Miracle-dz/UniFAR-FTUs huggingface dataset:
WHY IS A FLARE-RICH ACTIVE REGION CME-POOR?

Solar active regions (ARs) are the major sources of two of the most violent solar eruptions, namely flares and coronal mass ejections (CMEs). The largest AR in the past 24 years, NOAA AR 12192, which crossed the visible disk from 2014 October 17 to 30, unusually produced more than one hundred flares, including 32 M-class and 6 X-class ones, but only one small CME. Flares and CMEs are believed to be two phenomena in the same eruptive process. Why is such a flare-rich AR so CME-poor? We compared this AR with other four ARs; two were productive in both and two were inert. The investigation of the photospheric parameters based on the SDO/HMI vector magnetogram reveals that the flare-rich AR 12192, as with the other two productive ARs, has larger magnetic flux, current, and free magnetic energy than the two inert ARs but, in contrast to the two productive ARs, it has no strong, concentrated current helicity along both sides of the flaring neutral line, indicating the absence of a mature magnetic structure consisting of highly sheared or twisted field lines. Furthermore, the decay index above the AR 12192 is relatively low, showing strong constraint. These results suggest that productive ARs are always large and have enough current and free energy to power flares, but whether or not a flare is accompanied by a CME is seemingly related to (1) the presence of a mature sheared or twisted core field serving as the seed of the CME, or (2) a weak enough constraint of the overlying arcades.
On the Origin of the Fundamental Plane and Faber–Jackson Relations: Implications for the Star Formation Problem

We provide an explanation of the properties of the fundamental plane (FP) relation and its observed projections for a sample of nearby early-type galaxies (ETGs) in terms of a fine-tuning between the time-averaged star formation rate and their structural and dynamical characteristics. Their total V luminosity is linked with and the central velocity dispersion σ through the relation , with an rms = 0.215 (R = 0.64 and ). This fine-tuning permits us to obtain the FP in terms of two distinct “virtual planes” in the space. The first one (the virial plane; VP) represents the total galaxy mass derived from the scalar virial theorem and the mass-to-light ratio M/L, while the second plane comes from the relation , where is a parameter connected with . This is a mathematically convenient way for expressing the independence of the galaxy light from the virial equilibrium. Each galaxy in the space is identified by the intersection of these two planes. A posteriori, we show that the properties of the FP (tilt and scatter) and the zone of exclusion visible in the FP projections are consequences of this fine-tuning. The link between the FP properties and the SFR of galaxies provides a new view of the star formation phenomenon. The star formation history of an unperturbed galaxy seems to be driven by the initial conditions in the protogalaxies and is regulated across cosmic epochs by the variation of the main galaxy parameters (mass, luminosity, structural shape, and velocity dispersion).
Toward an understanding of entanglement for generalized n-qubit W-states

We solve stationarity equations of the geometric measure of entanglement for multi-qubit W-type states. In this way we compute analytically the maximal overlap of one-parameter n-qubit and two-parameter four-qubit W-type states and their nearest product states. Possible extensions to arbitrary W-type states and geometrical interpretations of these results are discussed in detail.
INTRINSIC SHAPE OF STAR-FORMING BzK GALAXIES. II. REST-FRAME ULTRAVIOLET AND OPTICAL STRUCTURES IN GOODS-SOUTH AND SXDS

We study the statistical intrinsic shape of star-forming BzK galaxies (sBzK galaxies) at z ∼ 2 in both rest-frame UV and rest-frame optical wavelengths. The sBzK galaxies are selected down to KAB = 24.0 mag in the GOODS-S and Subaru-XMM Deep Survey (SXDS) fields, where high-resolution images from the Hubble Space Telescope are publicly available. Of all 1028 galaxies in GOODS-S, 57% (583) show a single component in the Advanced Camera for Surveys/F850LP image. As Wide Field Camera (WFC3)/F160W images cover only part of GOODS-S and SXDS, 724/1028 and 2500/29835 sBzK galaxies in GOODS-S and SXDS, respectively, have WFC3 coverage. Of the sBzK galaxies in the WFC3/F160W images, 86% (626) and 82% (2044) appear as a single component in the GOODS-S and SXDS, respectively. A larger fraction of single-component objects in the F850LP images represents multiple star-forming regions in galaxies, while they are not so obvious in the F160W image which appears smoother. Most of the single-component sBzK galaxies show Sérsic indices of n = 0.5–2.5, in agreement with those of local disk galaxies. Their effective radii are 1.0–3.0 kpc and 1.5–4.0 kpc in F850LP and F160W images, respectively, regardless of the observed fields. The stellar surface mass density of the sBzK galaxies is also comparable to that of the local disk galaxies. However, the intrinsic shape of sBzK galaxies is not a round disk as seen in the local disk galaxies. By comparing apparent axial ratio (b/a) distributions of the sBzK galaxies with those of local disk galaxies by assuming tri-axial model with axes A > B > C, we found that their intrinsic face-on B/A ratios peak at B/A = 0.70 and B/A = 0.77–0.79 in the rest-frame UV and optical, respectively, and are statistically more bar-like than those of the local disk galaxies. The intrinsic edge-on C/A ratios in both rest-frame UV and optical wavelengths peak at 0.26, which is slightly larger than those of the local disk galaxies. Possible origins of this bar-like structure are bar instability, galaxy interaction, or continuous minor mergers. A study of galaxy structure evolution in cosmological simulations is desirable to examine the most likely scenario.
EXTENSIONS OF SOME COMMON FIXED POINT THEOREMS

In 1976, G. Jungck [4] initially proved a common fixed point theorem for commuting mappings, which generalizes the well-known Banach's fixed point theorem. This result has been generalized, extended and improved in various ways by many authors ([3], [5]-[7] and [9]-[13]). Recently, S. Sessa [11] introduced a generalization of commutativity, which is called^weak commutativity, and prove some common fixed point theorems for weakly commuting mappings, which generalize the result of K. M. Das and K. V. Naik [3]. On the other hand, G. Jungck [5] introduced the concept of more generalized commutativity, so called compatibility, which is more general than that of weak commutativity. The utility of compatibility in the context of fixed point theory was initially demonstrated, in extending a theorem of S. Park and J. S. Bae [10]. In general, commuting mappings are weakly commuting and weakly commuting mappings are compatible, but the converses are not necessarily true as in the examples of the section 2. By employing compatible mappings in stead of commuting mappings and using four mappings as opposed to three, G. Jungck [6] extended the results of M. S. Khan and M. Imdad [9], S・ L. Singh and S. P. Singh 卩이 and, quite recently, also obtained an interesting result concerning with his concept in his consecutive paper [7]. In this paper, we prove some common fixed point theorems for com­ patible mappings, which extend the results of D. E. Anderson, K. L. Singh and J. H. M. Whitfield [1] and G. Jungck [6], and give some examples to illustrate our main theorems.
Self‐regulated gravitational accretion in protostellar discs

We present a numerical model for the evolution of a protostellar disc that has formed self-consistently from the collapse of a molecular cloud core. The global evolution of the disc is followed for several million years after its formation. The capture of a wide range of spatial and temporal scales is made possible by use of the thin-disc approximation. We focus on the role of gravitational torques in transporting mass inward and angular momentum outward during different evolutionary phases of a protostellar disc with disc-to-star mass ratio of order 0.1. In the early phase, when the infall of matter from the surrounding envelope is substantial, mass is transported inward by the gravitational torques from spiral arms that are a manifestation of the envelope-induced gravitational instability in the disc. In the late phase, when the gas reservoir of the envelope is depleted, the distinct spiral structure is replaced by ongoing irregular non-axisymmetric density perturbations. The amplitude of these density perturbations decreases with time, though this process is moderated by swing amplification aided by the existence of the disc's sharp outer edge. Our global modelling of the protostellar disc reveals that there is typically a residual non-zero gravitational torque from these density perturbations, i.e. their effects do not exactly cancel out in each region. In particular, the net gravitational torque in the inner disc tends to be negative during first several million years of the evolution, while the outer disc has a net positive gravitational torque. Our global model of a self-consistently formed disc shows that it is also self-regulated in the late phase, so that it is near the Toomre stability limit, with a near-uniform Toomre parameter Q ≈ 1.5-2.0. Since the disc also has near-Keplerian rotation, and comparatively weak temperature variation, it maintains a near-power-law surface density profile proportional to r -3/2 .
Deep Learning on FPGAs with Multiple Service Levels for Edge Computing

In the Internet of Things (IoT) era, deep learning is emerging as a promising approach for extracting information from IoT devices. Deep learning is also employed in the edge computing environment based on the demand for faster processing. In the edge server, various hardware accelerators have been proposed in recent studies to speed up the execution of such DNNs. One such accelerator is Xilinx’s Deep Learning Processor Unit (DPU), designed for FPGA-based systems. However, the limited resource capacity of FPGAs in these edge servers imposes an enormous challenge for such implementation. Recent research has shown a clear trade-off between the “resources consumed” vs. the “performance achieved Taking a cue from these findings, we address the problem of efficient implementation of deep learning into the edge computing environment in this paper. The edge server employs FPGAs for executing the deep learning model. Each deep learning network is equipped with multiple distinct implementations represented by different service levels based on resource usage (where a higher service level implies higher performance with high resource consumption). To this end, we propose an Integer Linear Programming based optimal solution strategy for selecting a service level to maximize the overall performance subject to a given resource bound. Proof-of-concept case study with a deep learning network of multiple service levels of DPUs on a physical FPGA has also been provided.
Financial Development, Renewable Energy and Unemployment in North Africa

Purpose: The study examined the nexus between financial sector development, renewable energy usage and unemployment (UNEMP) in North African countries. The complementarities between (1) financial development (FIN) and renewable energy usage and (2) economic growth and financial development, and their influence on unemployment was also investigated within the context of North African countries. Design/Methodology/Approach: Panel data (1992-2019) analysis methods such as fixed effects, fully modified ordinary least squares (FMOLS) and pooled ordinary least squares (OLS) were used. Findings: Financial sector development had a significant unemployment reduction influence. Complementarity variables were also noted to have significantly reduced unemployment. Implications/Originality/Value: North African countries should therefore craft, develop and implement financial development, renewable energy usage (RENEW) and economic growth enhancement strategies and policies to increase job creation capacity.
Mutual information in interacting spin systems

Diese Dissertation kombiniert Ideen aus den Bereichen Quanteninformation und Festkorperphysik. Diese Verbindung hat sich bereits als auserordentlich erfolgreich erwiesen: Es hat sich gezeigt, dass anstelle des gesamten, exponentiell grosen, Hilbertraums nur ein kleiner Teil der Zustande tatsachlich physikalisch relevant ist. Durch Einsichten in die Verschrankungseigenschaften von Zustanden hat Quanteninformation hier wesentlich zu unserem Verstandnis beigetragen. In Anlehnung an solche Ideen wird in dieser Arbeit die Verwendung von mutual information (auch: Transinformation, gegenseitige Information, oder Synentropie) zur Beschreibung von Korrelationen in Festkorpersystemen motiviert und beschrieben. Dazu werden ferromagnetisch wechselwirkende Spinsysteme betrachtet. Im Bereich der Quanteninformation werden haufig die Grundzustande solcher Systeme diskutiert; in dieser Arbeit werden dagegen thermische Zustande bei endlicher Temperatur erortert werden. Mittels mutual information, die dabei als Verallgemeinerung von entanglement entropy (Verschrankungsentropie) fur den Fall gemischter Zustande gesehen werden kann, konnen wir dann die verschiedenen Phasen dieser Modelle untersuchen, und insbesondere die Phasenuber-gange zwischen ihnen. Wir werden im Wesentlichen zwei Klassen von Modellen betrachten: zum einen klassische Spins auf zweidimensionalen Gittern [Wilms11], und zum anderen vollstandig verbundene Modelle quantenmechanischer Spin-1/2-Teilchen [wilms2012finite]. In beiden Fallen zeigt die mutual information charakteristisches Verhalten am Phasenubergang und innerhalb der geordneten beziehungsweise ungeordneten Phasen. Insbesondere finden wir fur klassische Spins auf einem Gitter mittels numerischer Me-thoden eine Divergenz der ersten Ableitung der mutual information am kritischen Punkt, verbunden mit einem Maximum innerhalb der paramagnetischen Phase. Wir motivieren die Existenz dieses Maximums durch Betrachtungen von Fortuin-Kasteleyn-Clustern von parallel ausgerichteten Spins. Fur die vollstandig verbundenen Modelle zeigt sich ein anderes Verhalten: Die mutual information divergiert logarithmisch am Phasenubergang, sofern dieser ein Ubergang zweiter Ordnung ist; fur einen Ubergang erster Ordnung gibt es keine Divergenz. Analytische Rechnungen im klassischen Grenzfall unterstutzen hierbei die numerischen Ergebnisse. Das gefundene Verhalten ist konsistent mit bestehenden Resultaten, die bereits in anderen Arbeiten fur die entanglement entropy des Grundzustandes gefunden wurden.
Effect of active silica on performance of maize (Zea mays) under organic farming

A field experiment was conducted during kharif 2018-19 at Organic Unit of Instructional Farm, Rajasthan College of Agriculture, Maharana Pratap University of Agriculture and Technology, Udaipur, Rajasthan. The experiment consisting of six soil applications in main plots (0, 50, 75, 100, 125 and 150 kg/ha) and six foliar applications of active silica in sub plots (no spray, water spray, 0.25, 0.50, 0.75 and 1.0%) was carried out in split-plot design with three replications. Results indicated that significantly higher number of rows/cob, number of grains/row, test weight, grain, stover and biological yield was recorded with 150 kg/ha active silica application. Similarly, higher protein content in grain, Si content and uptake by plant at 60, 75 DAS and harvest, and N, P and K content and uptake in grain as well in stover was recorded at 150 kg/ha active silica application. Among foliar application, the spray of 1.0% active silica significantly enhanced the yield attributes, yield, protein content in grain, Si content and uptake by plant at 60, 75 DAS and harvest; and N, P and K content and uptake in grain as well in stover in maize (Zea mays L.) under organic production system.
Some refinements of Young type inequalities

In this paper, we study some improvements of Young type inequalities. We obtain some reverse improvements of Young inequality. Among other results, we show a re ﬁ ned Young inequality. For v ∈ [ 0 , 1 ] and a , b > 0, then a ∇ v b (cid:2) M Rv ( h ) a (cid:2) v b , where M v ( t ) = 1 + v ( 1 − v ) ( t − 1 ) 2 t and h = ba . And we also obtain a new Young type inequality. Furthermore, corresponding operator inequalities are also established. Mathematics
A RADIO-POLARIZATION AND ROTATION MEASURE STUDY OF THE GUM NEBULA AND ITS ENVIRONMENT

The Gum Nebula is 36°-wide shell-like emission nebula at a distance of only ∼450 pc. It has been hypothesized to be an old supernova remnant, fossil H ii region, wind-blown bubble, or combination of multiple objects. Here we investigate the magneto-ionic properties of the nebula using data from recent surveys: radio-continuum data from the NRAO VLA and S-band Parkes All Sky Surveys, and H &agr; ? > data from the Southern H-Alpha Sky Survey Atlas. We model the upper part of the nebula as a spherical shell of ionized gas expanding into the ambient medium. We perform a maximum-likelihood Markov chain Monte Carlo fit to the NVSS rotation measure data, using the H &agr; ? > data to constrain average electron density in the shell ne. Assuming a latitudinal background gradient in rotation measure, we find n e = 1.3 − 0.4 + 0.4 cm − 3 ? > , angular radius φ outer = 22 &fdg; 7 − 0.1 + 0.1 ? > , shell thickness dr = 18.5 − 1.4 + 1.5 pc ? > , ambient magnetic field strength B 0 = 3.9 − 2.2 + 4.9 &mgr; G ? > , and warm gas filling factor f = 0.3 − 0.1 + 0.3 ? > . We constrain the local, small-scale (∼260 pc) pitch-angle of the ordered Galactic magnetic field to + 7 ° ≲ ℘ ≲ + 44 ° ? > , which represents a significant deviation from the median field orientation on kiloparsec scales (∼−7.°2). The moderate compression factor X = 6.0 − 2.5 + 5.1 ? > at the edge of the H &agr; ? > shell implies that the “old supernova remnant” origin is unlikely. Our results support a model of the nebula as a H ii region around a wind-blown bubble. Analysis of depolarization in 2.3 GHz S-PASS data is consistent with this hypothesis and our best-fitting values agree well with previous studies of interstellar bubbles.
Searching for a preferred direction with Union2.1 data

A cosmological preferred direction was reported from the Type Ia supernovae data in recent years. We use the Union2.1 data to give a simple classification of such studies for the first time. Because the maximum anisotropic direction is independent of isotropic dark energy models, we adopt two cosmological models (Lambda CDM, wCDM) for the hemisphere comparison analysis and the Lambda cold dark matter (Lambda CDM) model for a dipole-fitting approach. In hemisphere comparison method, the matter density and the equation of state of dark energy are adopted as the diagnostic qualities in the Lambda CDM model and the wCDM model, respectively. In the dipole-fitting approach, we fit the fluctuation of distance modulus. We find that there is a null signal for the hemisphere comparison method, while a preferred direction (b = -14 degrees.3 +/- 10 degrees.1, l = 307.1 degrees +/- 16.2 degrees) for the dipole-fitting method. This result indicates that the dipole fit is more sensitive than the hemisphere comparison method.
TWO DISTINCT RED GIANT BRANCH POPULATIONS IN THE GLOBULAR CLUSTER NGC 2419 AS TRACERS OF A MERGER EVENT IN THE MILKY WAY

Recent spectroscopic observations of the outer halo globular cluster (GC) NGC 2419 show that it is unique among GCs, in terms of chemical abundance patterns, and some suggest that it was originated in the nucleus of a dwarf galaxy. Here we show, from the Subaru narrowband photometry employing a calcium filter, that the red giant branch (RGB) of this GC is split into two distinct subpopulations. Comparison with spectroscopy has confirmed that the redder RGB stars in the hk[=(Ca−b) − (b − y)] index are enhanced in [Ca/H] by ∼0.2 dex compared to the bluer RGB stars. Our population model further indicates that the calcium-rich second generation stars are also enhanced in helium abundance by a large amount (ΔY = 0.19). Our photometry, together with the results for other massive GCs (e.g., ω Cen, M22, and NGC 1851), suggests that the discrete distribution of RGB stars in the hk index might be a universal characteristic of this growing group of peculiar GCs. The planned narrowband calcium photometry for the Local Group dwarf galaxies would help to establish an empirical connection between these GCs and the primordial building blocks in the hierarchical merging paradigm of galaxy formation.
Inhibition of High-Temperature Requirement Protein A2 Protease Activity Represses Myogenic Differentiation via UPRmt

Skeletal muscles require muscle satellite cell (MuSC) differentiation to facilitate the replenishment and repair of muscle fibers. A key step in this process is called myogenic differentiation. The differentiation ability of MuSCs decreases with age and can result in sarcopenia. Although mitochondria have been reported to be involved in myogenic differentiation by promoting a bioenergetic remodeling, little is known about the interplay of mitochondrial proteostasis and myogenic differentiation. High-temperature-requirement protein A2 (HtrA2/Omi) is a protease that regulates proteostasis in the mitochondrial intermembrane space (IMS). Mice deficient in HtrA2 protease activity show a distinct phenotype of sarcopenia. To investigate the role of IMS proteostasis during myogenic differentiation, we treated C2C12 myoblasts with UCF101, a specific inhibitor of HtrA2 during differentiation process. A key step in this process is called myogenic differentiation. The differentiation ability of MuSCs decreases with age and can result in sarcopenia. Further, CHOP, p-eIF2α, and other mitochondrial unfolded protein response (UPRmt)-related proteins are upregulated. Therefore, we suggest that imbalance of mitochondrial IMS proteostasis acts via a retrograde signaling pathway to inhibit myogenic differentiation via the UPRmt pathway. These novel mechanistic insights may have implications for the development of new strategies for the treatment of sarcopenia.
$Z^\prime$ gauge bosons at the Tevatron

We study the discovery potential of the Tevatron for a Z-prime gauge boson. We introduce a parametrization of the Z-prime signal which provides a convenient bridge between collider searches and specific Z-prime models. The cross section for p pbar -> Z-prime X -> l^+ l^- X depends primarily on the Z-prime mass and the Z-prime decay branching fraction into leptons times the average square coupling to up and down quarks. If the quark and lepton masses are generated as in the standard model, then the Z-prime bosons accessible at the Tevatron must couple to fermions proportionally to a linear combination of baryon and lepton numbers in order to avoid the limits on Z--Z-prime mixing. More generally, we present several families of U(1) extensions of the standard model that include as special cases many of the Z-prime models discussed in the literature. Typically, the CDF and D0 experiments are expected to probe Z-prime-fermion couplings down to 0.1 for Z-prime masses in the 500--800 GeV range, which in various models would substantially improve the limits set by the LEP experiments.