Miracle-dz/UniFAR-FTUs huggingface dataset:
Formfactor perturbation expansions and confinement in the Ising field theory

We study the particle spectrum Mn(h) in the two-dimensional ferromagnetic Ising field theory in a weak external magnetic field h. According to the Wu and McCoy scenario of the weak confinement, pairs of fermions (domain walls) are coupled into bosonic kink–antikink bound states at small h > 0. Fluctuations with more than two fermions also contribute to the wavefunctions of the compound particles, leading to multi-fermion corrections to their masses Mn(h) in higher orders in h. We describe a perturbative procedure, which allows us to account for both multi-fermion fluctuations and the long-range confining interaction between fermions, and leads to the formfactor expansions for the renormalized parameters of the model. We obtain integral representations for the third-order multi-fermion correction to the mass Mn(h), which arises from the regular correction to the kernel of the Bethe–Salpeter equation.
COOL CORE CYCLES: COLD GAS AND AGN JET FEEDBACK IN CLUSTER CORES

Using high-resolution 3D and 2D (axisymmetric) hydrodynamic simulations in spherical geometry, we study the evolution of cool cluster cores heated by feedback-driven bipolar active galactic nuclei (AGNs) jets. Condensation of cold gas, and the consequent enhanced accretion, is required for AGN feedback to balance radiative cooling with reasonable efficiencies, and to match the observed cool core properties. A feedback efficiency (mechanical luminosity ≈ ϵ M ˙ acc c 2 ; ? > where M ˙ acc ? > is the mass accretion rate at 1 kpc) as small as 6 × 10−5 is sufficient to reduce the cooling/accretion rate by ∼10 compared to a pure cooling flow in clusters (with M 200 ≲ 7 × 10 14 ? > M ⊙ ? > ). This value is much smaller compared to the ones considered earlier, and is consistent with the jet efficiency and the fact that only a small fraction of gas at 1 kpc is accreted onto the supermassive black hole (SMBH). The feedback efficiency in earlier works was so high that the cluster core reached equilibrium in a hot state without much precipitation, unlike what is observed in cool-core clusters. We find hysteresis cycles in all our simulations with cold mode feedback: condensation of cold gas when the ratio of the cooling-time to the free-fall time ( t cool / t ff ? > ) is ≲10 leads to a sudden enhancement in the accretion rate; a large accretion rate causes strong jets and overheating of the hot intracluster medium such that t cool / t ff > 10 ; ? > further condensation of cold gas is suppressed and the accretion rate falls, leading to slow cooling of the core and condensation of cold gas, restarting the cycle. Therefore, there is a spread in core properties, such as the jet power, accretion rate, for the same value of core entropy or t cool / t ff ? > . A smaller number of cycles is observed for higher efficiencies and for lower mass halos because the core is overheated to a longer cooling time. The 3D simulations show the formation of a few-kpc scale, rotationally supported, massive ( ∼ 10 11 M ⊙ ? > ) cold gas torus. Since the torus gas is not accreted onto the SMBH, it is largely decoupled from the feedback cycle. The radially dominant cold gas (T < 5 × 104 K; ∣ v r ∣ > ∣ v φ ∣ ? > ) consists of fast cold gas uplifted by AGN jets and freely infalling cold gas condensing out of the core. The radially dominant cold gas extends out to 25 kpc for the fiducial run (halo mass 7 × 10 14 M ⊙ ? > and feedback efficiency 6 × 10−5), with the average mass inflow rate dominating the outflow rate by a factor of ≈2. We compare our simulation results with recent observations.
Transmittance assisted interpretation of 3D nerve fibre architectures

Transmission microscopy measurements of histological brain sections provide usually only 2D (in-plane) information about the spatial nerve fibre architecture. To access the third dimension (out-of-plane orientation) of the nerve fibres, more advanced techniques are required, such as Three-dimensional Polarized Light Imaging (3D-PLI) which uses birefringence measurements to derive the 3D fibre orientations. Here, we show that the polarization-independent transmitted light intensity (transmittance) already contains 3D information: we demonstrate in experimental studies of multiple species (rodent, monkey, human) that the transmittance decreases significantly (by more than 50 %) with increasing out-of-plane angle of the nerve fibres. Using finite-difference time-domain simulations, we demonstrate that this decrease is mainly caused by polarization-independent light scattering in combination with the finite numerical aperture of the imaging system, and that the transmittance does not depend on the crossing angle between in-plane fibres. This allows to use the transmittance e.g. to distinguish between in-plane crossing and out-of-plane nerve fibres in 3D-PLI measurements.
Learning robust and high-precision quantum controls

Robust and high-precision quantum control is extremely important but challenging for the functionalization of scalable quantum computation. In this paper, we show that this hard problem can be translated to a supervised machine learning task by thinking of the time-ordered quantum evolution as a layer-ordered neural network (NN). The seeking of robust quantum controls is then equivalent to training a highly generalizable NN, to which numerous tuning skills matured in machine learning can be transferred. This opens up a door through which a family of robust control algorithms can be developed. We exemplify such potential by introducing the commonly used trick of batch-based optimization, and the resulting batch-based gradient algorithm is numerically shown to be able to remarkably enhance the control robustness while maintaining high fidelity.
Screening of Nutritional Deficiency Manifestations Among Egyptian Elderly: Cross-sectional study

Background : Nutritional deficiencies are frequently not detected or misdiagnosed in old age as they could mimic the natural changes associated with aging Aim : To screen the clinical manifestations of nutritional deficiencies among the elderly . Method: A cross-sectional study was conducted on 100 elderly participants with chronic diseases, aged 65 or more, chosen randomly from the outpatient clinic and inpatient at Menoufia university hospital, Egypt. Tools of the study: Demographic and clinical data; a checklist of symptoms and signs of common nutritional deficiency; and a subjective global assessment (SGA). Results : the distribution of potential nutritional clinical manifestations among elderly revealed was variable ; skin rash (29%), easy bruising (41%), loss or thinning of hair (75%), spooning of nails (20%), impaired vision at night (37%), clouding and corneal dryness. (57%), bleeding gums (56%), bone deformities (bowlegs, knocked knees, curved spine) (6%), bone tenderness (49%). There were statistically significant difference between SGA and the following chronic diseases: (DM, hepatic, renal, and rheumatic) also significance associations between (skin rash in sun-exposed areas in hepatic diseases (p = 0.04), spooning of nails in renal disease (p = 0.06), Impaired night vision in cardiac and diabetic patients (p = 0.001), rheumatic diseases had more bone tenderness and diarrhea (p = 0.001) Conclusion : The most common nutritional deficiency manifestations among elderly were; thinning or loss of hair, corneal drying or clouding, bleeding gum, easy bruising, and bone tenderness. SGA based nutritional status of elderly was (35%) well-nourished, (49%) mild to moderate, and (16%) severe malnutrition.
DETAILED CHEMICAL ABUNDANCES IN THE r-PROCESS-RICH ULTRA-FAINT DWARF GALAXY RETICULUM 2

The ultra-faint dwarf (UFD) galaxy Reticulum 2 (Ret 2) was recently discovered in images obtained by the Dark Energy Survey. We have observed the four brightest red giants in Ret 2 at high spectral resolution using the Michigan/Magellan Fiber System. We present detailed abundances for as many as 20 elements per star, including 12 elements heavier than the Fe group. We confirm previous detection of high levels of r-process material in Ret 2 (mean [Eu/Fe] = +1.69 ± 0.05) found in three of these stars (mean [Fe/H] = −2.88 ± 0.10). The abundances closely match the r-process pattern found in the well-studied metal-poor halo star CS 22892–052. Such r-process-enhanced stars have not been found in any other UFD galaxy, though their existence has been predicted by at least one model. The fourth star in Ret 2 ([Fe/H] = −3.42 ± 0.20) contains only trace amounts of Sr ([Sr/Fe] = −1.73 ± 0.43) and no detectable heavier elements. One r-process enhanced star is also enhanced in C (natal [C/Fe] ≈ +1.1). This is only the third such star known, which suggests that the nucleosynthesis sites leading to C and r-process enhancements are decoupled. The r-process-deficient star is enhanced in Mg ([Mg/Fe] = +0.81 ± 0.14), and the other three stars show normal levels of α-enhancement (mean [Mg/Fe] = +0.34 ± 0.03). The abundances of other α and Fe-group elements closely resemble those in UFD galaxies and metal-poor halo stars, suggesting that the nucleosynthesis that led to the large r-process enhancements either produced no light elements or produced light-element abundance signatures indistinguishable from normal supernovae.
Large-scale fabrication of BN tunnel barriers for graphene spintronics

We have fabricated graphene spin-valve devices utilizing scalable materials made from chemical vapor deposition (CVD). Both the spin-transporting graphene and the tunnel barrier material are CVD-grown. The tunnel barrier is realized by Hexagonal boron nitride, used either as a monolayer or bilayer and placed over the graphene. Spin transport experiments were performed using ferromagnetic contacts deposited onto the barrier. We find that spin injection is still greatly suppressed in devices with a monolayer tunneling barrier due to resistance mismatch. This is, however, not the case for devices with bilayer barriers. For those devices, a spin relaxation time of ∼260 ps intrinsic to the CVD graphene material is deduced. This time scale is comparable to those reported for exfoliated graphene, suggesting that this CVD approach is promising for spintronic applications which require scalable materials.
A decade of radio imaging the relativistic outflow in the peculiar X-ray binary Circinus X-1

We present observations of the neutron star X-ray binary and relativistic jet source Circinus X-1 made at 4.8 and 8.6 GHz with the Australia Telescope Compact Array during a time interval of almost 10 yr. The system shows significant variations in the morphology and brightness of the radio features on all time-scales from days to years. Using the time delay between the successive brightening of the different components of the radio emission we were able to provide further evidence for the relativistic nature of the arcsec-scale outflow, with an apparent velocity beta(app) >= 12. No compelling evidence for an evolution of the orientation of the jet axis was found. We also place an upper limit on the proper motion of the system which is consistent with previous optical studies. Besides the previously reported radio flares close to the orbital phase 0.0 (interpreted as enhanced accretion at periastron passage), we identified outbursts with similar properties near the orbital phase 0.5. The global spectral index revealed a preferentially steep spectrum over the entire period of monitoring with a mean value and standard deviation alpha = -0.9 +/- 0.6(F-nu proportional to nu(alpha)), which became significantly flatter during the outbursts. Polarization was detected in one third of the epochs, and in one case Faraday rotation close to the core of the system was measured.
The growth and enrichment of intragroup gas

The thermal and chemical properties of the hot diffuse intragroup medium (IGrM) provide important constraints on the feedback processes associated with massive galaxy formation and evolution. Here we explore these constraints via a detailed analysis of the global properties of simulated z<3 galaxy groups from a cosmological simulation that includes a well-constrained prescription for stellar/supernovae-powered galactic outflows but no AGN feedback. Our aims are to (a) establish a baseline against which we will compare future models; (b) identify model successes due to stellar/supernovae-powered outflows; and (c) pinpoint features that signal the need for, and constrain the nature of, AGN feedback. Our simulation successfully reproduces key observed z=0 group IGrM properties, including the various X-ray Lx - Tx - entropy scaling relations, for all but the most massive groups. The z<1 redshift evolution of these also agree with observations. Contrary to expectations, the simulated groups' IGrM does not suffer catastrophic cooling. Yet, the z=0 group stellar mass is ~ 2X too large. This is due to the build-up of cold gas in the massive galaxies before they are incorporated inside groups. This in turn indicates that other feedback mechanisms must activate in real galaxies once their stellar masses grow to a few X 10^{10} M_sun. We show that these must be powerful enough to expel a significant fraction of the gas from the galactic halos. Gentle maintenance-mode (quenching) AGN feedback, as seen in galaxy clusters, will not do. Just as importantly, we find that the stellar/supernovae-powered winds are essential for understanding the IGrM metal abundances. Our simulation is able to reproduce the observed relationship between the global IGrM iron and silicon abundance and the group X-ray temperature, and these results ought to be relatively insensitive to the addition of AGN feedback.
Detecting a Stochastic Gravitational Wave Background in the presence of a Galactic Foreground and Instrument Noise

Department of Physics, Montana State University, Bozeman, MT 59717(Dated: January 10, 2014)Detecting a stochastic gravitational wave background requires that we rst understand and modelany astrophysical foregrounds. In the millihertz frequency band, the predominate foreground signalwill be from unresolved white dwarf binaries in the galaxy. We build on our previous work to showthat a stochastic gravitational wave background can be detected in the presence of both instrumentnoise and a galactic confusion foreground. The key to our approach is accurately modeling thespectra for each of the various signal components. We simulate data for a gigameter Laser Interfer-ometer Space Antenna (LISA) operating in the mHz frequency band detector operating with both6- and 4-links. We obtain posterior distribution functions for the instrument noise parameters, thegalaxy level and modulation parameters, and the stochastic background energy density. We ndthat we are able to detect a scale-invariant stochastic background with energy density as low as
Making and identifying optical superpositions of high orbital angular momenta

National Natural Science Foundation of China (NSFC) [11104233]; Fundamental Research Funds for the Central Universities [2011121043, 2012121015]; Natural Science Foundation of Fujian Province of China [2011J05010]; Program for New Century Excellent Talents in Fujian Province University; program for New Century Excellent Talents in University of China (NCET)
Cosmic variance of the galaxy cluster weak lensing signal

Intrinsic variations of the projected density profiles of clusters of galaxies at fixed mass are a source of uncertainty for cluster weak lensing. We present a semi-analytical model to account for this effect, based on a combination of variations in halo concentration, ellipticity and orientation, and the presence of correlated haloes. We calibrate the parameters of our model at the 10 per cent level to match the empirical cosmic variance of cluster profiles at M_200m=10^14.10^15 h^-1 M_sol, z=0.25. 0.5 in a cosmological simulation. We show that weak lensing measurements of clusters significantly underestimate mass uncertainties if intrinsic profile variations are ignored, and that our model can be used to provide correct mass likelihoods. Effects on the achievable accuracy of weak lensing cluster mass measurements are particularly strong for the most massive clusters and deep observations (with ~20 per cent uncertainty from cosmic variance alone at M_200m=10^15 h^-1 M_sol and z=0.25), but significant also under typical ground-based conditions. We show that neglecting intrinsic profile variations leads to biases in the mass-observable relation constrained with weak lensing, both for intrinsic scatter and overall scale (the latter at the 15 per cent level). These biases are in excess of the statistical errors of upcoming surveys and can be avoided if the cosmic variance of cluster profiles is accounted for.
Electrically tunable three-dimensional g -factor anisotropy in single InAs self-assembled quantum dots

Three-dimensional anisotropy of the Land\'e $g$ factor and its electrical modulation are studied for single uncapped InAs self-assembled quantum dots (QDs). The $g$ factor is evaluated from measurement of inelastic cotunneling via Zeeman substates in the QD for various magnetic field directions. We find that the value and anisotropy of the $g$ factor depends on the type of orbital state which arises from the three-dimensional confinement anisotropy of the QD potential. Furthermore, the $g$ factor and its anisotropy are electrically tuned by a side gate which modulates the confining potential.
Maximum speed of hypervelocity stars ejected from binaries

The recent detection of hypervelocity stars (HVSs) as late-type B-stars and HVS candidate G/K-dwarfs raises the important question of their origin. In this Letter, we investigate the maximum possible velocities of such HVSs if they are produced from binaries which are disrupted via an asymmetric supernova explosion. We find that HVSs up to ~770 and ~1280 km/s are possible in the Galactic rest frame from this scenario for these two subclasses of HVSs, respectively. We conclude that whereas a binary origin cannot easily explain all of the observed velocities of B-type HVSs (in agreement with their proposed central massive black hole origin) it can indeed account for the far majority (if not all) of the recently detected G/K-dwarf HVS candidates.
Data-Driven Malware Detection for 6G Networks: A Survey From the Perspective of Continuous Learning and Explainability via Visualisation

5G is inherently prone to security vulnerabilities. We witness that many today's networks contain 5G security flaws due to their reliance on the existing 4G network core. A lack of security standards for 5G IoT devices means network breaches and malware threats might run uncontrolled. The future 6G network is predicted to be implemented with artificial intelligence-driven communication via machine learning, enhanced edge computing, post-quantum cryptography and so forth. With the activation of edge computing, the computing power available at supercomputing servers is to be integrated directly into the devices at the entry point of a network in a distributed manner (e.g., antennas, routers, IoT sensors, etc). This feature brings an equal quality of service everywhere including remote regions (a.k.a service everywhere) which will trigger an exponential growth of associated applications. In this intricate environment, malware attacks are becoming more challenging to detect. This paper thus reviews the theoretical and experimental data-driven malware detection literature, in the large-scale data-intensive field, relating to: (1) continuous learning, including new concepts in multi-domain to multi-target learning and the challenges associated with unseen/unknown data, imbalance data and data scarcity, and (2) new explainability via visualisation concepts with a multi-labelling approach which allows identifying malware by their recipes while improving the interpretability of its decision process.
Pre-feasibility Study Establishment of Galleria Farm for Entomopathogenic Nematodes (EPNs) Bio-Insecticides.

The development of indigenous isolates of entomopathogenic nematodes (EPNs) in vivo is a point of concern for small and medium-sized businesses (SMBs), smaller family farms, greenhouse cultivation, or even a cottage industry. Although EPN research studies in Egypt aim to the identification and usage of highly potent and effective indigenous strains against economically significant insect pests, no companies have yet been established for the development and sale of these plant protection products except for small special units affiliated with some research institutes and universities. On increasing demand for non-chemical forms of pest control and the high price product of EPNs, this research assessed the financial feasibility of Galleria mellonella farming for in vivo production of EPNs at small and medium scales. The main finding indicated that the cost production of indigenous EPNs (one Sachest containing 5 x 10 7 IJs) is 200 LE which is considered a low-price product in comparison to the price of products which is variable from about US$ 15 to US$ 160 per sales unit. Moreover, the capital recovery period after one year is 99.7 %.
The double-degenerate model for the progenitors of Type Ia supernovae

The double-degenerate (DD) model, involving the merging of massive double carbon-oxygen white dwarfs (CO WDs) driven by gravitational wave radiation, is one of the classical pathways for the formation of Type Ia supernovae (SNe Ia). Recently, it has been proposed that the WD+He subgiant channel has a significant contribution to the production of massive double WDs, in which the primary WD accumulates mass by accreting He-rich matter from an He subgiant. We evolved about 1800 CO WD+He star systems and obtained a large and dense grid for producing SNe Ia through the DD model. We then performed a series of binary population synthesis simulations for the DD model, in which the WD+He subgiant channel is calculated by interpolations in the SN Ia production grid. According to our standard model, the Galactic birth rate of SNe Ia is about 2.4 x 10(-3) yr(-1) for the WD+He subgiant channel of the DD model; the total birth rate is about 3.7 x 10(-3) yr(-1) for all channels, reproducing that of observations. Previous theoretical models still have deficit with the observed SNe Ia with delay times 8Gyr. After considering the WD+He subgiant channel, we found that the delay time distributions are comparable with the observed results. Additionally, some recent studies proposed that the violent WD mergers are more likely to produce SNe Ia based on the DD model. We estimated that the violent mergers through the DD model may contribute to at most 16 per cent of all SNe Ia.