Miracle-dz/UniFAR-FTUs huggingface dataset:
Effect of Nano Additive on Mechanical Properties of Natural Fiber Reinforced Soil

ABSTRACT Organic soil is a poor bearing medium and is susceptible to uncharacteristic volume change and settlement behavior. Geotechnical design of substructures in organic soil is often of high economic value to account for its weak geotechnical properties. Fiber reinforcement improves the strength of the soil. However, fibers act as a mechanical reinforcement in soil mass rather than enhancing the intrinsic nature of the soil. But chemical additives alter its behavior, thereby improving its strength. This study investigates the strength and hydraulic conductivity (HC) of low plastic organic silt reinforced with banana fiber and nano-silica. Banana fiber was added in dosages of 0.25%, 0.50%, 0.75% and 1%. The optimum fiber dosage was 0.75%. Nano-silica was added to the 0.75% banana fiber reinforced soil at dosages of 0.2%, 0.4%, 0.6% and 0.8% to improve the strength of the reinforced soil. The effect of aging on HC and unconfined compressive strength (UCS) was studied for a period of 90 d. Results showed that nano-silica and banana fiber beneficially complemented each other in the enhancement of geotechnical properties. Nano-silica increased the strength of fiber-reinforced soil, and banana fiber averted the brittle failure nature imposed by the nano-silica. Also, it improved drainage characteristics through aggregation action.
Relative competency of urea in augmenting physiological and agronomic traits of baby corn (Zea mays)

Nitrogen is indispensable for aggrandizing productivity of crop but the losses associated due to swift transformation and release pattern are subjected to various losses leading to pitiful amount left for crop uptake, pollution and resource wastage. Present study was conducted to evaluate the efficacy of coated urea and nitrogen rates on baby corn growth, yield and NUE. The experiment comprised varieties PHM-1 and HM-4, coated urea (NCU, ZCU, SCU and PU) and nitrogen levels @180, 150, 120 kg N/ha along with the control. The study revealed that PHM-1 obtained significantly higher plant height, no. of cobs and weight of dehusked cob that led to significant increase of 18.47 and 19.67 % higher husked and dehusked cob yields over HM-4 which attained 12.6% higher fodder yield over latter. The baby corn cob yield and fodder yield were significantly higher in coated urea over prilled urea. The husked and dehusked yield of baby corn was higher in neem-coated urea over prilled urea by 14.81 and 14.37% respectively. H o w e v e r , a reduction of 59.9% in total fodder yield was recorded in control when compared to 180 kg N ha. Also, NPK uptake was higher then PHM-1 and uptake by coated urea was higher then prilled urea along with high uptake for 180 kg N/ha, further the AE and higher PE of baby corn cob was found highest in variety PHM-1 although for fodder, the higher AE was recorded in HM-4, whereas ANR was higher in PHM-1.
Hubble Space Telescope WFPC2 Color-Magnitude Diagrams for Globular Clusters in M31

We report new photometry for 10 globular clusters in M31, observed to a uniform depth of four orbits in F555W (V) and F814W (I) using WFPC2 on board the Hubble Space Telescope (HST). In addition, we have reanalyzed HST archival data of comparable quality for two more clusters. A special feature of our analysis is the extraordinary care taken to account for the effects of blended stellar images and the required subtraction of contamination from the field stellar populations in M31 in which the clusters are embedded. We thus reach 1 mag fainter than the horizontal branch (HB), even in unfavorable cases. We also show that an apparent peculiar steep slope of the HB for those clusters with blue HB stars is actually due to blends between blue HB stars and red giants. We present the color-magnitude diagrams (CMDs) and discuss their main features in comparison with the properties of the Galactic globular clusters. This analysis is augmented with CMDs previously obtained and discussed on eight other M31 clusters. We report the following significant results: (1) The loci of the red giant branches give reliable photometric metallicity determinations that generally compare very well with ground-based integrated spectroscopic and photometric measures, as well as giving good reddening estimates. (2) The HB morphologies follow the same behavior with metallicity as the Galactic globular clusters, with indications that the second-parameter effect can be present in some clusters of our sample. However, at [Fe/H] =∼ -1.7 we observe a number of clusters with red HB morphology such that the HB type versus [Fe/H] relationship is offset from that of the Milky Way (MW) and resembles that of the Fornax dwarf spheroidal galaxy. One explanation for the offset is that the most metal-poor M31 globular clusters are younger than their MW counterparts by 1–2 Gyr; further study is required. (3) The MV(HB) versus [Fe/H] relationship has been redetermined, and the slope (∼0.20) is very similar to the values derived from RR Lyrae stars in the MW and the LMC. The zero point of this relation (MV = 0.51 at [Fe/H] = -1.5) is based on the assumed distance modulus (m - M)0(M31) = 24.47 ± 0.03, and is consistent with the distance scale that places the LMC at (m - M)0(LMC) = 18.55.
Carnegie Supernova Project-II: Extending the Near-infrared Hubble Diagram for Type Ia Supernovae to z ∼ 0.1

The Carnegie Supernova Project-II (CSP-II) was an NSF-funded, four-year program to obtain optical and near-infrared observations of a “Cosmology” sample of ∼100 Type Ia supernovae located in the smooth Hubble flow (0.03 ≲ z ≲ 0.10). Light curves were also obtained of a “Physics” sample composed of 90 nearby Type Ia supernovae at z ≤ 0.04 selected for near-infrared spectroscopic timeseries observations. The primary emphasis of the CSP-II is to use the combination of optical and near-infrared photometry to achieve a distance precision of better than 5%. In this paper, details of the supernova sample, the observational strategy, and the characteristics of the photometric data are provided. In a companion paper, the near-infrared spectroscopy component of the project is presented.
On the possibilities of distinguishing Dirac from Majorana neutrinos

The problem if existing neutrinos are Dirac or Majorana particles is considered in a very pedagogical way. After a few historical remarks we recall the theoretical description of neutral spin 1/2 particles, emphasizing the difference between chirality and helicity which is important in our discussion. Next we describe the properties of neutrinos in the cases when their interactions are given by the standard model and by its extensions (massive neutrinos, right-handed currents, electromagnetic neutrino interaction, interaction with scalar particles). Various processes where the different nature of neutrinos could in principle be visible are reviewed. We clear up misunderstandings which have appeared in last suggestions how to distinguish both types of neutrinos.
Quantum field theory of a hyper-complex scalar field on a commutative ring

Inspired by the structural unification of unitary groups (quantum field theory) with orthogonal groups (relativity) proposed recently through a non-division algebra, we construct a hypercomplex field theory with an internal symmetry that unifies the U(1) compact gauge group with the SO(1,1) noncompact gauge group, using the commutative ring of hypercomplex numbers. From the quantum field theory point of view, the hypercomplex field encodes two charged bosons with opposite charge, and corresponds thus to a neutral compound boson. Furthermore, normal or- dering of operators is not required for controling the vacuum divergences; in an analogy with SUSY, the theory under study contains U(1) boson particles and their hyperbolic SO(1,1) boson partners, whose contributions to the vacuum energy cancel out exactly to a zero value. In fact the present scheme allows us to compare finite measuments of squeezed boson-number statistics obtained with and without normal ordering. Additionally we discuss on the potential applications of the squeezed boson states constructed on the commutative ring, in quantum teleportation and in related areas.
First-order mean motion resonances in two-planet systems: general analysis and observed systems

This paper focuses on two-planet systems in a first-order $(q+1):q$ mean motion resonance and undergoing type-I migration in a disc. We present a detailed analysis of the resonance valid for any value of $q$. Expressions for the equilibrium eccentricities, mean motions and departure from exact resonance are derived in the case of smooth convergent migration. We show that this departure, not assumed to be small, is such that period ratio normally exceeds, but can also be less than, $ (q+1)/q. $ Departure from exact resonance as a function of time for systems starting in resonance and undergoing divergent migration is also calculated. We discuss observed systems in which two low mass planets are close to a first-order resonance. We argue that the data are consistent with only a small fraction of the systems having been captured in resonance. Furthermore, when capture does happen, it is not in general during smooth convergent migration through the disc but after the planets reach the disc inner parts. We show that although resonances may be disrupted when the inner planet enters a central cavity, this alone cannot explain the spread of observed separations. Disruption is found to result in either the system moving interior to the resonance by a few percent, or attaining another resonance. We postulate two populations of low mass planets: a small one for which extensive smooth migration has occurred, and a larger one that formed approximately in-situ with very limited migration.
Random times at which insiders can have free lunches

We consider models of time continuous financial markets with a regular trader and an insider who are able to invest into one risky asset. The insider's additional knowledge consists in his ability to stop at a random time which is inaccessible to the regular trader, such as the last passage of a certain level before maturity by some stock price process, or the time at which the stock price reaches its maximum during the trading interval. We show that under very mild assumptions on the coefficients of the diffusion process describing these price processes the information drift caused by the additional knowledge of the insider cannot be eliminated by an equivalent change of probability measure. As a consequence, all our models allow the insider to have free lunches with vanishing risk, or even to exercise arbitrage.
Multiple Stellar Populations of Globular Clusters from Homogeneous Ca-CN Photometry. II. M5 (NGC 5904) and a New Filter System

Using our ingeniously designed new filter systems, we investigate multiple stellar populations of the red giant branch (RGB) and the asymptotic giant branch (AGB) in the globular cluster (GC) M5. Our results are the following. (1) Our index accurately traces nitrogen abundances in M5, while other color indices fail to do so. (2) We find bimodal CN distributions in both RGB and AGB sequences, with number ratios between CN-weak (CN-w) and CN-strong (CN-s) of n(CN-w):n(CN-s) = 29:71 (±2) and 21:79 (±7), respectively. (3) We also find a bimodal photometric [N/Fe] distribution for M5 RGB stars. (4) Our –[O/Fe] and –[Na/Fe] relations show clear discontinuities between the two RGB populations. (5) Although small, the RGB bump of CN-s is slightly brighter, = 0.07 ± 0.04 mag. If real, the difference in the helium abundance becomes = 0.028 ± 0.016, in the sense that CN-s is more helium enhanced. (6) Very similar radial but different spatial distributions with comparable center positions are found for the two RGB populations. The CN-s RGB and AGB stars are more elongated along the NW–SE direction. (7) The CN-s population shows a substantial net projected rotation, while that of the CN-w population is nil. (8) Our results confirm the deficiency of CN-w AGB stars previously noted by others. We show that it is most likely due to stochastic truncation in the outer part of the cluster. Finally, we discuss the formation scenario of M5.
Study of the fluvial activity on Mars through mapping, sediment transport modelling and spectroscopic analyses

Mars is the only planet, other than Earth, for which there are several evidences that liquid water was abundant at the surface. Among them, one of the best evidence is that the ancient terrains of Mars are covered with fluvial and lacustrine features such as valley networks, longitudinal valleys and basin lakes. In addition, spectroscopic data have shown the widespread presence of aqueous alteration minerals on the Martian surface, including clays composed by phyllosilicates and hydrated salts. The main subject of my PhD is the study of these specific features (such as valley networks and paleolakes) on Mars surface, both from the geological and spectroscopic point of view through mapping, sediment transport modelling and CRISM spectra analyses. There are, in fact, no doubts that these structures were carved by liquid water, but several questions remain about the mechanisms of their formation and the climatic conditions under which this formation occurred. In this context, the study of these structures along with the identification of hydrated minerals, are a key in the investigation of the past climatic conditions of the planet which can have, in turn, important astrobiological implications. I updated previous global maps of Martian valleys using a new photomosaic of the Martian surface and data at higher resolution with respect to those used in the previous works. Furthermore, I selected a subset of the mapped valleys which includes 63 large fluvial systems and evaluated their formation timescales on the basis of sediment transport modelling. In addition, analyses of CRISM spectral data were performed on a sample of open/closed basin lakes (associated with the mapped valleys) detecting the possible presence of hydrated minerals, in particular (Fe/Mg-smectite), sometimes in association with mafic materials (olivine).
Model of Energy Spectrum Parameters of Ground Level Enhancement Events in Solar Cycle 23

Mewaldt et al. (2012) fitted the observations of the ground level enhancement (GLE) events during solar cycle 23 to the double power law equation to obtain the four spectral parameters, the normalization constant C, low‐energy power law slope γ1, high‐energy power law slope γ2, and break energy E0. There are 16 GLEs from which we select 13 for study by excluding some events with complicated situation. We analyze the four parameters with conditions of the corresponding solar events. According to solar event conditions, we divide the GLEs into two groups, one with strong acceleration by interplanetary shocks and another one without strong acceleration. By fitting the four parameters with solar event conditions we obtain models of the parameters for the two groups of GLEs separately. Therefore, we establish a model of energy spectrum of solar cycle 23 GLEs, which may be used in prediction in the future.
Superconducting properties of nanocrystalline MgB2 thin films made by an in situ annealing process

We have studied the structural and superconducting properties of MgB2 thin films made by pulsed-laser deposition followed by in situ annealing. The cross-sectional transmission electron microscopy reveals a nanocrystalline mixture of textured MgO and MgB2 with very small grain sizes. A zero-resistance transition temperature (Tc0) of 34 K and a zero-field critical current density (Jc) of 1.3×106 A/cm2 were obtained. The irreversibility field was ∼8 T at low temperatures, although severe pinning instability was observed. The result is a step towards making the in situ deposition process a viable technique for MgB2 Josephson junction technologies.
Minimality and deadlockness of multitape automata

Abstract We consider the class M of deterministic binary two-tape automata for which those states of the automaton where reading from the additional second tape is implemented permit to continue the calculation only in the case where the read symbol is fixed in advance for all automata. For the automata of the class M, the so-called generalised minimisation problem is considered. This problem consists in finding all automata which are minimal in the number of states in any class of equivalent automata of M. In the paper, the decidability of the generalised minimisation problem in M is proved and a procedure to solve this problem is described and analysed.
Revealing structure and evolution within the corona of the Seyfert galaxy I Zw 1

X-ray spectral timing analysis is presented of XMM-Newton observations of the narrow line Seyfert 1 galaxy I Zwicky 1 (I Zw 1) taken in 2015 January. After exploring the effect of background flaring on timing analyses, X-ray time lags between the reflection-dominated 0.3-1.0keV energy and continuum-dominated 1.0-4.0keV band are measured, indicative of reverberation off the inner accretion disc. The reverberation lag time is seen to vary as a step function in frequency; across lower frequency components of the variability, 3e-4 to 1.2e-3Hz a lag of 160s is measured, but the lag shortens to (59 +/- 4)s above 1.2e-3Hz. The lag-energy spectrum reveals differing profiles between these ranges with a change in the dip showing the earliest arriving photons. The low frequency signal indicates reverberation of X-rays emitted from a corona extended at low height over the disc while at high frequencies, variability is generated in a collimated core of the corona through which luminosity fluctuations propagate upwards. Principal component analysis of the variability supports this interpretation, showing uncorrelated variation in the spectral slope of two power law continuum components. The distinct evolution of the two components of the corona is seen as a flare passes inwards from the extended to the collimated portion. An increase in variability in the extended corona was found preceding the initial increase in X-ray flux. Variability from the extended corona was seen to die away as the flare passed into the collimated core leading to a second sharper increase in the X-ray count rate.
The imprints of AGN feedback within a supermassive black hole's sphere of influence

We present a new 300 ks Chandra observation of M87 that limits pileup to only a few per cent of photon events and maps the hot gas properties closer to the nucleus than has previously been possible. Within the supermassive black hole's gravitational sphere of influence, the hot gas is multiphase and spans temperatures from 0.2 to 1 keV. The radiative cooling time of the lowest temperature gas drops to only 0.1-0.5 Myr, which is comparable to its free fall time. Whilst the temperature structure is remarkably symmetric about the nucleus, the density gradient is steep in sectors to the N and S, with $\rho{\propto}r^{-1.5\pm0.1}$, and significantly shallower along the jet axis to the E, where $\rho{\propto}r^{-0.93\pm0.07}$. The density structure within the Bondi radius is therefore consistent with steady inflows perpendicular to the jet axis and an outflow directed E along the jet axis. By putting limits on the radial flow speed, we rule out Bondi accretion on the scale resolved at the Bondi radius. We show that deprojected spectra extracted within the Bondi radius can be equivalently fit with only a single cooling flow model, where gas cools from 1.5 keV down below 0.1 keV at a rate of 0.03 M$_{\odot}$/yr. For the alternative multi-temperature spectral fits, the emission measures for each temperature component are also consistent with a cooling flow model. The lowest temperature and most rapidly cooling gas in M87 is therefore located at the smallest radii at ~100 pc and may form a mini cooling flow. If this cooling gas has some angular momentum, it will feed into the cold gas disk around the nucleus, which has a radius of ~80 pc and therefore lies just inside the observed transition in the hot gas structure.
Phase Diagram of Bilayer Composite Fermion States

Department of Physics, 104 Davey Laboratory, The Pennsylvania State University, University Park, Pennsylvania 16802(February 1, 2008)We construct a class of composite fermion states for bilayer electron systems in a strong transversemagnetic ﬁeld, and determine quantitatively the phase diagram as a function of the layer separation,layer thickness, and electron density. We ﬁnd, in general, that there are several transitions, andthat the incompressible phases are separated by compressible ones. The paired states of compositefermions, described by Pfaﬃan wave functions, are also considered.71. 10.Pm,73.43. -fI. INTRODUCTION
Subgroups of Bianchi groups and arithmetic quotients of hyperbolic 3-space

Let O be the ring of integers in an imaginary quadratic number-field. The group PSL 2 (O) acts discontinuously on hyperbolic 3-space H. If Γ ≤ PSL 2 (O) is a torsionfree subgroup of finite index then the manifold Γ\H can be compactified to a manifold M Γ so that the inclusion Γ\H ≤ M Γ is a homotopy equivalence. M Γ is a compact with boundary. The boundary being a union of finitely many 2-tori. This paper contains a computer-aided study of subgroups of low index in PSL 2 (O) for various O. The explicit description of these subgroups leads to a study of the homeomorphism types of the M Γ
Infrared probe of the anomalous magnetotransport of highly oriented pyrolytic graphite in the extreme quantum limit

We present a systematic investigation of the magnetoreflectance R ,B of highly oriented pyrolytic graphite in magnetic field B up to 18 T. From these measurements, we report the determination of lifetimes associated with the lowest Landau levels in the quantum limit. We find a linear field dependence for inverse lifetime 1 /B of the lowest Landau levels, which is consistent with the hypothesis of a three-dimensional 3D to 1D crossover in an anisotropic 3D metal in the quantum limit. This enigmatic result uncovers the origin of the anomalous linear in-plane magnetoresistance observed both in bulk graphite and recently in mesoscopic graphite samples.
The Planck Scale Underpinning for Space Time

We provide a rationale for the Planck scale being the minimum scale in the universe, as also its speciﬁc numerical values. In the process we answer the question of why the Planck scale is 10 20 times the Compton scale of elementary particles. These considerations show how the Planck scale provides an underpinning for space time.
Stacked lensing estimators and their covariance matrices: excess surface mass density versus lensing shear

Stacked lensing is a powerful means of measuring the average mass distribution around large-scale structure tracers. There are two stacked lensing estimators used in the literature, denoted as $\Delta\Sigma$ and $\gamma_+$, which are related as $\Delta\Sigma=\Sigma_{\rm cr}\gamma_+$ on each lens-source pair basis, where $\Sigma_{\rm cr}(z_l,z_s)$ is the critical surface mass density for lens and source at redshifts $z_l$ and $z_s$, respectively. In this paper we derive a formula for the covariance matrix of $\Delta\Sigma$-estimator focusing on "weight" function to improve the signal-to-noise ($S/N$), where we assume that the lensing fields and the distribution of lensing objects obey the Gaussian statistics. With this formula, we show that, if background galaxy shapes are weighted by an amount of $\Sigma_{\rm cr}^{-2}(z_l,z_s)$, the $\Delta\Sigma$-estimator is optimal (it maximizes the $S/N$) in the shot noise limited regime. We validate the covariance formula by using numerical simulations. We show that the $\Delta\Sigma$-estimator with the weight $\Sigma_{\rm cr}^{-2}$ gives a greater $(S/N)^2$ than that of the $\gamma_+$-estimator by about 5--25\% for lensing objects at redshifts comparable with or higher than the median of source galaxy redshifts for hypothetical Subaru HSC and DES surveys. However, for low-redshift lenses such as $z_l 2$. Our formula allows one to explore how the combination of the different estimators can approach an optimal estimator in all regimes of redshifts and separation scales.