Miracle-dz/UniFAR-FTUs huggingface dataset:
Orbital effects of spatial variations of fundamental coupling constants

We deal with the effects induced on the orbit of a test particle revolving around a central body by putative spatial variations of dimensionless fundamental coupling constants ζ . In particular, we assume a dipole gradient for ζ (r)/ζ along a generic direction ˆ k in space. We analytically work out the long-term variations of all the six standard osculating Keplerian orbital elements parameterizing the orbit of a test particle in a gravitationally bound two-body system. Apart from the semimajor axis a, the eccentricity e, the inclination I, the longitude of the ascending node � , the longitude of pericentreand the mean anomaly M undergo non-zero long-term changes. By using the usual decomposition along the radial (R), transverse (T) and normal (N) directions, we also analytically work out the long-term changesR, � T, � N andv R, �v T , �v N experienced by the position and the velocity vectors r and v of the test particle. Apart from � N, all the other five shifts do not vanish over one full orbital revolution. In the calculation we do not use a priori simplifying assumptions concerning e and I. Thus, our results are valid for a generic orbital geometry; moreover, they hold for any gradient direction ˆ. We compare our predictions to the latest observational results for some of the major bodies of the solar system. The largest predicted planetary perihelion precessions occur for the rocky planets, amounting to some 10 −2 -10 −3 mas per century. Apart from the Earth, they are 2 − 3 orders of magnitude smaller than the present-day accuracy in empirically determining the corrections � u � to the standard Newtonian-Einsteinian planetary perihelion rates. Numerically integrated time-series of the interplanetary range for some Earth-planet pairs yield Stark-like signatures as large as 0.1-10 mm; future planned planetary laser ranging facilities should be accurate at a cm level. The long-term variations of the lunar eccentricity and perigee are of the order of 10 −14 yr −1 and 10 −4 mas yr −1 , respectively, while the changeR in the radial component of the Moon's geocentric orbit is as large as 0.8 μm per orbit. A numerically calculated geocentric lunar range time-series has a maximum nominal peak-to-peak amplitude of just a few mm, with an average of 0.3 μm over 30 yr. The present-day accuracies in determining u e and u � for the Moon are 10 −12 yr −1 and 10 −1 mas yr −1 , respectively. The Apollo facility should be able to determine on a continuous basis of the Earth-Moon range with a mm accuracy.
Quantum secure direct communication based on supervised teleportation

We present a quantum secure direct communication(QSDC) scheme as an extension for a proposed supervised secure entanglement sharing protocol. Starting with a quick review on the supervised entanglement sharing protocol - the "Wuhan" protocol [Y. Li, et al., quant-ph/0709.1449 (2007)], we primarily focus on its further extend using for a QSDC task, in which the communication attendant Alice encodes the secret message directly onto a sequence of 2-level particles which then can be faithfully teleported to Bob using the shared maximal entanglement states obtained by the previous "Wuhan" protocol. We also evaluate the security of the QSDC scheme, where an individual self-attack performed by Alice and Bob - the out of control attack is introduced and the robustness of our scheme on the OCA is documented.
Calculation of the even-odd energy difference in superfluid Fermi systems using the pseudopotential theory

The pseudopotential theory is extended to the Bogoliubov-de Gennes equations to determine the excess energy when one atom is added to the trapped superfluid Fermi system with even number of atoms. Particular attention is paid to systems being at the Feshbach resonance point. The results for relatively small particle numbers are in harmony with the Monte Carlo calculations, but are also relevant for systems with larger particle numbers. Concerning the additional one-quasiparticle state we define and determine two new universal numbers to characterize its widths.
Evolution of the solar irradiance during the Holocene

Context. Long-term records of solar radiative output are vital for understanding solar variability and past climate change. Measurements of solar irradiance are available for only the last three decades, which calls for reconstructions of this quantity over longer time scales using suitable models. Aims. We present a physically consistent reconstruction of the total solar irradiance for the Holocene. Methods. We extend the SATIRE (Spectral And Total Irradiance REconstruction) models to estimate the evolution of the total (and partly spectral) solar irradiance over the Holocene. The basic assumption is that the variations of the solar irradiance are due to the evolution of the dark and bright magnetic features on the solar surface. The evolution of the decadally averaged magnetic flux is computed from decadal values of cosmogenic isotope concentrations recorded in natural archives employing a series of physics-based models connecting the processes from the modulation of the cosmic ray flux in the heliosphere to their record in natural archives. We then compute the total solar irradiance (TSI) as a linear combination of the jth and jth + 1 decadal values of the open magnetic flux. In order to evaluate the uncertainties due to the evolution of the Earth’s magnetic dipole moment, we employ four reconstructions of the open flux which are based on conceptually different paleomagnetic models. Results. Reconstructions of the TSI over the Holocene, each valid for a different paleomagnetic time series, are presented. Our analysis suggests that major sources of uncertainty in the TSI in this model are the heritage of the uncertainty of the TSI since 1610 reconstructed from sunspot data and the uncertainty of the evolution of the Earth’s magnetic dipole moment. The analysis of the distribution functions of the reconstructed irradiance for the last 3000 years, which is the period that the reconstructions overlap, indicates that the estimates based on the virtual axial dipole moment are significantly lower at earlier times than the reconstructions based on the virtual dipole moment. We also present a combined reconstruction, which represents our best estimate of total solar irradiance for any given time during the Holocene. Conclusions. We present the first physics-based reconstruction of the total solar irradiance over the Holocene, which will be of interest for studies of climate change over the last 11 500 years. The reconstruction indicates that the decadally averaged total solar irradiance ranges over approximately 1.5 W/m 2 from grand maxima to grand minima.
Massive young stellar objects in the N 66/NGC 346 region of the SMC

We present HK spectra of three sources located in the N 66 region of the Small Magellanic Cloud. The sources display prominent stellar Brγ and extended H2 emission, and exhibit infrared excesses at λ > 2 μm. Based on their spectral features, and photometric spectral energy distributions, we suggest that these sources are massive young stellar objects. The findings are interpreted as evidence of on-going high mass star formation in N 66.
A Recommendation Strategy Integrating Higher-Order Feature Interactions With Knowledge Graphs

Knowledge Graphs (KG) are efficient auxiliary information in recommender systems. However, in knowledge graph feature learning, a major objective is improvement for recommendation performance. One of the problems in the existing methods is that they cannot uncover the deep interaction information of users in a simple way, and this motivates effective learning of the potential embedded information through the knowledge graph. The Graph Convolutional Network (GCN) can be useful for learning information about graph structured data. This paper proposes a method that fuses higher order feature interactions and knowledge graphs and uses them for recommendation. For users, they uses Gated Recurrent Units (GRU) to focus on their preferences so that the ability of convolutional neural networks in processing user preference features is enhanced; for items, the cross-learning module is adopted to learn higher order features between items and entities; for users and entities, KG and user-item interaction information are combined followed by feature extraction of graph structured data by Light GCN, allowing the model to learn potential user-entity associations from the graph structured data. Current experiments on two real datasets show that the proposed model performs better than some recently developed models.
INFLUENCE OF THE AMBIENT SOLAR WIND FLOW ON THE PROPAGATION BEHAVIOR OF INTERPLANETARY CORONAL MASS EJECTIONS

We study three coronal mass ejection (CME)/interplanetary coronal mass ejection (ICME) events (2008 June 1–6, 2009 February 13–18, and 2010 April 3–5) tracked from Sun to 1 AU in remote-sensing observations of Solar Terrestrial Relations Observatory Heliospheric Imagers and in situ plasma and magnetic field measurements. We focus on the ICME propagation in interplanetary (IP) space that is governed by two forces: the propelling Lorentz force and the drag force. We address the question: which heliospheric distance range does the drag become dominant and the CME adjust to the solar wind flow. To this end, we analyze speed differences between ICMEs and the ambient solar wind flow as a function of distance. The evolution of the ambient solar wind flow is derived from ENLIL three-dimensional MHD model runs using different solar wind models, namely, Wang–Sheeley–Arge and MHD-Around-A-Sphere. Comparing the measured CME kinematics with the solar wind models, we find that the CME speed becomes adjusted to the solar wind speed at very different heliospheric distances in the three events under study: from below 30 R☉, to beyond 1 AU, depending on the CME and ambient solar wind characteristics. ENLIL can be used to derive important information about the overall structure of the background solar wind, providing more reliable results during times of low solar activity than during times of high solar activity. The results from this study enable us to obtain greater insight into the forces acting on CMEs over the IP space distance range, which is an important prerequisite for predicting their 1 AU transit times.
Formation of Wide-orbit Gas Giants Near the Stability Limit in Multi-stellar Systems

We have investigated the formation of a circumstellar wide-orbit gas giant planet in a multiple stellar system. We consider a model of orbital circularization for the core of a giant planet after it is scattered from an inner disk region by a more massive planet, which was proposed by Kikuchi et al. We extend their model for single star systems to binary (multiple) star systems, by taking into account tidal truncation of the protoplanetary gas disk by a binary companion. As an example, we consider a wide-orbit gas giant in a hierarchical triple system, HD131399Ab. The best-fit orbit of the planet is that with semimajor axis ∼80 au and eccentricity ∼0.35. As the binary separation is ∼350 au, it is very close to the stability limit, which is puzzling. With the original core location ∼20–30 au, the core (planet) mass ∼50 ME and the disk truncation radius ∼150 au, our model reproduces the best-fit orbit of HD131399Ab. We find that the orbit after the circularization is usually close to the stability limit against the perturbations from the binary companion, because the scattered core accretes gas from the truncated disk. Our conclusion can also be applied to wider or more compact binary systems if the separation is not too large and another planet with ≳20–30 Earth masses that scattered the core existed in inner region of the system.
Asymmetric exclusion model with several kinds of impurities

We formulate a new integrable asymmetric exclusion process with N − 1 = 0, 1, 2, … kinds of impurities and with hierarchically ordered dynamics. The model we proposed displays the full spectrum of the simple asymmetric exclusion model plus new levels. The first excited state belongs to these new levels and displays unusual scaling exponents. We conjecture that, while the simple asymmetric exclusion process without impurities belongs to the KPZ universality class with dynamical exponent , our model has a scaling exponent . In order to check the conjecture, we solve numerically the Bethe equation with N = 3 and N = 4 for the totally asymmetric diffusion and found the dynamical exponents and in these cases.
The young open cluster Trumpler 3

We present a photometric and spectroscopic study of the poorly investigated open cluster Trumpler 3. Basic parameters such as the age of 70 ± 10 Myr, the color excess E (B – V) = 0.30 ± 0.02 mag, the distance of 0.69 ± 0.03 kpc and the limiting radius of 12′ were redetermined and compared with previous preliminary studies. The distance of 0.65 ± 0.09 kpc was determined independently by spectral parallaxes. Simultaneously, our analysis allowed us to estimate a total number of members to be Ntot = 570 ± 90 and a total mass of the cluster to be Mtot = 270 ± 40 M⊙. We also determined a state of cluster's dynamical evolution. We conclude that Trumpler 3 is a young low-massive stellar ensemble with a typical mass function slope, located near to the outer edge of the Galaxy's Orion Spur. As a result of a wide-field search for short period variable stars, 24 variables were discovered in the cluster's area. Only one of them – a variable of the γ -Dor type – was found to be a likely cluster member (© 2010 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
The accretion of gas on to galaxies as traced by their satellites

We have compiled a large sample of isolated central galaxies from the Sloan Digital Sky Survey, which do not have a neighbour of comparable brightness within a projected distance of 1 Mpc. We use the colours, luminosities and surface brightnesses of satellite galaxies in the vicinity of these objects to estimate their neutral gas content and to derive the average total mass of H I gas contained in the satellites as a function of the projected radius from the primary. Recent calibrations of merging time-scales from N-body simulations are used to estimate the rate at which this gas will accrete on to the primary galaxies. Our estimated accretion rate falls short of that needed to maintain the observed level of star formation in the primaries by nearly two orders of magnitude. Nevertheless, there are strong correlations between the total mass of gas in satellites and the colours and specific star formation rates of primary galaxies of all stellar masses. The correlations are much weaker, if we consider the total stellar mass in satellites, rather than their total gas mass. We ask why star formation in the primaries should be correlated with gas contained in satellites at projected separations of an Mpc or more, well outside the virial radius of the dark matter haloes of these systems. We suggest that gas-rich satellites trace an underlying reservoir of ionized gas that is accreted continuously and that provides fuel for the ongoing star formation in galaxies in the local Universe.
Optimal Design of Convolutional Neural Network Architectures Using Teaching-Learning-Based Optimization for Image Classification

Convolutional neural networks (CNNs) have exhibited significant performance gains over conventional machine learning techniques in solving various real-life problems in computational intelligence fields, such as image classification. However, most existing CNN architectures were handcrafted from scratch and required significant amounts of problem domain knowledge from designers. A novel deep learning method abbreviated as TLBOCNN is proposed in this paper by leveraging the excellent global search ability of teaching–learning-based optimization (TLBO) to obtain an optimal design of network architecture for a CNN based on the given dataset with symmetrical distribution of each class of data samples. A variable-length encoding scheme is first introduced in TLBOCNN to represent each learner as a potential CNN architecture with different layer parameters. During the teacher phase, a new mainstream architecture computation scheme is designed to compute the mean parameter values of CNN architectures by considering the information encoded into the existing population members with variable lengths. The new mechanisms of determining the differences between two learners with variable lengths and updating their positions are also devised in both the teacher and learner phases to obtain new learners. Extensive simulation studies report that the proposed TLBOCNN achieves symmetrical performance in classifying the majority of MNIST-variant datasets, displays the highest accuracy, and produces CNN models with the lowest complexity levels compared to other state-of-the-art methods due to its promising search ability.
The Arecibo Galaxy Environment Survey – V. The Virgo cluster (I)

We present 21-cm observations of a 10 × 2 deg2 region in the Virgo cluster, obtained as part of the Arecibo Galaxy Environment Survey. 289 sources are detected over the full redshift range (−2000 < vhel < +20 000 km s−1) with 95 belonging to the cluster (vhel < 3000 km s−1). We combine our observations with data from the optically selected Virgo Cluster Catalogue (VCC) and the Sloan Digital Sky Survey. Most of our detections can be clearly associated with a unique optical counterpart, and 30 per cent of the cluster detections are new objects fainter than the VCC optical completeness limit. Seven detections may have no optical counterpart and we discuss the possible origins of these objects. Seven detections appear associated with early-type galaxies. We perform H i stacking on the H i-undetected galaxies listed in the VCC in this region and show that they must have significantly less gas than those actually detected in H i. Galaxies undetected in H i in the cluster appear to be really devoid of gas, in contrast to a sample of field galaxies from the Arecibo Legacy Fast ALFA (ALFALFA).
Warm absorber and truncated accretion disc in IRAS 05078+1626

Context. X-ray observations of unabsorbed active galactic nuclei provide an opportunity to explore the innermost regions of supermassive black hole accretion discs. Aims. Our goal in this paper is to investigate the central environment of a Seyfert 1.5 galaxy IRAS 05078+1626. Methods. We studied the time-averaged spectrum obtained with the EPIC and RGS instruments onboard XMM-Newton. Results. A power law continuum (photon index Γ � 1.75) dominates the 2‐10 keV energy range. A narrow iron K α spectral line is clearly seen, presumably originating in a distant torus, but no broad relativistic component was detected. However, the power law and the iron K α line alone do not provide a satisfactory fit in the soft X-ray band whose spectrum can be explained by the combination of three components: a) a cold photoelectric absorber with column density NH ≈ 10 21 cm −2 . This gas could be located either in outer parts of the accretion disc, at the rim of the torus or farther out in the host galaxy; b) a warm absorber with high ionization parameter (log ξ ≈ 2.2) and column density (NH ≈ 10 24 cm −2 ); c) an ionised reflection where the reflecting gas could be either in the inner wall of a warm absorber cone or in an ionised accretion disc. Conclusions. The first X-ray spectroscopic measurement of IRAS05078+1626 unveils some of the standard ingredients in Seyfert galaxies, such as a power law primary continuum, modified by reflection from the accretion disc and by the effect of complex, multiphase obscuration. However, data constrains the accretion disc, if present, not to extend closer than to 60 gravitational radii from the black hole.
Polymerization in the Borstar Polypropylene Hybrid Process: Combining Technology and Catalyst for Optimized Product Performance

Producing isotactic polypropylene (iPP) homo- and copolymers in a wide composition and property range according to customer demand requires perfect alignment between the process technology, catalyst system and polymer structure. The present review shows this for the Borstar® PP process, a hybrid process employing liquid bulk and gas phase stages, in an exemplary way. It starts with the process design and continues through two generations of Ziegler–Natta catalyst development history to the design of advanced multimodal random and multiphase copolymers. Essential elements of each of the three areas contributing to performance range are highlighted, and an outlook to future development is given.
THE FREQUENCY OF RAPID ROTATION AMONG K GIANT STARS

We present the results of a search for unusually rapidly rotating giant stars in a large sample of K giants (∼1300 stars) that had been spectroscopically monitored as potential targets for the Space Interferometry Mission's Astrometric Grid. The stars in this catalog are much fainter and typically more metal-poor than those of other catalogs of red giant star rotational velocities, but the spectra generally only have signal-to-noise ratio (S/N) of ∼20–60, making the measurement of the widths of individual lines difficult. To compensate for this, we have developed a cross-correlation method to derive rotational velocities in moderate S/N echelle spectra to efficiently probe this sample for rapid rotator candidates. We have discovered 28 new red giant rapid rotators as well as one extreme rapid rotator with a vsin i of 86.4 km s−1. Rapid rotators comprise 2.2% of our sample, which is consistent with other surveys of brighter, more metal-rich K giant stars. Although we find that the temperature distribution of rapid rotators is similar to that of the slow rotators, this may not be the case with the distributions of surface gravity and metallicity. The rapid rotators show a slight overabundance of low-gravity stars and as a group are significantly more metal-poor than the slow rotators, which may indicate that the rotators are tidally locked binaries.
Analysis of t tbar H Events at sqrt(s)=14 TeV with H -> WW

We study the process pp -> t tbar H at sqrt(s)=14 TeV where H -> WW. We focus on final states that include three or four leptons. Signal and background samples are generated at leading order (LO) and normalized to next-to-leading order (NLO) calculations. We employ the "Snowmass" detector simulation and event reconstruction. Cuts are selected which provide a substantial signal yield while suppressing the main backgrounds. Systematic uncertainties are estimated for the overall normalization of signal and background processes. With no improvement in the current theoretical uncertainties on sigma(t tbar H), we project a precision on a top quark Yukawa coupling of approximately 16% in 300 fb^-1 and 9% in 3000 fb^-1. If the theoretical uncertainties are halved, these improve to 14% and 6%, respectively.
Turbulent Couette Flow:An analytical solution

A simple analytical solution for turbulent plane Couette flow is obtained from a subset of the Navier-Stokes equations. This approach analyses the effect of the unsteady state Lagrangian diffusion of viscous momentum on the smoothed phase velocity. Three initial velocity profiles at the start of a turbulent wall cycle are considered. The predictions adequate identify the existence of three layers usually observed in turbulent flow fields, in particular a viscosity dominated wall layer and a log-law layer. Experimental measurements of time-averaged velocity are also well correlated. Key words: Couette flow, turbulent, attractors, analytical solution, Lagrangian partial derivative, time scale, initial conditions