Miracle-dz/UniFAR-FTUs huggingface dataset:
The Effect of Roselle (Hibiscus) Juice on Mood Improvement in Healthy Adults

Introduction: The juice of Hibiscus sabdariffa Linn is commonly used as a traditional medicine for hypertension, pyrexia, and mood improvement. This study aimed to examine the effect of hibiscus juice on the mood states of healthy Saudi adults. Methods: A total of 32 healthy adults were asked to complete a questionnaire and were subsequently provided with 250 mL of prepared hibiscus juice to drink daily for 1 week. The participants were instructed to answer the Beck Depression Inventory before and after 1 week of drinking the hibiscus juice daily. Results: The results indicated a significantly positive change in the participants’ daily mood after 1 week of drinking 250 mL of hibiscus juice daily. Drinking hibiscus juice enhanced mood status by increasing relaxation and decreasing fear of the future and heart palpitations in most participants. Furthermore, it increased the consumption of caffeinated drinks. However, drinking hibiscus juice had no effect on the number of meals consumed. Conclusion: Drinking hibiscus juice had significant beneficial effects on mood. These results may be useful for future public health recommendations, especially among young adults and children. Further studies with larger sample sizes and longer experimental durations are needed to confirm and generalise these findings.Keywords: Mood Improvement, Cognitive, Hibiscus, Saudi Arabia, Adults
IS DUST FORMING ON THE RED GIANT BRANCH IN 47 Tuc?

Using Spitzer Infrared Array Camera (IRAC) observations from the SAGE-SMC Legacy program and archived Spitzer IRAC data, we investigate dust production in 47 Tuc, a nearby massive Galactic globular cluster. A previous study detected infrared excess, indicative of circumstellar dust, in a large population of stars in 47 Tuc, spanning the entire red giant branch (RGB). We show that those results suffered from effects caused by stellar blending and imaging artifacts and that it is likely that no stars below ≈1 mag from the tip of the RGB are producing dust. The only stars that appear to harbor dust are variable stars, which are also the coolest and most luminous stars in the cluster.
The Galactic evolution of phosphorus

Context. As a galaxy evolves, its chemical composition changes and the abundance ratios of different elements are powerful probes of the underlying evolutionary processes. Phosphorous is an element whose evolution has remained quite elusive until now, because it is difficult to detect in cool stars. The infrared weak P i lines of the multiplet 1, at 1050−1082 nm, are the most reliable indicators of the presence of phosphorus. The availability of CRIRES at VLT has permitted access to this wavelength range in stellar spectra. Aims. We attempt to measure the phosphorus abundance of twenty cool stars in the Galactic disk. Methods. The spectra are analysed with one-dimensional model-atmospheres computed in local thermodynamic equilibrium (LTE). The line formation computations are performed assuming LTE. Results. The ratio of phosphorus to iron behaves similarly to sulphur, increasing towards lower metallicity stars. Its ratio with respect to sulphur is roughly constant and slightly larger than solar, [P/S] = 0.10 ± 0.10. Conclusions. We succeed in taking an important step towards the understanding of the chemical evolution of phosphorus in the Galaxy. However, the observed rise in the P/Fe abundance ratio is steeper than predicted by Galactic chemical evolution model developed by Kobayashi and collaborators. Phosphorus appears to evolve differently from the light odd-Z elements sodium and aluminium. The constant value of [P/S] with metallicity implies that P production is insensitive to the neutron excess, thus processes other than neutron captures operate. We suggest that proton captures on 30 Si and α captures on 27 Al are possibilities to investigate. We see no clear distinction between our results for stars with planets and stars without any detected planet.
Using check dam deposits to reconstruct changes in the sediment response of a small catchment on the Loess Plateau in China, during the period 1960–1990

Information on both the magnitude and relative contributions of inter‐gully and gully areas to the sediment yield from small catchments in the Loess Plateau of China represents an important requirement for understanding catchment sediment dynamics, assessing the sensitivity of catchment sediment budgets to environmental change and developing effective soil and water conservation strategies. Contemporary catchment monitoring programmes can provide such information, but there is also a need to consider past behaviour. Where long‐term records are lacking, attention has been directed to the potential for using the sediment deposits behind check dams to reconstruct the sediment response of the upstream catchment. This contribution reports a study of the 0.181 km2 Nianyangou catchment located in the hilly region of the Chinese Loess Plateau, in Shaanxi Province, China, which has extended a previous study aimed at using individual flood couplets preserved in the check dam deposits to reconstruct the record of annual sediment yield, to include the use of sediment source fingerprinting techniques to document changes in the annual sediment contribution from inter‐gully and gully areas for the period 1960–1990. The sediment response of the catchment provided evidence of two change points in 1964 (Period 1–Period 2) and 1983 (Period 2–Period 3), which reflect the introduction of soil and water conservation measures in the mid 1960s through to the 1970s and a change in the land tenure system in 1983. The annual sediment yields from inter‐gully and gully areas follow the trend P1 > P3 > P2, whereas the equivalent information on the relative contribution of inter‐gully and gully areas follow different trends P3 > P1 > P2 and P2 > P1 > P3, respectively.
General relativistic calculations for white dwarfs

The mass-radius relations for white dwarfs are investigated by solving the Newtonian as well as Tolman-Oppenheimer-Volkoff (TOV) equations for hydrostatic equilibrium assuming the electron gas to be non-interacting. We find that the Newtonian limiting mass of 1.4562 M ⊙ is modified to 1.4166 M ⊙ in the general relativistic case for He 2 4 (and C 6 12 ) white dwarfs. Using the same general relativistic treatment, the critical mass for Fe 26 56 white dwarfs is obtained as 1.2230 M ⊙ . In addition, departure from the ideal degenerate equation of state (EoS) is accounted for by considering Salpeter’s EoS along with the TOV equation, yielding slightly lower values for the critical masses, namely 1.4081 M ⊙ for He 2 4 , 1.3916 M ⊙ for C 6 12 and 1.1565 M ⊙ for Fe 26 56 white dwarfs. We also compare the critical densities for gravitational instability with the neutronization threshold densities to find that He 2 4 and C 6 12 white dwarfs are stable against neutronization with the critical values of 1.4081 M ⊙ and 1.3916 M ⊙ , respectively. However, the critical masses for O 8 16 , Ne 10 20 , Mg 12 24 , Si 14 28 , S 16 32 and Fe 26 56 white dwarfs are lower due to neutronization. Corresponding to their central densities for neutronization thresholds, we obtain their maximum stable masses due to neutronization by solving the TOV equation coupled with the Salpeter EoS.
Fast Analysis of Caffeic Acid-Related Molecules in Instant Coffee by Reusable Sonogel–Carbon Electrodes

Reusable Sonogel–Carbon electrodes containing carbon black (SNGC-CB) have been used for the electrochemical analysis of caffeic acid (CA) in real matrices. Measurements were firstly performed in standard solutions, in which SNGC-CB electrodes allowed the electrochemical determination of CA with high sensitivity and low limit of detection, equal to 0.76 μM. The presence of CB nanostructures in the formulation led to improved performances with respect to pristine SNGC electrodes. Then, measurements were performed in four instant coffees of different brands. A comparison between the results obtained by electrochemical, chromatographic and spectroscopic methods showed that SBGC-CB electrodes represent a simple and economic tool for the rapid assessment of caffeic acid-related molecules in instant coffees.
Critical exponent of quantum phase transitions driven by colored noise

We demonstrate that criticality in a driven-dissipative system is strongly influenced by the spectral properties of the bath. We study the open-system realization of the Dicke model, where a bosonic cavity mode couples to a large spin formed by two motional modes of an atomic Bose-Einstein condensate. The cavity mode is driven by a high-frequency laser and it decays to a Markovian bath, while the atomic mode interacts with a colored bath. We reveal that the soft mode fails to describe the characteristics of the criticality. We calculate the critical exponent of the superradiant phase transition and identify an inherent relation to the low-frequency spectral density function of the colored bath. We show that a finite temperature of the colored bath does not modify qualitatively this dependence on the spectral density function.
Generation of longitudinal flux tube waves in theoretical main-sequence stars: effects of model parameters

Aims. We compute the wave energy fluxes carried by longitudinal tube waves along vertically oriented thin magnetic fluxes tubes embedded in the atmospheres of theoretical main-sequence stars based on stellar parameters deduced by Kurucz and Gray. In addition, we present a fitting formula for the wave energy flux based on the governing stellar and magnetic parameters. Methods. A modified theory of turbulence generation based on the mixing-length concept is combined with the magnetohydrodynamic equations to numerically account for the wave energies generated at the base of magnetic flux tubes. Results. The results indicate a stiff dependence of the generated wave energy on the stellar and magnetic parameters in principal agreement with previous studies. The wave energy flux FLTW decreases by about a factor of 1.7 between G0 V and K0 V stars, but drops by almost two orders of magnitude between K0 V and M0 V stars. In addition, the values for FLTW are significantly higher for lower in-tube magnetic field strengths. Both results are consistent with the findings from previous studies. Conclusions. Our study complements existing descriptions of magnetic energy generation in late-type main-sequence stars. Our results will be helpful for calculating theoretical atmospheric models for stars of different levels of magnetic activity.
Spectral description of the dynamics of ultracold interacting bosons in disordered lattices

We study the dynamics of a nonlinear one-dimensional disordered system from a spectral point of view. The spectral entropy and the Lyapunov exponent are extracted from the short-time dynamics, and are shown to give a pertinent characterization of the different dynamical regimes. The chaotic and self-trapped regimes are governed by log-normal laws whose origin is traced to the exponential shape of the eigenstates of the linear problem. These quantities satisfy scaling laws depending on the initial state and explain the system's behaviour at longer times.
Atomistic Green's Function Method supported by ab initio Calculations : Application to phonon transport in ZnO and ZnS

Abstract We present an approach to calculate ballistic phonon transport that combines the atomisticGreen’s function (AGF) method with ab initio results. For the inter atomic potential we usethe harmonic approach. The equilibrium positions of the atoms and the inter atomic force con-stants(ifcs) are calculated using the ABINIT program package [1], which is based on density func-tional theory. Therefore, the presented approach is parameter free. From the Green’s functionof the system we determine the density of states as well as the transmission function. The ther-mal conductance is obtained within the linear response regime. We apply this approach to bulkZnO and bulk ZnS. Transmission functions for diﬀerent transport direction for each material arepresented. A comparison of the transmission function shows, that a ZnO/ZnS interface could bea promising phonon blocker. Adding such interfaces in ZnO or ZnS based thermoelectric devicescould therefore increase the ﬁgure of merit. PACS numbers: 72.20. Pa, 73.40. -c, 71.55. Gs
Nucleosynthesis of r‐process elements by jittering jets in core‐collapse supernovae

We calculate the nucleosynthesis inside the hot bubble formed in the jittering-jets model for core-collapse supernova explosions, and find the formation of several times 10−4 M⊙ r-process elements. In the jittering-jets model, fast jets launched from a stochastic accretion disc around the newly formed neutron star are shocked at several thousand km, and form hot high-pressure bubbles. These bubbles merge to form a large bubble that explodes the star. In this study, we assume a spherically symmetric homogenous bubble, and follow its evolution for about 1 s during which nuclear reactions take place. The jets last for about 1 s, their velocity vj= 0.5c, and their total energy is ∼1051 erg. We use jets’ neutron enrichment independent of time, and follow the nuclear reactions to the formation of seed nuclei up to Z≤ 50, on which more neutrons will be absorbed to form r-process elements. Based on the mass of the seed nuclei, we find the r-process element mass in our idealized model to be several times 10−4 M⊙, which is slightly larger than the value deduced from observations. More realistic calculations that relax the assumptions of a homogenous bubble and constant-power jets’ composition might lead to agreement with observations.
THE ABUNDANCE OF MOLECULAR HYDROGEN AND ITS CORRELATION WITH MIDPLANE PRESSURE IN GALAXIES: NON-EQUILIBRIUM, TURBULENT, CHEMICAL MODELS

Observations of spiral galaxies show a strong linear correlation between the ratio of molecular to atomic hydrogen surface density Rmol and midplane pressure. To explain this, we simulate three-dimensional, magnetized turbulence, including simplified treatments of non-equilibrium chemistry and the propagation of dissociating radiation, to follow the formation of H2 from cold atomic gas. The formation timescale for H2 is sufficiently long that equilibrium is not reached within the 20–30 Myr lifetimes of molecular clouds. The equilibrium balance between radiative dissociation and H2 formation on dust grains fails to predict the time-dependent molecular fractions we find. A simple, time-dependent model of H2 formation can reproduce the gross behavior, although turbulent density perturbations increase molecular fractions by a factor of few above it. In contradiction to equilibrium models, radiative dissociation of molecules plays little role in our model for diffuse radiation fields with strengths less than 10 times that of the solar neighborhood, because of the effective self-shielding of H2. The observed correlation of Rmol with pressure corresponds to a correlation with local gas density if the effective temperature in the cold neutral medium of galactic disks is roughly constant. We indeed find such a correlation of Rmol with density. If we examine the value of Rmol in our local models after a free-fall time at their average density, as expected for models of molecular cloud formation by large-scale gravitational instability, our models reproduce the observed correlation over more than an order-of-magnitude range in density.
Search for the H dibaryon on the lattice

We investigate the H-dibaryon, an I(J P ) = 0(0 + ) with s = 2, in the chiral and continuum regimes on anisotropic lattices in quenched QCD. Simulations are performed on modest lattices with refined techniques to obtain results with high accuracy over a spatial lattice spacing in the range of as � 0.19 0.40 fm. We present results for the energy difference between the ground state energy of the hexa-quark stranglet and the free two-baryon state from our ensembles. A negative energy shift observed in the chirally extrapolated results leads to the conclusion that the measured hexa-quark state is bound. This is further confirmed by the attractive interaction in the continuum limit with the observed H-dibaryon bound by 47 ± 37MeV.
AN UPDATED LOOK AT BINARY CHARACTERISTICS OF MASSIVE STARS IN THE CYGNUS OB2 ASSOCIATION

This work provides a statistical analysis of the massive star binary characteristics in the Cygnus OB2 association using radial velocity information of 114 B3–O5 primary stars and orbital properties for the 24 known binaries. We compare these data to a series of Monte Carlo simulations to infer the intrinsic binary fraction and distributions of mass ratios, periods, and eccentricities. We model the distribution of mass ratio, log-period, and eccentricity as power laws and find best-fitting indices of α = 0.1 ± 0.5, β = 0.2 ± 0.4, and γ = −0.6 ± 0.3, respectively. These distributions indicate a preference for massive companions, short periods, and low eccentricities. Our analysis indicates that the binary fraction of the cluster is 44% ± 8% if all binary systems are (artificially) assumed to have P < 1000 days; if the power-law period distribution is extrapolated to 104 years, then a plausible upper limit for bound systems, the binary fraction is ∼90% ± 10%. Of these binary (or higher order) systems, ∼45% will have companions close enough to interact during pre- or post-main-sequence evolution (semi-major axis ≲4.7 AU). The period distribution for P < 26 days is not well reproduced by any single power law owing to an excess of systems with periods around 3–5 days (0.08–0.31 AU) and a relative shortage of systems with periods around 7–14 days (0.14–0.62 AU). We explore the idea that these longer-period systems evolved to produce the observed excess of short-period systems. The best-fitting binary parameters imply that secondaries generate, on average, ∼16% of the V-band light in young massive populations. This means that photometrically based distance measurements for young massive clusters and associations will be systematically low by ∼8% (0.16 mag in the distance modulus) if the luminous contributions of unresolved secondaries are not taken into account.
Quantum quenches and generalized Gibbs ensemble in a Bethe Ansatz solvable lattice model of interacting bosons

We consider quantum quenches in the so-called q-boson lattice model. We argue that the Generalized Eigenstate Thermalization Hypothesis holds in this model, therefore the Generalized Gibbs Ensemble (GGE) gives a valid description of the stationary states in the long time limit. For a special class of initial states (which are the pure Fock states in the local basis) we are able to provide the GGE predictions for the resulting root densities. We also give predictions for the long-time limit of certain local operators. In the q → ∞ limit the calculations simplify considerably, the wave functions are given by Schur polynomials and the overlaps with the initial states can be written as simple determinants. In two cases we prove rigorously that the GGE prediction for the root density is correct. Moreover, we calculate the exact time dependence of a physical observable (the one-site Emptiness Formation Probability) for the quench starting from the state with exactly one particle per site. In the long-time limit the GGE prediction is recovered.
The First Stars: Mass Growth Under Protostellar Feedback

We perform three-dimensional cosmological simulations to examine the growth of metal-free, Population III (Pop III) stars under radiative feedback. We begin our simulation at z = 100 and trace the evolution of gas and dark matter until the formation of the first minihalo. We then follow the collapse of the gas within the minihalo up to densities of n = 10 12 cm −3 , at which point we replace the high-density particles with a sink particle to represent the growing protostar. We model the effect of Lyman-Werner (LW) radiation emitted by the protostar, and employ a ray-tracing scheme to follow the growth of the surrounding H ii region over the next 5000 yr. We find that a disk assembles around the first protostar, and that radiative feedback will not prevent further fragmentation of the disk to form multiple Pop III stars. Ionization of neutral hydrogen and photodissociation of H2 by LW radiation leads to heating of the dense gas to several thousand Kelvin, and this warm region expands outward at the gas sound speed. Once the extent of this warm region becomes equivalent to the size of the disk, the disk mass declines while the accretion rate onto the protostars is reduced by an order of magnitude. This occurs when the largest sink has grown to � 20 M⊙ while the second sink has grown to � 7 M⊙, and we estimate the main sink will approach an asymptotic value of 30 M⊙ by the time it reaches the main sequence. Our simulation thus indicates that the most likely outcome is a massive Pop III binary. However, we simulate only one minihalo, and the statistical variation between minihaloes may be substantial. If Pop III stars were typically unable to grow to more than a few tens of solar masses, this would have important consequences for the occurence of pair-instability supernovae in the early Universe as well as the Pop III chemical signature in the oldest stars observable today.
Entanglement entropy with localized and extended interface defects

The quantum Ising chain of length, $L$, which is separated into two parts by localized or extended defects is considered at the critical point where scaling of the interface magnetization is nonuniversal. We measure the entanglement entropy between the two halves of the system in equilibrium, as well as after a quench, when the interaction at the interface is changed for time $tg0$. For the localized defect the increase in the entropy with $\text{log}\text{ }L$ or with $\text{log}\text{ }t$ involves the same effective central charge, which is a continuous function of the strength of the defect. On the contrary for the extended defect the equilibrium entropy is saturated but the nonequilibrium entropy has a logarithmic time dependence the prefactor of which depends on the strength of the defect.
CEPHEID PERIOD–LUMINOSITY RELATIONS IN THE NEAR-INFRARED AND THE DISTANCE TO M31 FROM THE HUBBLE SPACE TELESCOPE WIDE FIELD CAMERA 3

We present measurements of 68 classical Cepheids, most detected from the Canada–France–Hawaii Telescope POMME Survey, with periods from 10 to 78 days observed in the near-infrared by the Panchromatic Hubble Andromeda Treasury Program using the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope (HST). The combination of HST's resolution and the use of near-infrared measurements provide a dramatic reduction in the dispersion of the period–luminosity relation over the present optical, ground-based data. Even using random phase magnitudes we measure a dispersion of just 0.17 mag, implying a dispersion of just 0.12 mag for mean magnitudes. The error in the mean for this relation is 1% in distance. Combined with similar observations of Cepheids in other hosts and independent distance determinations, we measure a distance to M31 of μ0 = 24.38 ± 0.06(statistical) ± 0.03(systematic), 752 ± 27 kpc, in good agreement with past measurements though with a better, 3% precision here. The result is also in good agreement with independent distance determinations from two detached eclipsing binaries allowing for an independent calibration of the Cepheid luminosities and a determination of the Hubble constant.