Miracle-dz/UniFAR-FTUs huggingface dataset:
Religion in the labor market: evidence from India

ABSTRACT In this paper, we analyse the education and wage gaps between Hindus and Muslims over the period 1983 to 2011–2012 in India. We find that Muslims are worse off than Hindus in terms of education and this disadvantage has increased over time. Our analysis shows that the wage gap is more pronounced at the higher end of the wage distribution which we interpret as a glass ceiling effect. We find that the wage gap has increased over time and the increase is more pronounced at the upper quantiles. Our decomposition analysis shows that difference in education has a significant contribution to the Hindu-Muslim wage gap. We find that the Hindu-Muslim gaps are more pronounced in urban areas relative to rural areas. Comparing Muslims with different Hindu castes, we find that while the disadvantaged castes have improved their condition relative to Muslims over time, the condition of Muslims relative to the advantaged castes has worsened. Dividing the sample into younger (aged 16–35) and older (36–65) cohorts, we find that the Hindu-Muslim gap in education is more acute in the younger cohort while the Hindu-Muslim wage gap is more pronounced for the older cohort.
Compressed sensing in the quaternion algebra

The article concerns compressed sensing methods in the quaternion algebra. We prove that it is possible to uniquely reconstruct - by $\ell_1$-norm minimization - a sparse quaternion signal from a limited number of its linear measurements, provided the quaternion measurement matrix satisfies so-called restricted isometry property with a sufficiently small constant. We also provide error estimates for the reconstruction of a non-sparse quaternion signal in the noisy and noiseless cases.
Weak Convergence of a Seasonally Forced Stochastic Epidemic Model

In this study we extend the results of Kurtz (1970,1971) to show the weak convergence of epidemic processes that include explicit time dependence, specifically where the transmission parameter,$\beta(t)$, carries a time dependency. We first show that when population size goes to infinity, the time inhomogeneous process converges weakly to the solution of the mean-field ODE. Our second result is that, under proper scaling, the central limit type fluctuations converge to a diffusion process.
Anomalous valley magnetic moment of graphene

Carrier interactions on graphene are studied. The study shows that besides the well-known Coulomb repulsion between carriers, there also exist four-fermion interactions associated with the U-process, one of which attracts carriers in different valleys. We then calculate the contributions to the valley magnetic moment from vertex corrections and from four-fermion corrections explicitly. The relative contributions are - 18% and 3%, respectively. Lastly we point out that we can mimic the heavy-quarkonium system by carrier interactions in graphene.
Results of Long-Baseline Neutrino Experiments Based on the Consideration of Frameworks

In this paper, we present an analysis of the outcomes of long-baseline neutrino experiments based on the consideration of frameworks. Our analysis suggests that the time difference between the time-of-flights corresponding to the speed of light (in vacuum) and that of the neutrino from a source to a detector is within the range of our predicted time difference assuming that the speed of neutrino follows a Galilean transformation. As the ghostly particles called neutrinos have peculiar properties which are still unresolved, so we propose measurements need to be performed at different times of the day to test any diurnal variations (if possible then any annual variations) due to the movement of the Earth.
Parabolic smoothing effect and local well-posedness of fifth order semilinear dispersive equations on the torus

We consider the Cauchy problem of fifth order dispersive equations on the torus. We assume that the initial data is sufficiently smooth and the nonlinear term is a polynomial depending on $\partial_x^3 u, \partial_x^2 u, \partial_x u$ and $u$. We prove that the local well-posedness holds on $[-T,T]$ when the nonlinear term satisfies a condition and otherwise, the local well-posedness holds with a smoothing effect only on either $[0,T]$ or $[-T,0]$ and nonexistence result holds on the other time interval, which means that the nonlinear term can not be treated as a perturbation of the linear part and the equation has a property of parabolic equations by an influence of the nonlinear term. As a corollary, we also have the same results for $(2j+1)$-st order dispersive equations.
Mobile communication on post-partum minor health alignments’ recovery and family planning seeking care among primiparous

Background: Coverage and quality of postnatal care for women and newborns tend to be relatively poor especially with COVID-19 outbreaks and length of stay in the health facility has shortened resulting in limited knowledge and skills of the postnatal homecare as well as family planning seeking care. With the development of communication technology, the maternity nurse becomes able to provide postpartum health teaching for enriching women with information to be able to deal with postpartum minor health alignments and timely family planning seeking care, also minimize the risk of infection caused by face-to-face follow up. Aim: The current study aimed to assess the impact of mobile communication on post-partum minor health alignments’ recovery and family planning seeking care among primiparous. Design: A quasi- experimental (Intervention /Control)) research design was used. Setting: This study was carried out in Obstetric and Gynecological Inpatient Wards and Labor and childbirth unit at Beni-Suef University Hospitals, Study subjects: A non-probability purposive sample of 119 primiparous mothers who were fulfilling the criteria. Tools: A structured interviewing questionnaire to conceal the data related to socio- demographic characteristics and mother’s knowledge about postpartum minor health alignments and family planning seeking care, follow up card and satisfaction Likert scale.
Superconducting gap in LiFeAs from three-dimensional spin-fluctuation pairing calculations

The lack of nesting of the electron and hole Fermi-surface sheets in the Fe-based superconductor LiFeAs, with a critical temperature of 18 K, has led to questions as to whether the origin of superconductivity in this material might be different from other Fe-based superconductors. Both angle-resolved photoemission and quasiparticle interference experiments have reported fully gapped superconducting order parameters with significant anisotropy. The system is also of interest because relatively strong correlations seem to be responsible for significant renormalization of the hole bands. Here we present calculations of the superconducting gap and pairing in the random-phase approximation using Fermi surfaces derived from measured photoemission spectra. The qualitative features of the gaps obtained in these calculations are shown to be different from previous two-dimensional theoretical works, and in good agreement with experiment on the main Fermi surface pockets. We analyze the contributions to the pairing vertex thus obtained and show that the scattering processes between electron and hole pockets that are believed to dominate the pairing in other Fe-based superconductors continue to do so in LiFeAs despite the lack of nesting, leading to gaps with anisotropic $s_\pm$ structure. Some interesting differences relating to the enhanced $d_{xy}$ orbital content of the LiFeAs Fermi surface are noted.
Larotrectinib in NTRK Fusion-Positive High-Grade Glioneuronal Tumor: A Case Report

Glioneuronal tumors are rare central nervous system tumors with heterogeneous histological and molecular features. While the majority are low grade, a small percentage can behave aggressively. Due to the rarity of these tumors, there is no consensus on how to treat high-grade glioneuronal tumors, and they are often managed similarly to glial tumors. With the advent of molecular profiling, management decisions are increasingly determined by molecular alterations in the tumor rather than the tumor type, which can be a useful approach for tumor types that do not have robust supportive clinical trial data due to low prevalence. We present a case of an 18-year-old patient with a high-grade glioneuronal neoplasm initially treated with craniospinal irradiation, vincristine, and cyclophosphamide. He presented eight years later with a recurrent tumor and was found to be positive for MEF2D-NTRK1 fusion. He was treated with surgical resection and postoperative intensity-modulated radiation therapy (IMRT; 55.8 Gy) with concurrent temozolomide, followed by the NTRK inhibitor larotrectinib. He achieved a radiographic response, with a decrease in residual enhancement and radiographic improvement over the course of treatment. He remained in clinical and radiographic remission for six months. This demonstrates the successful treatment of a high-grade glioneuronal NTRK fusion-positive tumor with larotrectinib, which has only been previously reported once in the literature.
Diagnostics of plasma photoemission at strong coupling

We compute the spectrum of photons emitted by the finite-temperature large-N SU(N) ${\cal {N}}=4$ supersymmetric Yang-Mills plasma coupled to electromagnetism, at strong yet finite 't Hooft coupling. We work in the holographic dual description, extended by the inclusion of the full set of ${\cal{O}}(\alpha'^3)$ type IIB string theory operators that correct the minimal supergravity action. We find that, as the t' Hooft coupling decreases, the peak of the spectrum increases, and the momentum of maximal emission shifts towards the infra-red, as expected from weak-coupling computations. The total number of emitted photons also increases as the 't Hooft coupling weakens.
SUPERNOVA REMNANT PROGENITOR MASSES IN M31

Using Hubble Space Telescope photometry, we age-date 59 supernova remnants (SNRs) in the spiral galaxy M31 and use these ages to estimate zero-age main-sequence masses (MZAMS) for their progenitors. To accomplish this, we create color–magnitude diagrams (CMDs) and employ CMD fitting to measure the recent star formation history of the regions surrounding cataloged SNR sites. We identify any young coeval population that likely produced the progenitor star, then assign an age and uncertainty to that population. Application of stellar evolution models allows us to infer the MZAMS from this age. Because our technique is not contingent on identification or precise location of the progenitor star, it can be applied to the location of any known SNRs. We identify significant young star formation around 53 of the 59 SNRs and assign progenitor masses to these, representing a factor of ∼2 increase over currently measured progenitor masses. We consider the remaining six SNRs as either probable Type Ia candidates or the result of core-collapse progenitors that have escaped their birth sites. In general, the distribution of recovered progenitor masses is bottom-heavy, showing a paucity of the most massive stars. If we assume a single power-law distribution, dN/dM∝Mα, then we find a distribution that is steeper than a Salpeter initial mass function (IMF) (α = −2.35). In particular, we find values of α outside the range −2.7 ⩾ α ⩾ −4.4 to be inconsistent with our measured distribution at 95% confidence. If instead we assume a distribution that follows a Salpeter IMF up to some maximum mass, then we find that values of MMax > 26 are inconsistent with the measured distribution at 95% confidence. In either scenario, the data suggest that some fraction of massive stars may not explode. The result is preliminary and requires more SNRs and further analysis. In addition, we use our distribution to estimate a minimum mass for core collapse between 7.0 and 7.8 M☉.
On the Fundamentals of the Three-dimensional Translation Gauge Theory of Dislocations

We propose a dynamical version of the three-dimensional translation gauge theory of dislocations. In our approach, we use the notions of dislocation density and dislocation current tensors as the translational field strengths and define corresponding response quantities (pseudomoment stress and dislocation momentum flux). For the equations of motion for dislocations, we derive a closed system of field equations in an elegant quasi-Maxwellian form. The dynamical Peach— Koehler force density is derived in this framework as well. Finally, we discuss the similarities and differences between Maxwell field theory and the dislocation gauge theory developed here.
Pulsations as a driver for LBV variability

Among the most spectacular variable stars are the Luminous Blue Variables (LBVs), which can show three types of variability. The LBV phase of evolution is poorly understood, and the driving mechanisms for the variability are not known. The most common type of variability, the S Dor instability, occurs on timescales of tens of years. During an S Dor outburst, the visual magnitude of the star increases, while the bolometric magnitude stays approximately constant. In this work, we investigate pulsation as a possible trigger for the S Dor type outbursts. We calculate the pulsations of envelope models using a nonlinear hydrodynamics code including a time-dependent convection treatment. We initialize the pulsation in the hydrodynamic model based on linear non-adiabatic calculations. Pulsation properties for a full grid of models from 20 to 85 M$_{\odot}$ were calculated, and in this paper we focus on the few models that show either long-period pulsations or outburst-like behaviour, with photospheric radial velocities reaching 70-80 km/s. At the present time, our models cannot follow mass loss, so once the outburst event begins, our simulations are terminated. Our results show that pulsations alone are not able to drive enough surface expansion to eject the outer layers. However, the outbursts and long-period pulsations discussed here produce large variations in effective temperature and luminosity, which are expected to produce large variations in the radiatively driven mass-loss rates.
THE Onfp CLASS IN THE MAGELLANIC CLOUDS

The Onfp class of rotationally broadened, hot spectra was defined some time ago in the Galaxy, where its membership to date numbers only eight. The principal defining characteristic is a broad, centrally reversed He ii λ 4686 emission profile; other emission and absorption lines are also rotationally broadened. Recent surveys in the Magellanic Clouds (MCs) have brought the class membership there, including some related spectra, to 28. We present a survey of the spectral morphology and rotational velocities, as a first step toward elucidating the nature of this class. Evolved, rapidly rotating hot stars are not expected theoretically, because the stellar winds should brake the rotation. Luminosity classification of these spectra is not possible, because the principal criterion (He ii λ4686) is peculiar; however, the MCs provide reliable absolute magnitudes, which show that they span the entire range from dwarfs to supergiants. The Onfp line-broadening distribution is distinct and shifted toward larger values from those of normal O dwarfs and supergiants with >99.99% confidence. All cases with multiple observations show line-profile variations, which even remove some objects from the class temporarily. Some of them are spectroscopic binaries; it is possible that the peculiar profiles may have multiple causes among different objects. The origin and future of these stars are intriguing; for instance, they could be stellar mergers and/or gamma-ray-burst progenitors.
Detecting Exomoons via Doppler Monitoring of Directly Imaged Exoplanets

Teachey et al. recently reported the detection of a candidate exomoon, tentatively designated Kepler-1625b I, around a giant planet in the Kepler field. The candidate exomoon would be about the size and mass of Neptune, considerably larger than any moon in our solar system, and if confirmed, would be the first in a new class of giant moons or binary planets. Motivated by the large mass ratio in the Kepler-1625b planet and satellite system, we investigate the detectability of similarly massive exomoons around directly imaged exoplanets via Doppler spectroscopy. The candidate moon around Kepler-1625b would induce a radial velocity (RV) signal of about 200 on its host planet, large enough that similar moons around directly imaged planets orbiting bright, nearby stars might be detected with current or next generation instrumentation. In addition to searching for exomoons, an RV survey of directly imaged planets could reveal the orientations of the planets’ spin axes, making it possible to identify Uranus analogs.
Efficiently Exploring Ordering Problems through Conflict-directed Search

In planning and scheduling, solving problems with both state and temporal constraints is hard since these constraints may be highly coupled. Judicious orderings of events enable solvers to efficiently make decisions over sequences of actions to satisfy complex hybrid specifications. The ordering problem is thus fundamental to planning. Promising recent works have explored the ordering problem as search, incorporating a special tree structure for efficiency. However, such approaches only reason over partial order specifications. Having observed that an ordering is inconsistent with respect to underlying constraints, prior works do not exploit the tree structure to efficiently generate orderings that resolve the inconsistency. In this paper, we present Conflict-directed Incremental Total Ordering (CDITO), a conflict-directed search method to incrementally and systematically generate event total orders given ordering relations and conflicts returned by sub-solvers. Due to its ability to reason over conflicts, CDITO is much more efficient than Incremental Total Ordering. We demonstrate this by benchmarking on temporal network configuration problems that involve routing network flows and allocating bandwidth resources over time.
ORBITAL AND SPIN PARAMETER VARIATIONS OF PARTIAL ECLIPSING LOW MASS X-RAY BINARY X 1822-371

We report our measurements for the orbital and spin parameters of X 1822-371 using its X-ray partial eclipsing profile and pulsar timing from data collected by the Rossi X-ray Timing Explorer (RXTE). Four more X-ray eclipse times obtained by the RXTE 2011 observations were combined with historical records to trace the evolution of the orbital period. We found that a cubic ephemeris likely better describes the evolution of the X-ray eclipse times during a time span of about 34 years with a marginal second order derivative of s−1. Using the pulse arrival time delay technique, the orbital and spin parameters were obtained from RXTE observations from 1998 to 2011. The detected pulse periods show that the neutron star in X 1822-371 is continuously spun-up with a rate of s s−1. Although the evolution of the epoch of the mean longitude l = π/2 (i.e., Tπ/2) gives an orbital period derivative value consistent with that obtained from the quadratic ephemeris evaluated from the X-ray eclipse, the detected Tπ/2 values are significantly and systematically earlier than the corresponding expected X-ray eclipse times by 90 ± 11 s. This deviation is probably caused by asymmetric X-ray emissions. We also attempted to constrain the mass and radius of the neutron star using the spin period change rate and concluded that the intrinsic luminosity of X 1822-371 is likely more than 1038 erg s−1.
Spherically symmetric charged-dS solution in $f(T)$ gravity theories

A tetrad field with spherical symmetry is applied to the charged field equations of $f(T)$ gravity theory. A special spherically-symmetric charged-dS solution is obtained. The scalar torsion of this solution is a vanishing quantity. The spacetime of the derived solution is rewritten as a multiplication of three matrices: The first matrix is a special case of Euler$'$s angle "so(3)", the second matrix represents a boost transformation, while the third matrix is the square root of the spherically-symmetric charged-dS metric. It is shown that the boost matrix is important because it plays an essential role in adjusting the spacetime to become a solution for $f(T)$ theory.
ELASTOGRAPHY IN TA TIGHTNESS TO EVALUATE MUSCLE PHYSIOLOGY – A DIAGNOSTIC APPROACH

Shear wave elastography is useful for treating the musculoskeletal system. This drug is used to treat tendonitis, ligamentitis, and muscle pain. In the human body, the Achilles tendon is the strongest. The quantity and incidence of Achilles tendon overuse injuries and total ruptures in developed countries has increased in recent decades, owing to the fact that most Achilles tendon injuries occur in sports and there has been a general increase in sporting activity. Tendinopathy is the most common clinical diagnosis for Achilles tendon overuseinjuries, and it is marked by pain and swelling in the Achilles tendon, as well as an inability to engage in strenuous activities. Nonoperative treatment is helpful for the majority of people with Achilles tendon injuries, and those who do not respond to nonoperative treatment require surgery. In sports that demand jumping, running, and fast turns, a complete rupture of the Achilles tendon is common. Blue, green, and yellow/red are the color associated with rigid, intermediate, and soft tissue, respectively.Colour mapping will help us in rehabilitation .
Symmetry-breaking instability of leapfrogging vortex rings in a Bose-Einstein condensate

Three coaxial quantized vortex rings in a Bose-Einstein condensate exhibit aperiodic leapfrogging dynamics. It is found that such circular vortex rings are dynamically unstable against deformation breaking axial rotational symmetry. The dynamics of the system are analyzed using the Gross-Pitaevskii and vortex-filament models. The dependence of the instability on the initial arrangement of the vortex rings is investigated. The system is found to be significantly unstable for a specific configuration of the three vortex rings.
Modern Observations of Hubble’s First-discovered Cepheid in M31

We present a modern ephemeris and modern light curve of the first-discovered Cepheid variable in M31, Edwin Hubble’s M31-V1. Observers of the American Association of Variable Star Observers (AAVSO) undertook these observations during the latter half of 2010. The observations were in support of an outreach program by the Space Telescope Science Institute’s Hubble Heritage project, but the resulting data are the first concentrated observations of M31-V1 made in modern times. AAVSO observers obtained 214 V-band, Rc-band, and unfiltered observations from which a current ephemeris was derived. The ephemeris derived from these observations is JDMax = 2,455,430.5( ± 0.5) + 31.4( ± 0.1)E. The period derived from the 2010 data is in agreement with the historic values of the period, but the single season of data precludes a more precise determination of the period or measurement of the period change using these data alone. However, using an ephemeris based upon the period derived by Baade and Swope, we are able to fit all of the observed data acceptably well. Continued observations in the modern era will be very valuable in linking these modern data with data from the 1920s–1930s and 1950s and will enable us to measure period change in this historic Cepheid. In particular, we strongly encourage intensive observations of this star around predicted times of maximum to constrain the date of maximum to better than 0.5 days.