Miracle-dz/UniFAR-FTUs huggingface dataset:
Two lectures on D-geometry and noncommutative geometry

Over the last few years, a new paradigm for thinking about fundamental theories of physics has emerged, using the ideas of supersymmetry, effective theory, and duality. The largest, perhaps all-encompassing example, is called M theory, and subsumes the known superstring theories and eleven dimensional supergravity. We now have a fairly good understanding of the moduli space of M theory compactifications with extended supersymmetry. In contrast to some of the expectations raised by string theory in the 80’s, geometry as already studied by the mathematicians: algebraic geometry, differential geometry, and so on, has played a central role. Partly this has been because of the choice of questions. One specifies an effective field theory by specifying a field content and Lagrangian; on very general grounds the fields should be thought of as a set of coordinates on some configuration space; the potential as a function; the kinetic term as a metric on this space. This is true if we derive the theory in a conventional Kaluza-Klein picture, and the geometry of this effective field theory has much in common with that of the internal manifold. It is just as true if we derive the theory from some generalization of the Kaluza-Klein picture in which the internal space is not described by conventional geometry, say because it is too small, because it is singular, because quantum fluctuations are large, or perhaps because our starting point is not geometrical. Thus the language of differential geometry will always be useful; complex or Kahler geometry will be useful given the appropriate supersymmetry, and so on. Once we start studying the structure of the internal space itself we might
Mastication Wear of Two Low Profile Attachment Systems for Overdenture: An In Vitro Study

Background. Edentulism is still a major problem in the world’s population today. Implant-retained overdenture has proven to be a valid therapeutic solution in the mandible. This type of rehabilitation requires replacement of the matrices when those reach inadequate retention due to wearing processes. This study is aimed at evaluating the drop in retention of low-profile precision attachments following the application of vertical chewing forces. Two different attachment designs were compared. Methods. This in vitro study simulated an implant-retained overdenture on an edentulous mandible. Two low-profile attachments were compared. Loaded and unloaded sides were considered. Tests were performed by exerting a vertical cyclic force on the prosthesis at the level of the first molar of a hemiarch. Retention tests were performed before and after 400.000 chewing cycles, comparable to one year of use. Results. The presence of vertical load wear was identified and characterized. Retention never fell below the values indicated by the manufacturer. Furthermore, significant differences were identified between the two retention systems. Conclusions. Loss of occlusal load retention is a component that must be evaluated by the clinician during the design of implant-prosthetic rehabilitation, particularly in those cases where elevated occlusal forces or parafunctions are present.
Nondestructive Evaluation of Detuned Wavelength for As-Grown VCSEL Epi-Wafer

We propose a nondestructive method to estimate the peak wavelength of the active quantum well (QW) region of an as-grown vertical-cavity surface-emitting laser (VCSEL) epi-wafer based on room temperature electroluminescence (EL) measurements. Contacts for the electrical excitation are established using flexible conductive materials on the epilayers without the fabrication of metal electrodes. The angle dependence of the EL properties is investigated to analyze the detuned wavelength of the active QW region for the VCSEL structure. The wavelength offset caused by detuning obtained from the as-grown epi-wafer correlates with the laser threshold properties of the VCSEL chips fabricated from the epi-wafer. The results show the possibility of a nondestructive evaluation method without metal electrodes for as-grown VCSEL epi-wafers, particularly the active QW region, which has been challenging to optically analyze from completed VCSEL epi-structures.
Multi-epoch X-ray observations of the Seyfert 1.2 galaxy Mrk 79: bulk motion of the illuminating X-ray source

Multi-epoch X-ray spectroscopy (0.3 25keV) of the Seyfert 1.2 galaxy Mrk 79 (UGC 3973) spanning nearly eight years and a factor of three in broadband flux are analysed. The data are obtained at seven epochs with either XMM-Newtonor Suzaku. Comparison with contemporaneous RXTE monitoring indicate that all flux states of Mrk 79 are represe nted by the data. The spectra are fitted in a self-consistent manner adopting a power law and ionised reflection to describe the broadband continuum. Modification of the spe ctra by a distant photoionised medium, seen predominantly in emission, are also included. Under the assumption that the inner disk is at the innermost stable circular orbit, our blu rred reflection models give a spin of a = 0.7±0.1. The reflection component in each spectrum is weaker than pre dicted by simple reflection models. If the illuminating X-ray emission is pro duced by flares above the disk that move at mildly relativistic velocities, however, diminish ed reflection is expected. Light bending due to strong gravity near black holes can influence how th e illuminating and reflected flux are observed; variations in Mrk 79 do not suggest that lig ht bending is important in this source.
A moderate cooling flow phase at galaxy formation

I study the possibility that a cooling flow (CF) exists at the main phase of supermassive black hole (SMBH) growth during galaxy formation. To ensure that jets launched by the SMBH efficiently expel gas from the galaxy, as is required by recent results, the gas should be in the hot phase, rather than in cold clouds. The short radiative cooling time of the hot gas leads to the formation of a CF, but heating by the active galactic nucleus prevents catastrophic cooling. Cold blobs that start as instabilities in the hot phase feed the SMBH from an extended region, form an accretion disc, and lead to the formation of jets. These jets can expel large quantities of gas out of the galaxy. This cycle, which is termed the cold feedback mechanism in CFs in clusters of galaxies, might explain the correlation of SMBH to bulge masses. Stars are formed, but at a lower rate than what is expected when heating is not included. Such a CF is termed a moderate CF.
Cooperative Buffer Management With Fine-Grained Data Migrations for Hybrid Memory Systems

Hybrid memory composed of DRAM and persistent memory (PM) offers a promising way to realize large-capacity main memory supporting in-memory data storage and computing. However, traditional buffer management schemes focus on improving the hit ratio but lack awareness of the limitations of PM, e.g., slower write time and lower write endurance than DRAM. Therefore, developing new buffer management policies that can reduce costly write-backs of PM blocks while maintaining high performance for the hybrid buffer, is of paramount importance. Existing approaches mainly use a page-grained buffering policy, which will cause unnecessary data migrations between DRAM and PM, leading to a high number of disk I/Os and PM writes. Aiming to reduce I/O costs and PM writes, we propose a new buffer manager named HiBuffer for DRAM/PM-based hybrid memory systems. HiBuffer presents several novel ideas. First, it adopts multigrained data layouts to manage the hybrid buffer cooperatively. In addition to the page granularity, we introduce Lines for the DRAM buffer and Sectors to the PM buffer, forming a buffer with three granularities, including Line, Sector, and Page. We prove that the multigrained cooperative buffer management can deliver higher performance than existing page-grained schemes. Second, we propose a sector-grained method to migrate data from DRAM to PM, which can avoid unnecessary data movements and reduce PM writes. Third, we use an out-of-place updating mechanism to absorb updates in DRAM, which can further reduce the writes to PM. We compare HiBuffer with three existing schemes, including LRU, CLOCK-DWF, and MiniPage, on five synthetic workloads and the YCSB benchmark using real Intel Optane DC PM. The results in terms of various metrics, including running time, PM writes, hit ratio, and disk I/Os, suggest the efficiency of HiBuffer. In particular, HiBuffer reduces the running time by up to 37.8% and the writes to PM by up to 83% compared to the competitors when evaluated on the YCSB benchmark.
Study of the Abundance Patterns in the Metal-Poor Stellar Stream

Abstract The chemical abundances of the metal-poor stars in the stellar stream provide important information for setting constraints on models of neutron-capture processes. The study of these stars could gives us a better understanding of the r-process nucleosynthesis and chemical composition of the early Galaxy. Using the updated main r-process and weak r-process patterns, we fit abundances in the stellar stream stars. The weak r-process component coefficients are almost constant for the sample stars, including r-rich stars, which means that both the weak r-process and Fe are produced as primary elements from Type II supernovae and their yields have nearly a constant mass fraction. The difference between the stream stars and r-rich stars is obvious. For the stream stars, the fact that the increased trend in the main r-process component coefficients as metallicity increases means a gradual increase in the production of main r-process elements relative to iron. This behaviour implies that the masses of progenitors for the main r-process are smaller than those of the weak r-process. Furthermore, we find that the metal-poor stream star HD 237846 is a weak r-process star.
Population structure and genetic diversity of chickpea germplasms

In various leguminous crops, chickpea is the fourth most important legume contributing 3.1% to the total legume production. Grains of chickpea are rich source of proteins, minerals and vitamins which makes them suitable for both food and feed. For any crop to be improved, the knowledge of genetic diversity of wild and elite cultivar is very important. Therefore among various available marker systems, molecular markers are more reliable and accurate, therefore are very commonly used for genetic diversity analysis, phylogenetic studies and cultivar identification. Due to several advantages of Inter Simple Sequence Repeat (ISSR) markers in present study we analyzed the genetic diversity, structure, cross-species transferability and allelic richness in 50 chickpea collection using 23 ISSR markers. The observed parameters such as allele number varied from 3 to 16, and PIC varied from 0.15 to 0.4988 respectively. Further, range of allele size varied from 150 to 1600 bp which shows the significance of ISSR markers for chickpea germplasms characterization. On the basis of ISSR marker genotypic data dendrogram were constructed which divides these 50 chickpea in group I and II showing the reliability of ISSR markers. Among 50 chickpea, the accession P 74-1 is in group I and rest are in group II. Further we made mini-core collection of 15 diverse chickpea and subgrouped them. Dendrogram, PCA, Dissimilarity matrix and Bayesian model based genetic clustering of 50 chickpea germplasms revealed that P 74-1,P 1883, P 1260 very diverse chickpea accession. Characterization of these diverse chickpea would help in maintenance breeding, conservation and in future could be used to develop climate resilient elite cultivar of chickpea. Utilization of these novel ISSRs markers in diversity analysis and population structure characterization of 50 chickpea germplasm suggests their wider efficacy in superior scale for molecular breeding studies in chickpea.
Accretion of Uranus and Neptune from inward-migrating planetary embryos blocked by Jupiter and Saturn

Reproducing Uranus and Neptune remains a challenge for simulations of solar system formation. The ice giants' peculiar obliquities suggest that they both suffered giant collisions during their formation. Thus, there must have been an epoch of accretion dominated by collisions among large planetary embryos in the primordial outer solar system. We test this idea using N-body numerical simulations including the effects of a gaseous protoplanetary disk. One strong constraint is that the masses of the ice giants are very similar -- the Neptune/Uranus mass ratio is $\sim1.18$. We show that similar-size ice giants do indeed form by collisions between planetary embryos beyond Saturn. The fraction of successful simulations varies depending on the initial number of planetary embryos in the system, their individual and total masses. Similar-sized ice giants are consistently reproduced in simulations starting with 5-10 planetary embryos with initial masses of $\sim$3-6 ${\rm M_\oplus}$. We conclude that accretion from a population of planetary embryos is a plausible scenario for the origin of Uranus and Neptune.
Microstructure and magnetic anisotropy of ultrathin Co/Pt multilayers grown on GaAs (1̄1̄1̄) by molecular-beam epitaxy

Multilayers of (Co3 A, Pt15 A)x, x=15 or 30 repeats, with or without a 200 A silver buffer layer, were grown on GaAs (111) substrates by molecular‐beam epitaxy. Vibrating sample magnetometry measurements confirmed that the samples with the Ag buffer layer show strong uniaxial magnetic anisotropy perpendicular to the surface. The perpendicular anisotropy exhibited by these metallic superlattices is discussed in terms of the microstructure of the overall multilayer stack, as well as the structural characteristics of the Co interface layer. Samples grown on the Ag buffer layer show strong (111) texture with 30–40‐nm‐size twin‐related grains. These grains, correspond to the two possible (111) stacking sequence for an fcc lattice, i.e., double positioning. However, direct growth on GaAs (111) results in randomly oriented 10–20 nm grains. All samples exhibit a repeat period of 1.83 nm in both low‐angle reflectivity and high‐angle Θ–2Θ x‐ray scattering measurements. In addition, transverse scans through the low‐.
Hamiltonian cosmology in bigravity and massive gravity

In the Hamiltonian language we provide a study of flat-space cosmology in bigravity and massive gravity constructed mostly with de Rham, Gabadadze, Tolley (dRGT) potential. It is demonstrated that the Hamiltonian methods are powerful not only in proving the absence of the Boulware-Deser ghost, but also in solving other problems. The purpose of this work is to give an introduction both to the Hamiltonian formalism and to the cosmology of bigravity. We sketch three roads to the Hamiltonian of bigravity with the dRGT potential: the metric, the tetrad and the minisuperspace approaches.
A Conceptual Framework for Understanding Faster-Than-Light Neutrinos

Recent experiments have led to the production of neutrinos with transit times indicating the appearance of traveling faster than the speed of light. In this paper, we present a conceptual framework to understand how faster-than-light events involving neutrinos (as indicated by time-of-flight) might occur. We propose that observations of this kind do not violate the special theory of relativity; instead, they only help to provide evidence in support of the general theory of relativity at quantum scales. Given the relativistic effects of the neutrino on its local spacetime environment, the measured time-of-flight at the macroscopic level is attributable to a decrease in the effective path length traversed by the neutrino. Specifically, along preferred directions, we show that the Kerr metric allows for the compression of spacetime; hence, the decreased path length hypothesis is plausible. Furthermore, when the motion of the neutrino is along the preferred direction for spacetime compression, the Kerr metric also predicts strong frame dragging effects near the Planck length. In the region where strong frame dragging occurs, we propose that the microscopic explanation for the path length compression is due to the formation of 'micro-wormholes' near the Planck length.
Gravitational radiative corrections from effective field theory

In this paper we construct an effective field theory (EFT) that describes long wavelength gravitational radiation from compact systems. To leading order, this EFT consists of the multipole expansion, which we describe in terms of a diffeomorphism invariant point particle Lagrangian. The EFT also systematically captures 'post-Minkowskian' corrections to the multipole expansion due to nonlinear terms in general relativity. Specifically, we compute long distance corrections from the coupling of the (mass) monopole moment to the quadrupole moment, including up to two mass insertions. Along the way, we encounter both logarithmic short distance (UV) and long wavelength (IR) divergences. We show that the UV divergences can be (1) absorbed into a renormalization of the multipole moments and (2) resummed via the renormalization group. The IR singularities are shown to cancel from properly defined physical observables. As a concrete example of the formalism, we use this EFT to reproduce a number of post-Newtonian corrections to the gravitational wave energy flux from nonrelativistic binaries, including long distance effects up to 3 post-Newtonian (v{sup 6}) order. Our results verify that the factorization of scales proposed in the NRGR framework of Goldberger and Rothstein is consistent up to order 3PN.
Multi-wavelength study of XMMU J2235.3-2557: the most massive galaxy cluster at z > 1

Context. The galaxy cluster XMMU J2235.3−2557 (hereafter XMM2235), spectroscopically confirmed at z = 1.39, is one of the most distant X-ray selected galaxy clusters. It has been at the center of a multi-wavelength observing campaign with ground and space facilities. Aims. We characterize the galaxy populations of passive members, the thermodynamical properties and metal abundance of the hot gas, and the total mass of the system using imaging data with HST/ACS (i775 and z850 bands) and VLT/ISAAC (J and KS bands), extensive spectroscopic data obtained with VLT/FORS2, and deep (196 ks) Chandra observations. Methods. Chandra data allow temperature and metallicity to be measured with good accuracy and the X-ray surface brightness profile to be traced out to 1 � (or 500 kpc), thus allowing the mass to be reliably estimated. Out of a total sample of 34 spectroscopically confirmed cluster members, we selected 16 passive galaxies (without detectable [OII]) within the central 2 � (or 1 Mpc) with ACS coverage, and inferred star formation histories for subsamples of galaxies inside and outside the core by modeling their spectrophotometric data with spectral synthesis models. Results. Chandra data show a regular elongated morphology, closely resembling the distribution of core galaxies, with a significant cool core. We measure a global X-ray temperature of kT = 8.6 +1.3 −1.2 keV (68% confidence), which we find to be robust against several systematics involved in the X-ray spectral analysis. By detecting the rest frame 6.7 keV Iron K line in the Chandra spectrum, we measure a metallicity Z = 0.26 +0.20 −0.16 Z� . In the likely hypothesis of hydrostatic equilibrium, we obtain a total mass of Mtot( 1, with a baryonic content, both its galaxy population and intracluster gas, in a significantly advanced evolutionary stage at 1/ 3o f the current age of the Universe.
A Brief Review on mm-Wave Antennas for 5G and Beyond Applications

Due to exponential growth in wireless communication in the last decade, which continues towards future applications, mm-wave has shown tremendous potential and has been established as the backbone of most modern-day high data rate communication systems. Despite many challenges associated with this technology, several inherent advantages have established it as an attractive and essential choice for high data rate communication systems. It is well known that antennas are crucial integral components of any communication system. Most modern-day mm-wave communication devices require a low profile, wideband, and highly efficient antenna system. Recent advancements in research and development in this field have been reported through many publications. This article reviews the mm-wave antennas with briefs about their characterization setup, fabrication technologies and some of the associated challenges.
Machine learning algorithms for sentiment analysis

Проводится комплексный анализ технологии машинного обучения. В ходе исследования разработаны алгоритмы глубокого обучения для анализа тональности текста и проведено сравнение их эффективности с другими классификаторами на основе алгоритмов машинного обучения. The study provides a comprehensive analysis of machine learning technology. In the course of the study, deep learning algorithms were developed for analyzing the sentiment of the text and a comparison was made of their effectiveness with other classifiers based on machine learning algorithms.
The response of gas giant ionospheres to space environment forcing

James O’Donoghue The Response Of Gas Giant Ionospheres To Space Environment Forcing At high spatial and spectral resolution, the 10-metre Keck and 3metre NASA IRTF ground-based telescopes were used to observe Saturn and Jupiter, respectively. Pole-to-pole profiles of H3 emission were recorded along the planets’ respective noon meridians. The low latitude ionospheric H3 emission of these planets was thought to be broadly uniformly decreasing towards the equator, with the transition from bright emission at the poles produced by particle precipitation, to the weaker background glow elsewhere produced by sunlight. Instead, however, a pattern of intensity variability was detected at both Jupiter and Saturn. This pattern was found to be symmetric about the magnetic equator at Saturn, with peaks in H3 intensity magnetically mapping to gaps in Saturn’s rings. The transport of water ions from the gaps in Saturn’s rings to the planetary ionosphere, delivered via magnetic field lines, was used to explain this, as water ions cause an increased H3 density and therefore emission. In the same dataset, the temperature of Saturn’s H3 aurorae remained effectively constant, whilst the H3 column density and total emission varied greatly. The southern auroral oval was found to be significantly warmer than its northern counterpart, having average temperatures of 583 and 527 K, respectively. This asymmetry was attributed to an inverse relationship between ionospheric Joule and ion drag heating with magnetic field strength. Jupiter’s low latitude ionosphere also appears to vary significantly in H3 emission, but this time in longitude. This may be due to an inversely proportional relationship between magnetic field strength and particle precipitation. In summary, the planetary ionospheres of Saturn and Jupiter have been found to be globally subjected to space environment forcing. Whilst such forcing was well established for the auroral regions, we have here discovered that particle precipitation can dominate the low latitude ionospheres of the gas giants.
Evaluating a new NEMO-based Persian/Arabian Gulf tidal operational model

A 3-D baroclinic pre-operational model, including tides of the Persian/Arabian Gulf, has been developed at the Met Office using the NEMO framework. The non-assimilative model is believed to represent a significant improvement over the existing POLCOMS based system, benefiting from: extended domain; improved resolution; more accurate representation of coasts and bathymetry; improved representation of tides; and improved representation of salinity. As expected, with sea surface temperature (SST) data assimilation, the accuracy of SST is significantly improved. However, data assimilation also appears to help reduce thermal biases throughout the water column, within the limited accuracy of a climatology comparison. Operational implementation occurred in late 2012.