of Debye shielding and Landau damping

This paper brings further insight into the recently published N-body description of Debye shielding and Landau damping (Escande et al 2014 Plasma Phys. Control. Fusion 57 025017). Its fundamental equation for the electrostatic potential is derived in a simpler and more rigorous way. Various physical consequences of the new approach are discussed, and this approach is compared with the seminal one by Pines and Bohm (1952 Phys. Rev. 85 338–53).
Connection of anisotropic conductivity to tip-induced space-charge layers in scanning tunneling spectroscopy of p-doped GaAs

The electronic properties of shallow acceptors in p-doped GaAs{110} are investigated with scanning tunneling microscopy at low temperature. Shallow acceptors are known to exhibit distinct triangular contrasts in STM images for certain bias voltages. Spatially resolved I(V)-spectroscopy is performed to identify their energetic origin and behavior. A crucial parameter - the STM tip's work function - is determined experimentally. The voltage dependent potential configuration and band bending situation is derived. Ways to validate the calculations with the experiment are discussed. Differential conductivity maps reveal that the triangular contrasts are only observed with a depletion layer present under the STM tip. The tunnel process leading to the anisotropic contrasts calls for electrons to tunnel through vacuum gap and a finite region in the semiconductor.
New atmospheric parameters and spectral interpolator for the MILES cool stars

Context: The full spectrum fitting of stellar spectra against a library of empirical spectra is a well-established approach to measure the atmospheric parameters of FGK stars with a high internal consistency. Extending it towards cooler stars still remains a challenge. Aims: We address this question by improving the interpolator of the MILES (Medium-resolution INT Library of Empirical Spectra) library in the low effective temperature regime (Tefff < 4800 K), and we refine the determination of the parameters of the cool MILES stars. Methods: We use the ULySS package to determine the atmospheric parameters (Teff, logg and [Fe/H]), and measure the biases of the results with respect to our updated compilation of parameters calibrated against theoretical spectra. After correcting some systematic effects, we compute a new interpolator that we finally use to redetermine the atmospheric parameters homogeneously and assess the biases. Results: Based on an updated literature compilation, we determine Teff in a more accurate and unbiased manner compared to those determined with the original interpolator. The validity range is extended downwards to about Teff = 2900 K compared to 3500 K previously. The mean residual biases on Teff, logg, and [Fe/H], with respect to the literature compilation for the coolest stars (Teff <= 3800 K) computed using the new interpolator, are -15 K, -0.02 dex, and 0.02 dex respectively. The corresponding estimations of the external precision are 63 K, 0.23 dex, and 0.15 dex respectively. For the stars with Teff in the range 3800 - 4200 K, the determinations of Teff and [Fe/H] have been slightly improved. At higher temperatures, the new interpolator is comparable to the original one. The new version of the interpolator is publicly available.
Acetyl Co-A Carboxylase Inhibition Halts Hyperglycemia Induced Upregulation of De Novo Lipogenesis in Podocytes and Proximal Tubular Cells

The effect of glycemic stress on de novo lipogenesis (DNL) in podocytes and tubular epithelial cells is understudied. This study is aimed (A) to show the effect of glycemic stress on DNL, and (B) to assess the effect of acetyl-Co A (ACC) inhibition on halting upregulation of DNL, on the expression of other lipid regulatory genes in the DNL pathway, and on markers of fibrosis and apoptosis in podocytes and tubular epithelial cells. We used cultured mouse primary tubular epithelial cells, mouse proximal tubular (BUMPT) cells, and immortal mouse podocytes and measured their percentage of labeled 13C2-palmitate as a marker of DNL after incubation with 13C2 acetate in response to high glucose concentration (25 mM). We then tested the effect of ACC inhibition by complimentary strategies utilizing CRISPR/cas9 deletion or incubation with Acaca and Acacb GapmeRs or using a small molecule inhibitor on DNL under hyperglycemic concentration. Exposure to high glucose concentration (25 mM) compared to osmotic controlled low glucose concentration (5.5 mM) significantly increased labeled palmitate after 24 h up to 72 h in podocytes and primary tubular cells. Knocking out of the ACC coding Acaca and Acacb genes by CRISPR/cas9, downregulation of Acaca and Acacb by specific antisense LNA GapmeRs and inhibition of ACC by firsocostat similarly halted/mitigated upregulation of DNL and decreased markers of fibrosis and programmed cell death in podocytes and various tubular cells. ACC inhibition is a potential therapeutic target to mitigate or halt hyperglycemia-induced upregulation of DNL in podocytes and tubular cells.
Duals and thinnings of some relatives of the contact process

This paper considers contact processes with additional voter model dynamics. For such models, results of Lloyd and Sudbury can be applied to find a self-duality, as well as dualities and thinning relations with systems of random walks with annihilation, branching, coalescence, and deaths. We show that similar relations, which are known from the literature for certain interacting SDE's, can be derived as local mean field limits of the relations of Lloyd and Sudbury.
High-energy cosmic neutrinos from spine-sheath BL Lac jets

We recently proposed that structured (spine-sheath) jets associated to BL Lac objects offer a suitable environment for the production of the extragalactic high-energy ($E>100$ TeV) neutrino recently revealed by IceCube. Our previous analysis was limited to low-power BL Lac objects. We extend our preliminary study to the entire BL Lac population. We assume that the power of cosmic rays as well as the radiative luminosity of the sheath depend linearly on the the jet power. In turn, we assume that the latter is well traced by the $\gamma$-ray luminosity. We exploit the BL Lac $\gamma$-ray luminosity function and its cosmic evolution as recently inferred from Fermi-LAT data to derive the expected neutrino cumulative intensity from the entire BL Lac population. When considering only the low-power BL Lacs, a large cosmic ray power for each source is required to account for the neutrino flux. Instead, if BL Lacs of all powers produce neutrinos, the power demand decreases, and the required cosmic ray power becomes of the same order of the radiative jet power. We also discuss the prospects for the direct association of IceCube events with BL Lacs, providing an estimate of the expected counts for the most promising sources.
CHROMOSPHERIC EVAPORATION IN AN M1.8 FLARE OBSERVED BY THE EXTREME-ULTRAVIOLET IMAGING SPECTROMETER ON HINODE

We discuss observations of chromospheric evaporation for a complex flare that occurred on 2012 March 9 near 03:30 UT obtained from the Extreme-ultraviolet Imaging Spectrometer (EIS) on board the Hinode spacecraft. This was a multiple event with a strong energy input that reached the M1.8 class when observed by EIS. EIS was in raster mode and fortunately the slit was almost at the exact location of a significant energy input. Also, EIS obtained a full-CCD spectrum of the flare, i.e., the entire CCD was readout so that data were obtained for about the 500 lines identified in the EIS wavelength ranges. Chromospheric evaporation characterized by 150–200 km s−1 upflows was observed in multiple locations in multi-million degree spectral lines of flare ions such as Fe xxii, Fe xxiii, and Fe xxiv, with simultaneous 20–60 km s−1 upflows in million degree coronal lines from ions such as Fe xii–Fe xvi. The behavior of cooler, transition region ions such as O vi, Fe viii, He ii, and Fe x is more complex, but upflows were also observed in Fe viii and Fe x lines. At a point close to strong energy input in space and time, the flare ions Fe xxii, Fe xxiii, and Fe xxiv reveal an isothermal source with a temperature close to 14 MK and no strong blueshifted components. At this location there is a strong downflow in cooler active region lines from ions such as Fe xiii and Fe xiv, on the order of 200 km s−1. We speculate that this downflow may be evidence of the downward shock produced by reconnection in the current sheet seen in MHD simulations. A sunquake also occurred near this location. Electron densities were obtained from density sensitive lines ratios from Fe xiii and Fe xiv. Atmospheric Imaging Assembly (AIA) observations from the Solar Dynamics Observatory are used with JHelioviewer to obtain a qualitative overview of the flare. However, AIA data are not presented in this paper. In summary, spectroscopic data from EIS are presented that can be used for predictive tests of models of chromospheric evaporation as envisaged in the Standard Flare Model.
Broad-band linear polarization in late-type active dwarfs

We present recent polarimetric results of magnetically active late-type dwarfs. The polarization in these stars is found to be wavelength dependent, decreasing towards the longer wavelength. The average values of degree of polarization in these active dwarfs are found to be 0.16+/-0.01, 0.080+/-0.006, 0.056+/-0.004 and 0.042+/-0.003 per cent in B, V, R, and I bands, respectively. Present results indicate that polarization in the majority of active dwarfs are primarily due to sum of the polarization by magnetic intensification and scattering. However, supplementary sources of the polarization are also found to be present in some active stars. The correlations between the degree of polarization and various activity parameters like Rossby number, chromospheric activity indicator and coronal activity indicator are found to be stronger in B band and weaker in I band.
Precision medicine and glaucoma management: how mathematical modeling and artificial intelligence help in clinical practice

Electrical Engineering Computer Science, University of Missouri, Columbia, MO, United States; Statistics, University of Missouri, Columbia, MO, United States; School of Social Work, University of Missouri System, Columbia, MO, United States; Department of Ophthalmology, Icahn School of Medicine at Mount Sinai, New York, NY, United States; IRCCS Fondazione Bietti, Rome, Italy; Centro Oculistico Italiano, Brescia, Italy; Department of Ophthalmologyh, Moran Eye Center, Salt Lake City, UT, United States; Department of Ophthalmology, Aristotle University of Thessaloniki, Thessaloniki, Greece; Singapore Eye Research Institute, Singapore, Singapore; Eye Clinic, Lithuanian University of Health Sciences, Kaunas, Lithuania; Institute for Refractive and Ophthalmic Surgery, Zürich, Switzerland; Department of Ophthalmology, Rabin Medical Center, Petah Tikva, Israel; Mathematics, University of Missouri, Columbia, MO, United States
Nested ANOVA vs. Crossed ANOVA: When and How To Use Which.

ABSTRACT Analysis of variance (ANOVA) designs typically use what is referred to as crossed design to test for differences between means of groups. In a balanced, or crossed, one-way ANOVA, each student (unit of analysis) would have a score in each of the experimental conditions. In a two-way design, the analysis is considered crossed if each level from one way is contained in each level of the other way. In this design, every person (unit of analysis) has a score in every cell. Many experimental designs in the behavioral sciences do not qualify as a crossed design. Units of measurement are rather "nested" inside other factors. A crossed experimental design would neglect the hierarchical structure of the data and produce incorrect interpretations of results. Neglecting a nested design when one actually exists will make the researcher: (1) wrongly attribute a main effect to an interaction effect when, in fact, no interaction exists; (2) divide by the wrong degrees of freedom when determining the mean square and F-value (and the statistical significance of the F-value); and (3) assume that a main effect has a smaller effect size (eta-squared) because the sum of squares for that effect is being partly attributed to the interaction effect. (SLD)
High-voltage, low-current GaInP/GaInP/GaAs/GaInNAs/Ge solar cells

Four-junction GaInP/GaAs/GaInNAs/Ge solar cells are a widely-pursued route toward AM0 efficiencies of 35% and above, and terrestrial efficiencies of up to 40%. Extensive research into the new material system of GaInNAs has so far yielded subcells with AM0 current densities far below the /spl sim/17 mA/cm/sup 2/ needed to current match the other subcells in the stack. A new multijunction structure, a 5-junction GaInP/GaInP/GaAs/GaInNAs/Ge cell, divides the solar spectrum more finely in order to relax this current matching requirement, by using an optically thin, high-bandgap GaInP top subcell, with an additional thick, low-bandgap GaInP subcell beneath it, in combination with a GaInNAs subcell. In this way, the 5-junction cell design allows the practical use of GaInNAs subcells to increase the efficiency of multijunction cells. Light I-V and external quantum efficiency measurements of the component subcells of such 5-junction cells are discussed. Experimental results are presented for the first time on GaInP/GaInP/GaAs/GaInNAs/Ge cells with the top four junctions active, with measured V/sub oc/ of 3.90 V.
Monte Carlo generation of Bohmian trajectories

We report on a Monte Carlo method that generates one-dimensional trajectories for Bohm's formulation of quantum mechanics that does not involve differentiation or integration of any equations of motion. At each time, t = nδt (n = 1, 2, 3, …), N particle positions are randomly sampled from the quantum probability density. Trajectories are built from the sorted N sampled positions at each time. These trajectories become the exact Bohm solutions in the limits N → ∞ and δt → 0. Higher dimensional problems can be solved by this method for separable wavefunctions. Several examples are given, including the two-slit experiment.
Numerical solution of the incompressible Navier-Stokes equations

The current work is initiated in an effort to obtain an efficient, accurate, and robust algorithm for the numerical solution of the incompressible Navier-Stokes equations in two- and three-dimensional generalized curvilinear coordinates for both steady-state and time-dependent flow problems. This is accomplished with the use of the method of artificial compressibility and a high-order flux-difference splitting technique for the differencing of the convective terms. Time accuracy is obtained in the numerical solutions by subiterating the equations in psuedo-time for each physical time step. The system of equations is solved with a line-relaxation scheme which allows the use of very large pseudo-time steps leading to fast convergence for steady-state problems as well as for the subiterations of time-dependent problems. Numerous laminar test flow problems are computed and presented with a comparison against analytically known solutions or experimental results. These include the flow in a driven cavity, the flow over a backward-facing step, the steady and unsteady flow over a circular cylinder, flow over an oscillating plate, flow through a one-dimensional inviscid channel with oscillating back pressure, the steady-state flow through a square duct with a 90 degree bend, and the flow through an artificial heart configuration with moving boundaries. An adequate comparison with the analytical or experimental results is obtained in all cases. Numerical comparisons of the upwind differencing with central differencing plus artificial dissipation indicates that the upwind differencing provides a much more robust algorithm, which requires significantly less computing time. The time-dependent problems require on the order of 10 to 20 subiterations, indicating that the elliptical nature of the problem does require a substantial amount of computing effort.
GRAVITATIONAL ENCOUNTERS AND THE EVOLUTION OF GALACTIC NUCLEI. III. ANOMALOUS RELAXATION

This paper is the third in a series presenting the results of direct numerical integrations of the Fokker–Planck equation for stars orbiting a supermassive black hole (SBH) at the center of a galaxy. The algorithm of Paper II included diffusion coefficients that described the effects of random (“classical”) and correlated (“resonant”) relaxation. In this paper, the diffusion coefficients of Paper II have been generalized to account for the effects of “anomalous relaxation,” the qualitatively different way in which eccentric orbits evolve in the regime of rapid relativistic precession. Two functional forms for the anomalous diffusion coefficients are investigated, based on power-law or exponential modifications of the resonant diffusion coefficients. The parameters defining the modified coefficients are first constrained by comparing the results of Fokker–Planck integrations with previously published N-body integrations. Steady-state solutions are then obtained via the Fokker–Planck equation for models with properties similar to those of the Milky Way nucleus. Inclusion of anomalous relaxation leads to the formation of less prominent cores than in the case of resonant relaxation alone, due to the lengthening of diffusion timescales for eccentric orbits. Steady-state capture rates of stars by the SBH are found to always be less than capture rates in the presence of resonant relaxation alone.
THE FAR-ULTRAVIOLET UPS AND DOWNS OF ALPHA CENTAURI

Four years (2010–2014) of semiannual pointings by the Hubble Space Telescope Imaging Spectrograph (STIS) on nearby Alpha Centauri have yielded a detailed time history of far-ultraviolet (FUV: 1150–1700 Å) emissions of the solarlike primary (A: G2 V) and the cooler but more active secondary (B: K1 V). This period saw A climbing out of a prolonged coronal X-ray minimum, as documented contemporaneously by Chandra, while B was rising to, then falling from, a peak of its long-term (∼8 year) starspot cycle. The FUV fluxes of the primary were steady over most of the STIS period, although the [Fe xii] λ1242 coronal forbidden line ( T ∼ 1.5 ? > MK) partly mirrored the slowly rising X-ray fluxes. The FUV emissions of the secondary more closely tracked the rise and fall of its coronal luminosities, especially the “hot lines” Si iv, C iv, and N v ( T ∼ 0.8 ? > –2 × 105 K), and coronal [Fe xii] itself. The hot lines of both stars were systematically redshifted, relative to narrow chromospheric emissions, by several km s−1, showing little change in amplitude over the four-year period, especially for α Cen B, despite the significant evolution of its coronal activity. Further, the hot lines of both stars, individually and epoch-averaged, displayed non-Gaussian shapes, which most trivially could be decomposed into two components, one narrow (FWHM ∼25–45 km s−1), the other broad (60–80 km s−1). A bimodal Gaussian strategy had been applied previously to the α Cen stars, but this was the first opportunity to evaluate any time dependence. In fact, not much variation of the component properties was seen, even over the major cycle changes of B. Curiously, the line fluxes were about equally divided between the narrow and broad components for both stars. The fact that there is minimal activity dependence of the narrow/broad flux partition, as well as densities derived from O iv] line ratios, either during the cycle evolution of B or between A and B, suggests that there is a dominant “quantum” of FUV surface activity that is relatively unchanged during the cycle, aside from the fractional area covered.