Miracle-dz/UniFAR-FTUs huggingface dataset:
Preparedness for the Dengue Epidemic: Vaccine as a Viable Approach

Dengue fever is one of the significant fatal mosquito-borne viral diseases and is considered to be a worldwide problem. Aedes mosquito is responsible for transmitting various serotypes of dengue viruses to humans. Dengue incidence has developed prominently throughout the world in the last ten years. The exact number of dengue cases is underestimated, whereas plenty of cases are misdiagnosed as alternative febrile sicknesses. There is an estimation that about 390 million dengue cases occur annually. Dengue fever encompasses a wide range of clinical presentations, usually with undefinable clinical progression and outcome. The diagnosis of dengue depends on serology tests, molecular diagnostic methods, and antigen detection tests. The therapeutic approach relies completely on supplemental drugs, which is far from the real approach. Vaccines for dengue disease are in various stages of development. The commercial formulation Dengvaxia (CYD-TDV) is accessible and developed by Sanofi Pasteur. The vaccine candidate Dengvaxia was inefficient in liberating a stabilized immune reaction toward different serotypes (1–4) of dengue fever. Numerous promising vaccine candidates are now being developed in preclinical and clinical stages even though different serotypes of DENV exist that worsen the situation for a vaccine to be equally effective for all serotypes. Thus, the development of an efficient dengue fever vaccine candidate requires time. Effective dengue fever management can be a multidisciplinary challenge, involving international cooperation from diverse perspectives and expertise to resolve this global concern.
A catalogue of absorption-line systems in QSO spectra

We present a new catalog of absorption-line systems identified in the quasar spectra. It contains data on 821 QSOs and 8558 absorption systems comprising 16 139 absorption lines with measured redshifts in the QSO spectra. The catalog includes absorption-line systems consisting of lines of heavy elements, lines of neutral hydrogen, Lyman limit systems, damped Ly α absorption systems, and broad absorption-line systems. Using the data of the present catalog we also discuss redshift distributions of absorption-line systems.
Contribution of the tRNA Ile 4317A 3 G mutation to the phenotypic manifestation of the deafness-associated mitochondrial 12S rRNA 1555A 3 G mutation

The 1555A 3 G mutation in mitochondrial 12S rRNA has been associated with aminoglycoside-induced and non-syn-dromic deafness in many individuals worldwide. Mitochondrial genetic modifiers are proposed to influence the phenotypic expression of m.1555A 3 G mutation. Here, we report that a deafness-susceptibility allele (m.4317A 3 G) in
Radiation driven winds in X-ray binaries.

We discuss the properties of a radiation-driven stellar wind in an X-ray binary system. The Castor, Abbott, Klein line-driven wind model is used, but the effects of the compact companion (gravity and continuum radiation pressure) and the centrifugal force due to orbital motion are included. These forces destroy the spherical symmetry of the wind and can make the mass loss and accretion strong functions of the size of the primary relative to its critical potential lobe. We in most systems the wind alone could power the X-ray emission. It also appears that, in the evolution of these systems, there would be a continuous transition from wind accretion to critical potential lobe overflow. The model is also used to make a prediction about the nature of a suspected binary system which is not known to be an X-ray emitter.
An Anisotropic Low-Dimensional Ising System, [ ( C H 3 ) 3 NH]Co Cl 3 · 2 H 2 O: Its Structure and Canted Antiferromagnetic Behavior

The crystal structure at room temperature and the heat-capacity and magnetic susceptibilities at low temperatures of single crystals of [${(\mathrm{C}{\mathrm{H}}_{3})}_{3}$NH]Co${\mathrm{Cl}}_{3}$ \ifmmode\cdot\else\textperiodcentered\fi{} 2${\mathrm{H}}_{2}$O are reported. The orthorhombic crystals belong to the space group $\mathrm{Pnma}$ with $a=16.671(3)$ \AA{}, $b=7.273(1)$ \AA{} $c=8.113(2)$ \AA{}, and $Z=4$. The structure consists of chains of edge-sharing trans- [Co${\mathrm{Cl}}_{4}$${(\mathrm{O}{\mathrm{H}}_{2})}_{2}$] octahedra running parallel to the $b$ axis. At 4.135 \ifmmode^\circ\else\textdegree\fi{}K, [${(\mathrm{C}{\mathrm{H}}_{3})}_{3}$NH]Co${\mathrm{Cl}}_{3}$ \ifmmode\cdot\else\textperiodcentered\fi{} 2${\mathrm{H}}_{2}$O undergoes a second-order phase transition. The heat-capacity data have been analyzed using Onsager's solution for the two-dimensional Ising model. The lattice contribution was taken into account by using the lattice of the isostructural [${(\mathrm{C}{\mathrm{H}}_{3})}_{3}$NH]Cu${\mathrm{Cl}}_{3}$ \ifmmode\cdot\else\textperiodcentered\fi{} 2${\mathrm{H}}_{2}$O and a corresponding states procedure. The three principal-axis single-crystal susceptibilities display an unusual amount of anisotropy. Two of the data sets (one parallel and one perpendicular to the chemical chain) have been fit to an Ising linear-chain model. A small molecular-field correction significantly improved one of those fits. The $a$-axis susceptibility displays an unusually sharp rise, with decreasing temperature, very close to ${T}_{N}$ along with the suggestion of a net moment persisting below the transition. Thus, a Dzyaloshinsky-Moriya antisymmetric exchange interaction was assumed to be operative, since it is symmetry alowed in this space group, and Moriya's molecular-field-susceptibility calculation was used to fit this data set. All four of the data sets are quite reasonably described, the specific heat and one of the susceptibility sets within experimental error, by the following set of parameters: rectangular lattice exchange parameters of $\frac{J}{k}=(7.7\ifmmode\pm\else\textpm\fi{}0.2)$ \ifmmode^\circ\else\textdegree\fi{}K and $\frac{{J}^{\ensuremath{'}}}{k}=(0.09\ifmmode\pm\else\textpm\fi{}0.01)$ \ifmmode^\circ\else\textdegree\fi{}K; spectroscopic splitting parameters of ${g}_{a}=2.95\ifmmode\pm\else\textpm\fi{}0.05$, ${g}_{b}=3.90\ifmmode\pm\else\textpm\fi{}0.01$, and ${g}_{c}=6.54\ifmmode\pm\else\textpm\fi{}0.01$; and a Dzyaloshinsky-Moriya antisymmetric exchange parameter of $|\frac{D}{k}|=(4.9\ifmmode\pm\else\textpm\fi{}0.2)$ \ifmmode^\circ\else\textdegree\fi{}K. Finally, a consistent spin structure is proposed in which the intrachain interaction is ferromagnetic with the compound ordering antiferromagnetically below 4.135\ifmmode^\circ\else\textdegree\fi{}K such that there is a small net moment in the $a$ direction.
Evidence for the rare decay B+→Ds+π0

The authors have searched for the rare decay B{sup +} {yields} D{sub s}{sup +}{pi}{sup 0}. The analysis is based on a sample of 232 million {Upsilon}(4S) {yields} B{bar B} decays collected with the BABAR detector at the PEP-II e{sup +}e{sup -} storage ring. They find 19.6 signal events, corresponding to a significance of 4.7 {sigma}. The extracted signal yield including statistical and systematic uncertainties is 20.1{sub -6.0-1.5}{sup +6.8+0.4}, and they measure {Beta}(B{sup +} {yields} D{sub s}{sup +}{pi}{sup 0}) = (1.5{sub -0.4}{sup +0.5} {+-} 0.1 {+-} 0.2) x 10{sup -5}, where the first uncertainty is statistical, the second is systematic, and the last is due to the uncertainty on the D{sub s}{sup +} decay and its daughter decay branching fractions.
Periodic Variability of the Barium Central Star of the Planetary Nebula Abell 70

Abell 70 is a planetary nebula (PN) whose nucleus at optical wavelengths is a G8 star with enhanced carbon and s-process abundances--a "barium star. " The cool star is a binary companion of the true, hot central star. In several other members of this rare class, the cool star is known to rotate with a period of only a few days. This is attributed to a spin-up that occurred due to accretion from the wind of the central star during its post-AGB PN ejection; this also accounts for the unusual chemical composition of the companion's photosphere. We obtained photometry of the central star of Abell 70 on 104 nights in 2010-11, and find a periodic 2.061-day variation, but with a variable amplitude--indicating that the variability is due to starspots on a chromospherically active star. Abell 70 thus joins other members of this class in having a rapidly rotating and chemically peculiar late-type companion of the hot central star.
THE N-NETWORK MODEL WITH UPGRADES

In this article we introduce a new method of mitigating the problem of long wait times for low-priority customers in a two-class queuing system. To this end, we allow class 1 customers to be upgraded to class 2 after they have been in queue for some time. We assume that there are ci servers at station i, i=1, 2. The servers at station 1 are flexible in the sense that they can work at either station, whereas the servers at station 2 are dedicated. Holding costs at rate hi are accrued per customer per unit time at station i, i=1, 2. This study yields several surprising results. First, we show that stability analysis requires a condition on the order of the service rates. This is unexpected since no such condition is required when the system does not have upgrades. This condition continues to play a role when control is considered. We provide structural results that include a c-μ rule when an inequality holds and a threshold policy when the inequality is reversed. A numerical study verifies that the optimal control policy significantly reduces holding costs over the policy that assigns the flexible server to station 1. At the same time, in most cases the optimal control policy reduces waiting times of both customer classes.
Probing homogeneity with standard candles

We show that standard candles can provide some valuable information about the density contrast, which could be particularly important at redshifts where other observations are not available. We use an inversion method to reconstruct the local radial density profile from luminosity distance observations assuming background cosmological parameters obtained from large scale observations. Using type Ia Supernovae, Cepheids and the cosmological parameters from the Planck mission we reconstruct the radial density profiles along two different directions of the sky. We compare these profiles to other density maps obtained from luminosity density, in particular Keenan et al. 2013 and the \textsc{2M++} galaxy catalogue. The method independently confirms the existence of inhomogeneities, could be particularly useful to correctly normalize density maps from galaxy surveys with respect to the average density of the Universe, and could clarify the apparent discrepancy between local and large scale estimations of the Hubble constant. When better observational supernovae data will be available, the accuracy of the reconstructed density profiles will improve and will allow to further investigate the existence of structures whose size is beyond the reach of galaxy surveys.
Cosmologies with varying light speed

We analyse a generalisation of general relativity that incorporates a cosmic time-variation of the velocity of light in vacuum, $c,$ and the Newtonian gravitation 'constant', $G,$ proposed by Albrecht and Maguejo. We find exact solutions for Friedmann universes and determine the rate of variation of $c$ required to solve the flatness and classical cosmological constant problems. Potential problems with this approach to the resolution of the flatness and classical cosmological constant problems are highlighted. Reformulations are suggested which give the theory a more desirable limit as a theory of varying $G$ in the limit of constant $c$ and its relationship to theories with varying electron charge and constant $c$ are discussed.
Detecting Population III Stars through Observations of Near-Infrared Cosmic Infrared Background Anisotropies

Following the successful mapping of the last scattering surface by the Wilkinson Microwave Anisotropy Probe (WMAP) and balloon experiments, the epoch of the first stars, when Population III stars formed, is emerging as the next cosmological frontier. It is not clear what these stars' properties were, when they formed, or how long their era lasted before leading to the stars and galaxies we see today. We show that these questions can be answered with the current and future measurements of the near-IR cosmic infrared background (CIB). Theoretical arguments suggest that Population III stars were very massive and short-lived stars that formed at z ~ 10-20 at rare peaks of the density field in the cold dark matter universe. Because Population III stars probably formed individually in small minihalos, they are not directly accessible to current telescopic studies. We show that these stars left a strong and measurable signature via their contribution to the CIB anisotropies for a wide range of their formation scenarios. The excess in the recently measured near-IR CIB anisotropies over that from normal galaxies can be explained by contribution from early Population III stars. These results imply that Population III were indeed very massive stars and that their epoch started at z ~ 20 and lasted past z ≲ 13. We show the importance of accurately measuring the CIB anisotropies produced by Population III with future space-based missions.
Theoretical analysis of quantum dynamics in one-dimensional lattices: Wannier-Stark description

This paper presents a formalism describing the dynamics of a quantum particle in a one-dimensional, tilted, time-dependent lattice. The description uses the Wannier-Stark states, which are localized in each site of the lattice, and provides a simple framework leading to fully analytical developments. Particular attention is devoted to the case of a time-dependent potential, which results in a rich variety of quantum coherent dynamics.
Sound modes at the BCS-BEC crossover

First and second sound speeds are calculated for a uniform superfluid gas of Fermi atoms as a function of temperature, density, and interaction strength. The second sound speed is of particular interest as it is a clear signal of a superfluid component and it determines the critical temperature. The sound modes and their dependence on density, scattering length, and temperature are calculated in the BCS, molecular Bose-Einstein condensate (BEC), and unitarity limits and a smooth crossover is extrapolated. It is found that first and second sounds undergo avoided crossing on the BEC side due to mixing. Consequently, they are detectable at crossover both as density and thermal waves in traps.
What the Optical Recombination Lines Can Tell Us about the Broad-Line Regions of Active Galactic Nuclei

We investigate the effect of a global change in the ionizing continuum level on the behavior of the strong optical broad emission lines seen in spectra of the nuclear emission-line regions of active galactic nuclei (AGNs), including the Balmer lines, He I λ5876, and He II λ4686. Unlike most of the prominent heavy-element lines found in the UV, the optical hydrogen and helium recombination lines' emissivities are strongly dependent on the incident continuum flux, since these lines arise out of excited states whose optical depths depend on the incident flux of photons. Using photoionization calculations, we determine the luminosity-dependent responsivities, η(r, L(t)) = Δ log Lline/Δ log Lcont, of these lines for a general model of the broad emission line region (BLR), with the purpose of establishing them as important probes of the physical conditions within the BLRs of AGNs. The dependence of these lines' emissivities on the incident photon flux invokes a dependence in their responsivities on distance from the central continuum source. In particular, the responsivities of these lines are generally anticorrelated with the incident photon flux. Thus, their responsivities vary with distance within the BLR for a fixed continuum luminosity and change with time as the continuum source varies. Consequently, after correcting for light-travel-time effects, the response of the Balmer and optical helium lines should generally be strongest during low continuum luminosity states. Responsivity that depends on photon flux and continuum state may explain a number of outstanding problems currently under investigation in broad-line variability studies of these and other emission lines. These include the origin of the intrinsic Baldwin effect, measurements of luminosity-dependent lags (a "breathing" BLR), and luminosity-dependent variations in integrated broad emission line flux ratios (including He II λ4686/Hβ), broad-line profile shapes, and radial velocity-dependent intensity ratios. The broad Hα/Hβ and He I/Hβ flux ratios and the Balmer emission line responsivity are observed to decrease from the line center to the line wings. These, along with our findings, lead to the conclusion that the BLR velocity field diminishes with increasing distance from the central continuum source. This is consistent with recent reverberation studies that find a relationship between the emission-line lag and rms profile width for multiple lines in individual AGNs, which implies that the velocity field is dominated by a central massive object. Finally, the responsivity of ionization-bounded clouds can account for much of the observed behavior of the optical recombination lines (e.g., the weak response of the Balmer line wings) previously attributed to a substantial contribution from matter-bounded clouds at small BLR radii.
Mesoscopic description of reactions for anomalous diffusion: a case study

Reaction–diffusion equations deliver a versatile tool for the description of reactions in inhomogeneous systems under the assumption that the characteristic reaction scales and the scales of the inhomogeneities in the reactant concentrations separate. In the present work, we discuss the possibilities of a generalization of reaction–diffusion equations to the case of anomalous diffusion described in terms of continuous-time random walks with decoupled step length and waiting time probability densities, the first being Gaussian or Lévy, the second one being an exponential or a power law lacking the first moment. We consider a special case of an irreversible or reversible conversion and show that only in the Markovian case of an exponential waiting time distribution can the diffusion term and the reaction term be decoupled. In all other cases, the properties of the reaction affect the transport operator, so the form of the corresponding reaction–anomalous diffusion equations does not closely follow the form of the usual reaction–diffusion equations.
COMBUSTION OSCILLATIONS IN A TWIN-STREAM AFTERBURNER

Abstract In a modern turbo-fan engine, the afterburner flame-holders are positioned in the mixing flow between the core and bypass streams. These two streams have different velocities and temperatures. They also have different duct lengths and, therefore, different acoustic properties. The influence of such a twin-stream supply on acoustically coupled combustion oscillations is investigated in this paper. Measurements on an experimental rig show how differences in the acoustic impedances, the mean velocities and the mean temperatures in the two supply streams lead to appreciably different unsteady heat release rates in the two streams. These affect the frequency of the combustion oscillations. A theory explains these results and correctly describes the variation in frequency as the properties of the two supply streams are varied.
The Lyα Forest of a Lyman Break Galaxy: Very Large Telescope Spectra of MS 1512–cB58 at z = 2.724

The high-redshift galaxy MS 1512-cB58 (z = 2.724, mV = 20.64) has been observed with the very efficient high-resolution UV-Visual Eschelle Spectograph on the Very Large Telescope. Although this is a very challenging observational program for a Southern Hemisphere telescope (the galaxy is located at +36° declination), high-resolution spectra (FWHM ≃ 26 km s-1) have revealed, with unprecedented detail along a galaxy sight line, the Lyα forest due to intervening clouds in the intergalactic medium (IGM). The mean depression DA due to IGM absorption blueward of the galaxy Lyα wavelength and the number density dn/dz of Lyα clouds have been compared with equivalent results obtained for QSO sight lines at similar redshifts. Our results indicate a possible excess of absorption close to the galaxy. The mean depression at ~150 h Mpc comoving (Ωm = 0.3, ΩΛ = 0.7) from the galaxy is DA = 0.36 ± 0.03, to be compared with 0.22 ± 0.04 expected from a best fit to QSO sight lines. In the same region (z ≃ 2.610), the number density of lines with H I column density in excess of 1014 atoms cm-2 is also ~3 σ larger than expected. This high-density region is at least 60 h Mpc comoving wide, but the large Lyα absorption of the galaxy itself prevents us from detecting a possible structure extending down to the galaxy. This excess of Lyα clouds is suggestive of two possible scenarios. One is the presence of a supercluster of Lyα clouds not associated with cB58. The other is a high density of gas associated with the environment of cB58. Indeed, a hint of the complexity of cB58 and possibly its environment is given by the huge velocity range (almost 1000 km s-1) between the optical emission of star-forming regions and UV absorption of its interstellar medium.
Out-of-equilibrium evolution of scalar fields in FRW cosmology: Renormalization and numerical simulations

We present a renormalized computational framework for the evolution of a self-interacting scalar field (inflaton) and its quantum fluctuations in a FRW background geometry. We include a coupling of the field to the Ricci scalar with a general coupling parameter $\ensuremath{\xi}. $ We take into account the classical and quantum back reactions; i.e., we consider the dynamical evolution of the cosmic scale factor. We perform, in the one-loop and in large-$N$ approximations, the renormalization of the equation of motion for the inflaton field, and of its energy momentum tensor. Our formalism is based on a perturbative expansion for the mode functions, and uses dimensional regularization. The renormalization procedure is manifestly covariant and the counterterms are independent of the initial state. Some shortcomings in the renormalization of the energy-momentum tensor in an earlier publication are corrected. We avoid the occurrence of initial singularities by constructing a suitable class of initial states. The formalism is implemented numerically and we present some results for the evolution in the post-inflationary preheating era.
Magnetization precession due to a spin-polarized current in a thin nanoelement: Numerical simulation study

In this paper a detailed numerical study in frames of the Slonczewski formalism of magnetization oscillations driven by a spin-polarized current through a thin elliptical nanoelement is presented. We show that a sophisticated micromagnetic model, where a polycrystalline structure of a nanoelement is taken into account, can explain qualitatively all most important features of the magnetization oscillation spectra recently observed experimentally S. I. Kiselev et al., Nature 425, 380 2003, namely, existence of several equidistant spectral bands, sharp onset and abrupt disappearance of magnetization oscillations with increasing current, absence of the out-of-plane regime predicted by a macrospin model, and the relation between frequencies of so-called small-angle and quasichaotic oscillations. However, a quantitative agreement with experimental results especially concerning the frequency of quasichaotic oscillations could not be achieved in the region of reasonable parameter values, indicating that further model refinement is necessary for a complete understanding of the spin-driven magnetization precession even in this relatively simple experimental situation.