Miracle-dz/UniFAR-FTUs huggingface dataset:
Factors associated with development of adverse events after taking COVID-19 vaccine in a tribal state of India: Regression analysis

Background: Coronavirus disease (COVID-19) vaccination becomes a crucial weapon in the pandemic's control. Two vaccines, Covishield and Covaxin, are approved in India to vaccinate against the virus. Hence, the present study was done to determine the factors associated with the development of adverse events after taking the COVID-19 vaccine in a tribal state of India. Materials and Methods: This was a cross-sectional analytical study. All persons who were willing to participate in our study and had received the first or second dose of the COVID-19 vaccine from January 1 to March 31, 2021, were included. We got 1497 complete responses via (free, web-based Google Docs Editors suite offered by google, Founders- Larry Page Sergey Brin. Menlo Park, California, United States). So our final sample size came out to be 1497 in which analysis was done. The data was compiled in MS excel sheets (Microsoft version 2013, Microsoft Corporation, Redmond, Washington, United States) and a template was generated which was further analyzed in SPSS version 20 (version 25.0; IBM Corp., Armonk, NY, USA). Results: The total number of respondents who participated in the surveillance of adverse events following immunization (AEFI) was 1497. Among them, a majority have taken the Covishield vaccine followed by Covaxin. The majority of participants were female of age group less than 30 years and above 18 years with a mean age of 33.63 ± 51.51. The most common AEFI was pain at the site of injection, after the first and second dose followed by fever after the first and second dose within 24 h following immunization. Conclusion: We conclude that factors like the type of vaccine, gender, and participants who have allergies have a higher risk of presenting the adverse events after the COVID-19 vaccination.
Open physical systems: from GENERIC to port-Hamiltonian systems

Formulations of open physical systems within the framework of Non-Equilibrium Reversible/Irreversible Coupling (associated with the acronym "GENERIC") is related in this work with state-space realizations that are given as boundary port-Hamiltonian systems. This reformulation is carried out explicitly by splitting the dynamics of the system into a reversible contribution given by a Poisson bracket and an irreversible contribution given by a symmetric dissipation bracket, and is facilitated by the introduction of an exergy-like potential.
GENERAL RELATIVISTIC SIMULATIONS OF ACCRETION INDUCED COLLAPSE OF NEUTRON STARS TO BLACK HOLES

Neutron stars (NSs) in the astrophysical universe are often surrounded by accretion disks. Accretion of matter onto an NS may increase its mass above the maximum value allowed by its equation of state, inducing its collapse to a black hole (BH). Here we study this process for the first time, in three-dimensions, and in full general relativity. By considering three initial NS configurations, each with and without a surrounding disk (of mass ∼7% MNS), we investigate the effect of the accretion disk on the dynamics of the collapse and its imprint on both the gravitational wave (GW) and electromagnetic (EM) signals that can be emitted by these sources. We show in particular that, even if the GW signal is similar for the accretion induced collapse (AIC) and the collapse of an NS in vacuum (and detectable only for Galactic sources), the EM counterpart could allow us to discriminate between these two types of events. In fact, our simulations show that, while the collapse of an NS in vacuum leaves no appreciable baryonic matter outside the event horizon, an AIC is followed by a phase of rapid accretion of the surviving disk onto the newly formed BH. The post-collapse accretion rates, on the order of ∼10−2 M☉ s−1, make these events tantalizing candidates as engines of short gamma-ray bursts.
ON THE SOURCE OF FARADAY ROTATION IN THE JET OF THE RADIO GALAXY 3C 120

The source of Faraday rotation in the jet of the radio galaxy 3C 120 is analyzed through Very Long Baseline Array observations carried out between 1999 and 2007 at 86, 43, 22, 15, 12, 8, 5, 2, and 1.7 GHz. Comparison of observations from 1999 to 2001 reveals uncorrelated changes in the linear polarization of the underlying jet emission and the Faraday rotation screen: while the rotation measure (RM) remains constant between approximately 2 and 5 mas from the core, the RM-corrected electric vector position angles (EVPAs) of two superluminal components are rotated by almost 90° when compared to other components moving through similar jet locations. On the other hand, the innermost 2 mas experiences a significant change in RM—including a sign reversal—but without variations in the RM-corrected EVPAs. Similarly, observations in 2007 reveal a double sign reversal in RM along the jet, while the RM-corrected EVPAs remain perpendicular to the jet axis. Although the observed coherent structure and gradient of the RM along the jet support the idea that the Faraday rotation is produced by a sheath of thermal electrons that surrounds the emitting jet, the uncorrelated changes in the RM and RM-corrected EVPAs indicate that the emitting jet and the source of Faraday rotation are not closely connected physically and have different configurations for the magnetic field and/or kinematical properties. Furthermore, the existence of a region of enhanced RM whose properties remain constant over three years requires a localized source of Faraday rotation, favoring a model in which a significant fraction of the RM originates in foreground clouds.
Origin of low surface brightness galaxies: a dynamical study

Low Surface Brighness Galaxies (LSBs), inspite of being gas rich, have low star formation rates and are, therefore, low surface brightness in nature. We calculate Q$_{\rm{RW}}$, the 2-component disc stability parameter as proposed by Romeo \& Wiegert (2011), as a function of galactocentric radius $R$ for a sample of five LSBs, for which mass models, as obtained from HI 21cm radio-sythesis observations and R-band photometry, were available in the literature. We find that the median value of Q$_{\rm{RW}}^{\rm{min}}$, the minimum of Q$_{\rm{RW}}$ over $R$, lies between 2.6 and 3.1 for our sample LSBs, which is higher than the median value of 1.8 $\pm$ 0.3 for Q$_{\rm{RW}}^{\rm{min}}$ for a sampleof high surface brightness galaxies (HSBs) as obtained in earlier studies. This clearly shows that LSBs have more stable discs than HSBs, which could explain their low star formation rates and, possibly, their low surface brightness nature. Interestingly, the calculated values of Q$_{\rm{RW}}$ decrease only slightly (median Q$_{\rm{RW}}^{\rm{min}}$ $\sim$ 2.3 - 3) if the discs were taken to respond to the gravitational potential of the dark matter halo only, but reduce by $\sim$ a factor of 2-3 (median Q$_{\rm{RW}}^{\rm{min}}$ $\sim$ 0.7 - 1.5) if they respond to their self-gravity alone. This implies that the dark matter halo is crucial in regulating disc stability in LSBs, which may have important implications for models of galaxy formation and evolution.
Organ Crosstalk in Acute Kidney Injury: Evidence and Mechanisms

Acute kidney injury (AKI) is becoming a public health problem worldwide. AKI is usually considered a complication of lung, heart, liver, gut, and brain disease, but recent findings have supported that injured kidney can also cause dysfunction of other organs, suggesting organ crosstalk existence in AKI. However, the organ crosstalk in AKI and the underlying mechanisms have not been broadly reviewed or fully investigated. In this review, we summarize recent clinical and laboratory findings of organ crosstalk in AKI and highlight the related molecular mechanisms. Moreover, their crosstalk involves inflammatory and immune responses, hemodynamic change, fluid homeostasis, hormone secretion, nerve reflex regulation, uremic toxin, and oxidative stress. Our review provides important clues for the intervention for AKI and investigates important therapeutic potential from a new perspective.
HE 1327–2326, an Unevolved Star with [Fe/H]<–5.0. II. New 3D–1D Corrected Abundances from a Very Large Telescope UVES Spectrum

We present a new abundance analysis of HE 1327–2326, which is currently the most iron-poor star, based on observational data obtained with the VLT Ultraviolet and Visual Echelle Spectrograph (UVES). We correct the one-dimensional (1D) LTE abundances for three-dimensional (3D) effects to provide an abundance pattern that supersedes previous works and should be used to observationally test current models of the chemical yields of the first-generation supernovae (SNe). Apart from confirming the 1D LTE abundances found in previous studies before accounting for 3D effects, we make use of a novel technique to apply the 3D–1D corrections for CNO which are a function of excitation potential and line strength for the molecular lines that comprise the observable CH, NH, and OH features. We find that the fit to the NH band at 3360 Å is greatly improved due to the application of the 3D–1D corrections. This may indicate that 3D effects are actually observable in this star. We also report the first detection of several weak Ni lines. The cosmologically important element Li is still not detected; the new Li upper limit is extremely low, A(Li) < 0.62, and in stark contrast with results not only from the Wilkinson Microwave Anisotropy Probe (WMAP) but also from other metal-poor stars. We also discuss how the new corrected abundance pattern of HE 1327–2326 is being reproduced by individual and integrated yields of SNe.
On the equatorial Ekman layer

The steady incompressible viscous flow in the wide gap between spheres rotating rapidly about a common axis at slightly different rates (small Rossby number) has a long and celebrated history. The problem is relevant to the dynamics of geophysical and planetary core flows, for which, in the case of electrically conducting fluids, the possible operation of a dynamo is of considerable interest. A comprehensive asymptotic study, in the small Ekman number limit $E\ll 1$ , was undertaken by Stewartson (J. Fluid Mech., vol. 26, 1966, pp. 131–144). The mainstream flow, exterior to the $E^{1/2}$ Ekman layers on the inner/outer boundaries and the shear layer on the inner sphere tangent cylinder $\mathscr{C}$ , is geostrophic. Stewartson identified a complicated nested layer structure on $\mathscr{C}$ , which comprises relatively thick quasigeostrophic $E^{2/7}$ - (inside $\mathscr{C}$ ) and $E^{1/4}$ - (outside $\mathscr{C}$ ) layers. They embed a thinner ageostrophic $E^{1/3}$ shear layer (on $\mathscr{C}$ ), which merges with the inner sphere Ekman layer to form the $E^{2/5}$ -equatorial Ekman layer of axial length $E^{1/5}$ . Under appropriate scaling, this $E^{2/5}$ -layer problem may be formulated, correct to leading order, independent of $E$ . Then the Ekman boundary layer and ageostrophic shear layer become features of the far-field (as identified by the large value of the scaled axial coordinate $z$ ) solution. We present a numerical solution of the previously unsolved equatorial Ekman layer problem using a non-local integral boundary condition at finite $z$ to account for the far-field behaviour. Adopting $z^{-1}$ as a small parameter we extend Stewartson’s similarity solution for the ageostrophic shear layer to higher orders. This far-field solution agrees well with that obtained from our numerical model.
X-ray optical systems: from metrology to Point Spread Function

One of the problems often encountered in X-ray mirror manufacturing is setting proper manufacturing tolerances to guarantee an angular resolution - often expressed in terms of Point Spread Function (PSF) - as needed by the specific science goal. To do this, we need an accurate metrological apparatus, covering a very broad range of spatial frequencies, and an affordable method to compute the PSF from the metrology dataset. [. ] However, the separation between these spectral ranges is difficult do define exactly, and it is also unclear how to affordably combine the PSFs, computed with different methods in different spectral ranges, into a PSF expectation at a given X-ray energy. For this reason, we have proposed a method entirely based on the Huygens-Fresnel principle to compute the diffracted field of real Wolter-I optics, including measured defects over a wide range of spatial frequencies. Owing to the shallow angles at play, the computation can be simplified limiting the computation to the longitudinal profiles, neglecting completely the effect of roundness errors. Other authors had already proposed similar approaches in the past, but only in far-field approximation, therefore they could not be applied to the case of Wolter-I optics, in which two reflections occur in sequence within a short range. The method we suggest is versatile, as it can be applied to multiple reflection systems, at any X-ray energy, and regardless of the nominal shape of the mirrors in the optical system. The method has been implemented in the WISE code, successfully used to explain the measured PSFs of multilayer-coated optics for astronomic use, and of a K-B optical system in use at the FERMI free electron laser.
Efficacy of Radiofrequency Ablation in Chronic Pain Management

The aim of this study is to determine the efficacy of radiofrequency ablation in management of chronic pain. Radiofrequency ablation in pain management was done in 21 patients who were experiencing chronic pain in different regions of the body. Patients were divided into three groups according to region of pain i.e. chronic lower back pain, trigeminal neuralgia, and osteoarthritis. Pre-treatment and Post-treatment pain score were taken with numeric rating scale (NRS). Denervation was achieved in the pain originating region with the help of Cosman RFG-1A radiofrequency generator under fluoroscopy obtained from Axiom Artis U. The comparison between pre pain score and post pain score revealed the pain was almost nullified in 52% of the patients whereas in 33% it was reduced to tolerable levels and 15% still had some trouble, though pain was slightly reduced as compared before ablation. Radiofrequency ablation alleviated the pain in cases where oral medications were not enough and surgical management could not be done or had a failure.
The Enumeration of Cyclic MNOLS

In this paper we study collections of mutually nearly orthogonal Latin squares ($\text{MNOLS}$), which come from a modification of the orthogonal condition for mutually orthogonal Latin squares. In particular, we find the maximum $\mu$ such that there exists a set of $\mu$ cyclic $\text{MNOLS}$ of order $n$ for $n \leq 18$, as well as providing a full enumeration of sets and lists of $\mu$ cyclic $\text{MNOLS}$ of order $n$ under a variety of equivalences with $n \leq 18$. This resolves in the negative a conjecture that proposed the maximum $\mu$ for which a set of $\mu$ cyclic $\text{MNOLS}$ of order $n$ exists is $\lceil n/4\rceil +1$.
VORTICITY OF INTERGALACTIC MEDIUM VELOCITY FIELD ON LARGE SCALES

We investigate the vorticity of the intergalactic medium (IGM) velocity field on large scales with cosmological hydrodynamic simulation of the concordance model of ΛCDM. We show that the vorticity field is significantly increasing with time as it can effectively be generated by shocks and complex structures in the IGM. Therefore, the vorticity field is an effective tool to reveal the nonlinear behavior of the IGM, especially the formation and evolution of turbulence in the IGM. We find that the vorticity field does not follow the filament and sheet structures of the underlying dark matter density field and shows highly non-Gaussian and intermittent features. The power spectrum of the vorticity field is then used to measure the development of turbulence in Fourier space. We show that the relation between the power spectra of vorticity and velocity fields is perfectly in agreement with the prediction of a fully developed homogeneous and isotropic turbulence in the scale range from 0.2 to about 3 h−1 Mpc at z ∼ 0. This indicates that the cosmic baryonic field is in the state of fully developed turbulence on scales less than about 3 h−1 Mpc. The random field of the turbulent fluid yields turbulent pressure to prevent the gravitational collapsing of the IGM. The vorticity and turbulent pressure are strong inside and even outside of high density regions. In IGM regions with 10 times mean overdensity, the turbulent pressure can be on an average equivalent to the thermal pressure of the baryonic gas with a temperature of 1.0 × 105 K. Thus, the fully developed turbulence would prevent the baryons in the IGM from falling into the gravitational well of dark matter halos. Moreover, turbulent pressure essentially is dynamical and non-thermal, which makes it different from a pre-heating mechanism, as it does not affect the thermal state and ionizing process of hydrogen in the IGM.
Bayesian peak-bagging of solar-like oscillators using MCMC: a comprehensive guide

Context. Asteroseismology has entered a new era with the advent of the NASA Kepler mission. Long and continuous photometric observations of unprecedented quality are now available which have stimulated the development of a number of suites of innovative analysis tools. Aims. The power spectra of solar-like oscillations are an inexhaustible source of information on stellar structure and evolution. Robust methods are hence needed in order to infer both individual oscillation mode parameters and parameters describing non-resonant features, thus making a seismic interpretation possible. Methods. We present a comprehensive guide to the implementation of a Bayesian peak-bagging tool that employs a Markov chain Monte Carlo (MCMC). Besides making it possible to incorporate relevant prior information through Bayes’ theorem, this tool also allows one to obtain the marginal probability density function for each of the fitted parameters. We apply this tool to a couple of recent asteroseismic data sets, namely, to CoRoT observations of HD 49933 and to ground-based observations made during a campaign devoted to Procyon. Results. The developed method performs remarkably well at constraining not only in the traditional case of extracting oscillation frequencies, but also when pushing the limit where traditional methods have difficulties. Moreover it provides an rigorous way of comparing competing models, such as the ridge identifications, against the asteroseismic data.
Effects of Feeding Regimes and Postmortem Aging on Meat Quality, Fatty Acid Composition, and Volatile Flavor of Longissimus Thoracis Muscle in Sunit Sheep

Simple Summary This manuscript investigated the effects of different feeding regimes on antioxidant activity, meat quality, fatty acid composition, lipid oxidation, and volatile matter production in the longissimus thoracis muscle of Sunit sheep during postmortem aging. It was found that pasture-fed sheep had better oxidative stability, meat quality, and fatty acid composition. At the same time, aging affected the oxidative stability, meat quality, and fatty acid composition of sheep meat, which in turn had an impact on the flavor composition of sheep meat. Aging also eliminates the differences caused by different feeding regimes to a certain extent. The purpose of this study was to investigate the effects of feeding regimes and aging time on the meat quality of sheep and to provide meat professionals with a theoretical basis that can be applied in practical production. It also accelerated the transition from traditional grazing to indoor rearing to maintain ecological balance. Abstract The effects of different feeding regimes on antioxidant activity, meat quality, fatty acid composition, lipid oxidation, and volatile matter production in the longissimus thoracis (LT) of Sunit sheep at 0, 24, 48, 72, and 96 h postmortem were investigated. The results showed that the activity of antioxidant enzymes, tenderness, water retention, and percentage of unsaturated fatty acids were significantly higher in the pasture-fed sheep (PF) than in the concentrate-fed sheep (CF) (p < 0.05). During postmortem aging, antioxidant activity, water retention, and the proportion of unsaturated fatty acids decreased in the PF and CF (p < 0.05), while malondialdehyde (MDA) content, the proportion of saturated fatty acids, and the content of flavor substances resulting from fat oxidation increased. After 24 h of LT muscle aging, the pH and shear force of the meat started to increase and the color stabilized. The differences between shear force values and lipid volatile flavor substance content of sheep meat under different feeding regimes disappeared with increasing aging time. PF had better oxidative stability and fatty acid composition. Postmortem aging changed the oxidative stability of sheep meat, thus affecting meat quality and fatty acid composition and consequently meat flavor composition, while aging also eliminated to some extent the differences caused by feeding regimes.
On the number of relevant operators in asymptotically safe gravity

The asymptotic safety scenario of gravity conjectures that i) the quantum field theory of gravity exists thanks to the presence of a non-trivial ultraviolet fixed point of the renormalization group, and that ii) the fixed point has only a finite number of relevant perturbations, i.e., a finite number of UV-stable directions (or, in other words, a finite number of free parameters to be fixed experimentally). Within the f(R) approximation of the functional renormalization group equation of gravity, we show that assuming the first half of the conjecture to be true, the remaining half follows from general arguments, that is, we show that assuming the existence of a non-trivial fixed point, the fact that the number of relevant directions is finite is a general consequence of the structure of the equations.
Broken degeneracies: the rotation curve and velocity anisotropy of the Milky Way halo

We use distant blue horizontal branch stars with Galactocentric distances 16 < r < 48 kpc as kinematic tracers of the Milky Way dark halo. We model the tracer density as an oblate, power law embedded within a spherical power-law potential. Using a distribution function method, we estimate the overall power-law potential and the velocity anisotropy of the halo tracers. We measure the slope of the potential to be γ ∼ 0.4, and the overall mass within 50 kpc is ∼4 × 10 11 M� . The tracer velocity anisotropy is radially biased with β ∼ 0.5, which is in good agreement with local solar neighbourhood studies. Our results provide an accurate outer circular velocity profile for the Milky Way and suggest a relatively high-concentration dark matter halo (cvir ∼ 20).