Miracle-dz/UniFAR-FTUs huggingface dataset:
Hα ABSORPTION IN TRANSITING EXOPLANET ATMOSPHERES

Absorption of stellar Hα by the upper atmosphere of the planet HD 189733b has recently been detected by Jensen et al. Motivated by this observation, we have developed a model for atomic hydrogen in the n = 2 state and compared the resulting Hα line profile to the observations. The model atmosphere is in hydrostatic balance, as well as thermal and photoionization equilibrium. Collisional and radiative transitions are included in the determination of the n = 2 state level population. We find that Hα absorption is dominated by an optical depth τ ∼ 1 shell, composed of hydrogen in the metastable 2s state that is located below the hydrogen ionization layer. The number density of the 2s state within the shell is found to vary slowly with radius, while that of the 1s state falls rapidly. Thus while the Lyα absorption, for a certain wavelength, occurs inside a relatively well defined impact parameter, the contribution to Hα absorption is roughly uniform over the entire atomic hydrogen layer. The model can approximately reproduce the observed Lyα and Hα integrated transit depths for HD 189733b by using an ionization rate enhanced over that expected for the star by an order of magnitude. For HD 209458b, we are unable to explain the asymmetric Hα line profile observed by Jensen et al., as the model produces a symmetric line profile with transit depth comparable to that of HD 189733b. In an appendix, we study the effect of the stellar Lyα absorption on the net cooling rate.
New approach to cosmological bulk viscosity

Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235(Dated: September 18, 2014)We examine the cosmological consequences of an alternative to the standard expression for bulkviscosity, one which was proposed to avoid the propagation of superluminal signals without thenecessity of extending the space of variables of the theory. The Friedmann equation is derived forthis case, along with an expression for the eﬀective pressure. We ﬁnd solutions for the evolutionof the density of a viscous component, which diﬀers markedly from the case of conventional Eckarttheory; our model evolves toward late-time phantom-like behavior with a future singularity. Entropyproduction is addressed, and some similarities and diﬀerences to approaches based on the Mueller-Israel-Stewart theory are discussed.I. INTRODUCTION
Stakeholder engagement and corporate performances: Empirical evidence from an emerging economy

From inception to execution, United Nations Sustainable Development Goals (SDGs) are based on multi-stakeholder partnerships. Therefore, SDGs can be described as a pragmatic stakeholder engagement model. In this research article, the impact of the adoption of SDGs by firms on their financial, environmental, and social performance is examined. Based on the publication of sustainability reporting by firms in compliance with GRI standards, 89 selected Indian firms from the NSE 500 were included in the content analysis for data collection. In addition, multiple linear regression was used to analyse secondary data to establish an empirical relationship between SDGs adoption and corporate performance. The findings of this study revealed that the adoption of SDGs by firms is significantly and positively associated with their financial, environmental, and social performances. This article contributes to academic knowledge on sustainable development and provides important implications for researchers, practitioners, and policymakers. This article contributes to academic knowledge of sustainable development and corporate performance and provides important implications for researchers, practitioners, and policymakers
Invariance of Pontrjagin classes for Bott manifolds

A Bott manifold is the total space of some iterated $\mathbb C P^1$-bundle over a point. We prove that any graded ring isomorphism between the cohomology rings of two Bott manifolds preserves their Pontrjagin classes. Moreover, we prove that such an isomorphism is induced from a diffeomorphism if the Bott manifolds are $\mathbb Z/2$-trivial, where a Bott manifold is called $\mathbb Z/2$-trivial if its cohomology ring with $\mathbb Z/2$-coefficient is isomorphic to that of a product of $\mathbb C P^1$'s.
Kinematics comparison of squat (2D vs 3D analysis) for remote learning – pilot study

Bodyweight squats are a common exercise in athletic training and rehabilitation due to their biomechanical and neuromuscular similarities to fundamental movements in a variety of sports and their requirements of coordination of major joints and numerous muscle groups (Schoenfeld, 2010). They are essential for kinesiology students, whose future careers often include athletic training and rehabilitation, to learn how to analyze the kinematics of a squat. While 3D movement analysis is considered the gold standard for motion capture (Chung & Ng, 2012), 2D digital video analysis is more commonly chosen in education environments to provide hands-on experience. However, few studies have investigated the differences between 2D and 3D analysis of squats (Escamilla et al., 2001; Krause et al., 2015; Schmitz et al., 2015). Therefore, the current study aims to compare 2D and 3D measurements of narrow-stance squats while enhancing learning by engaging students with hands-on experience using free, open-source software. Fifteen healthy adults (nine females, six males, 26.93 ± 9.04 years old) participated in this study. Following proper COVID safety guidelines, 2D analyses were performed by undergraduate students at home while 3D analyses were performed using a motion capture system in the laboratory. Lower extremity joint angles and displacements were calculated using 2D and 3D methods. Statistical significances were found when comparing the differences between both measurements except for hip flexion. Nonetheless, the resulting angular and linear measurements from both 2D and 3D analyses aligned with previous research, suggesting that 2D digital video analysis is a viable option for educational purposes despite the significant differences.
Creating effective brand names with sound symbolic mappings

Background: The present study was designed to investigate the use of sound symbolic mappings in fictitious brand names. Sound symbolic mappings refer to the existence of a nonarbitrary relationship between individual sounds and associations of different attributes and concepts. Given that sounds have inherent meaning in them, brand names in line with the established symbolic effects could communicate tailored messages that are congruent with consumer expectations of a product. Purpose: As perceived congruency between a product and its label is highly desirable in marketing, the study sets out to test the noted effects in brand names. It was aimed to confirm the strength of sound symbolic effects through greater preference for names with a symbolic fit with the product. Study design/methodology/approach: Two product categories were chosen, and a set of fictitious brand names were created. The names differed only on the sounds purported to convey targeted symbolic associations of salient product characteristics. The participants were presented with a forced choice task consisting of paired name samples and a stated product category for each pair. Finding/conclusions: The results confirmed the presence of sound symbolic effects as participants favoured the names with embedded symbolism. This leads to a conclusion that sound symbolism may be used to affect consumer choices based on brand name preference. Limitations/future research: Even though the study included only two products and used forced choice tasks limited on name pairs, the findings clearly imply the potential of sound symbolic mappings in creating efficient brand names. Broadening the research to other products and the service sector would surely deliver intriguing results.
SUBSTRUCTURE IN THE STELLAR HALOS OF THE AQUARIUS SIMULATIONS

We characterize the substructure in the simulated stellar halos of Cooper et al. which were formed by the disruption of satellite galaxies within the cosmological N-body simulations of galactic halos of the Aquarius project. These stellar halos exhibit a wealth of tidal features: broad overdensities and very narrow faint streams akin to those observed around the Milky Way. The substructures are distributed anisotropically on the sky, a characteristic that should become apparent in the next generation of photometric surveys. The normalized RMS of the density of stars on the sky appears to be systematically larger for our halos compared with the value estimated for the Milky Way from main-sequence turnoff stars in the Sloan Digital Sky Survey. We show that this is likely to be due in part to contamination by faint QSOs and redder main-sequence stars, and might suggest that ∼10% of the Milky Way halo stars have formed in situ.
Collaborative and Conditional Deep Adversarial Network for Intelligent Bearing Fault Diagnosis

In real applications, the data distribution may be inconsistent due to the different working conditions of the equipment, resulting in significant performance degradation of a well-trained faults diagnosis model. To this end, unsupervised domain adaptation (UDA) technique is proposed to bridge the distribution gap between the source and the target domain. Most studies on UDA-based faults diagnosis put much attention on extracting domain-invariant features without considering how to improve the discriminant capability of these features in the target domain. In this study, the collaborative and conditional deep adversarial network (CCDAN) is proposed for cross-domain bearing faults diagnosis. In CCDAN, characteristic fault features at different scales are learned and utilized for domain adaptation. The domain classifier at each scale is fed with discriminative information conveyed in the label predictions, resulting in better alignment of feature distributions per class between different domains. By collaborative and adversarial learning (CAL) across different scales, the learned features are expected to be domain-invariant and also discriminant for faults diagnosis in the target domain. In addition, the multiple kernel variant of maximum mean discrepancies (MK-MMDs) is introduced to further reduce the feature distribution discrepancy. Experiments performed on two different datasets proved the effectiveness and superiority of our model.
Helicity protected ultrahigh mobility Weyl fermions in NbP

Noncentrosymmetric transition-metal monopnictides, including TaAs, TaP, NbAs, and NbP, are emergent topological Weyl semimetals (WSMs) hosting exotic relativistic Weyl fermions. In this Rapid Communication, we elucidate the physical origin of the unprecedented charge carrier mobility of NbP, which can reach $1\ifmmode\times\else\texttimes\fi{}{10}^{7}\phantom{\rule{0.28em}{0ex}}{\mathrm{cm}}^{2}{\phantom{\rule{0.16em}{0ex}}\mathrm{V}}^{\ensuremath{-}1}{\phantom{\rule{0.16em}{0ex}}\mathrm{s}}^{\ensuremath{-}1}$ at 1.5 K. Angle- and temperature-dependent quantum oscillations, supported by density function theory calculations, reveal that NbP has the coexistence of $p$- and $n$-type WSM pockets in the ${k}_{z}=1.16\ensuremath{\pi}/c$ plane (W1-WSM) and in the ${k}_{z}=0$ plane near the high symmetry points $\mathrm{\ensuremath{\Sigma}}$ (W2-WSM), respectively. Uniquely, each W2-WSM pocket forms a large dumbbell-shaped Fermi surface enclosing two neighboring Weyl nodes with the opposite chirality. The magnetotransport in NbP is dominated by these highly anisotropic W2-WSM pockets, in which Weyl fermions are well protected from defect backscattering by real spin conservation associated to the chiral nodes. However, with a minimal doping of $\ensuremath{\sim}1%$ Cr, the mobility of NbP is degraded by more than two orders of magnitude, due to the invalidity of helicity protection to magnetic impurities. Helicity protected Weyl fermion transport is also manifested in chiral anomaly induced negative magnetoresistance, controlled by the W1-WSM states. In the quantum regime below 10 K, the intervalley scattering time by impurities becomes a large constant, producing the sharp and nearly identical conductivity enhancement at low magnetic field.
Click Chemistry: A Promising Tool for Building Hierarchical Structures

The hierarchical structures are utilized at different levels in nature. Moreover, a wide spectrum of nature’s properties (e.g., mechanical, physical and biological properties) has been attributed to this hierarchy. Different reviews have been published to cover the use of click chemistry in building hierarchical structures. However, each one of those reviews focused on a narrow area on this topic, i.e., specific chemical reaction, such as in thiol-ene chemistry, or a specific molecule or compound such as polyhedral oligomeric silsesquioxane, or a certain range of hierarchical structures between the nano to micro range, e.g., nanocrystals. In this review, a frame to connect the dots between the different published works has been demonstrated. This article will not attempt to give an exhaustive review of all the published work in the field, instead the potential of click chemistry to build hierarchical structures of different levels using building blocks of different length scales has been shown through two main approaches. The first is a one-step direct formation of 3D micro/macrometer dimensions structures from Pico dimensions structures (molecules, monomers, etc.). The second approach includes several steps Pico ➔ 0D nano ➔ 1D nano ➔ 2D nano ➔ 3D nano/micro/macro dimensions structures. Another purpose of this review article is to connect between (a) the atomic theory, which covers the atoms and molecules in the picometer dimensions (picoscopic chemistry set); (b) “nano-periodic system” model, which covers different nanobuilding blocks in the nanometers range such as nanoparticles, dendrimers, buckyball, etc. which was developed by Tomalia; and (c) the micro/macrometer dimensions level.
Perpendicular magnetic anisotropy and the magnetization process in CoFeB/Pd multilayer films

The perpendicular magnetic anisotropy (PMA) and dynamic magnetization-reversal process in [CoFeB t nm/Pd 1.0 nm]n(t = 0.4, 0.6, 0.8, 1.0 and 1.2 nm; n = 2 − 20) multilayer films have been studied by means of magnetic hysteresis and Kerr effect measurements. Strong and controllable PMA with an effective uniaxial anisotropy up to 7.7 × 106 Jm−3 and a saturation magnetization as low as 200 emu cm−3 are achieved. The surface/interfacial anisotropy of the CoFeB/Pd interfaces—the main contribution to the PMA—is separated from the effective uniaxial anisotropy of the films and appears to increase with the number of CoFeB/Pd bilayers. Observation of the magnetic domains during a magnetization-reversal process, using polar magneto-optical Kerr microscopy, reveals the detailed behavior of the nucleation and displacement of the domain walls.
CLUSTERING OF MODERATE LUMINOSITY X-RAY-SELECTED TYPE 1 AND TYPE 2 AGNS AT Z ∼ 3

We investigate, for the first time at z ∼ 3, the clustering properties of 189 Type 1 and 157 Type 2 X-ray active galactic nuclei (AGNs) of moderate luminosity (〈Lbol〉 = 1045.3 erg s−1), with photometric or spectroscopic redshifts in the range 2.2 < z < 6.8. These samples are based on Chandra and XMM-Newton data in COSMOS. We find that Type 1 and Type 2 COSMOS AGNs at z ∼ 3 inhabit DMHs with typical mass of log Mh = 12.84 and 11.73 h−1M☉, respectively. This result requires a drop in the halo masses of Type 1 and 2 COSMOS AGNs at z ∼ 3 compared to z ≲ 2 XMM-COSMOS AGNs with similar luminosities. Additionally, we infer that unobscured COSMOS AGNs at z ∼ 3 reside in 10 times more massive halos compared to obscured COSMOS AGNs, at the 2. 6σ level. This result extends to z ∼ 3 the results found in COSMOS at z ≲ 2, and rules out the picture in which obscuration is purely an orientation effect. A model which assumes that the AGNs activity is triggered by major mergers is quite successful in predicting both the low halo mass of COSMOS AGNs and the typical mass of luminous SDSS quasars at z ∼ 3, with the latter inhabiting more massive halos respect to moderate luminosity AGNs. Alternatively we can argue, at least for Type 1 COSMOS AGNs, that they are possibly representative of an early phase of fast (i.e., Eddington limited) BH growth induced by cosmic cold flows or disk instabilities. Given the moderate luminosity, these new fast growing BHs have masses of ∼107–8 M☉ at z ∼ 3 which might evolve into ∼108.5–9 M☉ mass BHs at z = 0. Following our clustering measurements, we argue that this fast BH growth at z ∼ 3 in AGNs with moderate luminosity occurs in DMHs with typical mass of ∼ 6× 1012 h−1M☉.
A study of low-metallicity DLAs at high redshift and C ii* as a probe of their physical conditions

We present a detailed high spectral resolution (R $\sim$ 40000) study of five high-z damped Lyman $\alpha$ systems (DLAs) and one sub-DLA detected along four QSO sightlines. Four of these DLAs are very metal-poor with [Fe/H] $\le$ $-$2. One of them, at z$_{abs}$ = 4.20287 towards J0953$-$0504, is the most metal-poor DLA at z $>$ 4 known till date. This system shows no enhancement of C over Fe and O, and standard Population II star yields can explain its relative abundance pattern. The DLA at z$_{abs}$ = 2.34006 towards J0035$-$0918 has been claimed to be the most carbon-enhanced metal-poor DLA. However, we show that thermal broadening is dominant in this system and, when this effect is taken into account, the measured carbon enhancement ([C/Fe] = 0.45 $\pm$ 0.19) becomes $\sim$ 10 times less than what was reported previously. The gas temperature in this DLA is estimated to be in the range of 5000 $-$ 8000 K, consistent with a warm neutral medium phase. From photoionization modelling of two of the DLAs showing C II* absorption, we find that the metagalactic background radiation alone is not sufficient to explain the observed C II* cooling rate, and local heating sources, probably produced by in-situ star formation, are needed. Cosmic ray heating is found to contribute $\gtrsim$ 60% to the total heating in these systems. Using a sample of metal-poor DLAs with C II* measurements, we conclude that the cosmic ray ionization rate is equal to or greater than that seen in the Milky Way in $\sim$ 33% of the systems with C II* detections.
The Monitor Project: stellar rotation at 13 Myr - I. A photometric monitoring survey of the young open cluster h Persei

We aim at constraining the angular momentum evolution of low mass stars by measuring their rotation rates when they begin to evolve freely towards the ZAMS, i.e. after the disk accretion phase has stopped. We conducted a multi-site photometric monitoring of the young open cluster h Persei that has an age of ~13 Myr. The observations were done in the I-band using 4 different telescopes and the variability study is sensitive to periods from less than 0.2 day to 20 days. Rotation periods are derived for 586 candidate cluster members over the mass range 0.4 10 Myr). The results are consistent with models that assume significant core-envelope decoupling during the angular momentum evolution to the ZAMS.
Is the 2MASS clustering dipole convergent

There is a long-standing controversy about the convergence of the dipole moment of the galaxy angular distribution (the so-called clustering dipole). We study the growth of the clustering dipole of galaxies as a function of the limiting flux of the sample from the Two Micron All Sky Survey (2MASS). Contrary to some earlier claims, we find that the dipole does not converge before the completeness limit of the 2MASS Extended Source Catalog, i.e. up to 13.5 mag in the near-infrared K_s band (equivalent to an effective distance of 300 Mpc/h). We compare the observed growth of the dipole with the theoretically expected, conditional one (i.e., given the velocity of the Local Group relative to the CMB), for the LambdaCDM power spectrum and cosmological parameters constrained by WMAP. The observed growth turns out to be within 1-sigma confidence level of its theoretical counterpart once the proper observational window of the 2MASS flux-limited catalog is included. For a contrast, if the adopted window is a top-hat, then the predicted dipole grows significantly faster and converges to its final value for a distance of about 300 Mpc/h. By comparing the observational windows, we show that for a given flux limit and a corresponding distance limit, the 2MASS flux-weighted window passes less large-scale signal than the top-hat one. We conclude that the growth of the 2MASS dipole for effective distances greater than 200 Mpc/h is only apparent. On the other hand, for a distance of 80 Mpc/h (mean depth of the 2MASS Redshift Survey) and the LambdaCDM power spectrum, the true dipole is expected to reach only ~80% of its final value. Eventually, since for the window function of 2MASS the predicted growth is consistent with the observed one, we can compare the two to evaluate beta = (Omega_m)^0.55 / b. The result is beta = 0.38+-0.04, which leads to an estimate of the density parameter Omega_m = 0.20+-0.08.
Inhibitory Effect of GRAS Essential Oils and Plant Extracts on the Growth of Aspergillus westerdijkiae and Aspergillus carbonarius Strains

The effect of essential oils (obtained using hydrodistillation) and plant extracts (ethanolic, aqueous, and hexanic extractions) of 10 different plants cultivated in Brazil were tested using the diffusion agar method, with the objective of evaluating the inhibitory effect of the oils and extracts on the mycelial growth of Aspergillus westerdijkiae NRRL 3174 and A. carbonarius RC 2054 (UNRC). Of the 40 essential oils and plant extracts analyzed, oregano essential oil and plant extract, rosemary essential oil, and the clove ethanolic extract were the best choice to obtain the growth parameters (radial growth rates (mm day−1) and lag phase (h)) due the good results presented and the volume of oil/extract obtained. Comparing all the essential oils and plant extracts that were tested for growth parameters, the best results were obtained for the clove ethanolic extract for both strains assayed. These results demonstrated an outstanding potential use of some of these products in prevention of fungal contamination in food. However, further studies need to be conducted to determine the ability of these oils and extracts to inhibit or reduce ochratoxin A production.
Evaluating the Psychometric Properties of Persian Version of the Pain Resilience Scale in Cancer Patients

Background: Pain resilience can protect cancer patients from emotional turmoil as a protective factor in adapting to chronic pain. Objectives: This study aimed to evaluate cancer patients’ psychometric properties in the Persian version of the Pain Resilience Scale. Methods: This methodological study was conducted on 200 patients with cancer, who referred to the chemotherapy section of Imam Reza Hospital in Kermanshah, Iran in 2021 to examine the psychometric properties of the Persian version of the Ankawi Pain Resilience Scale. The subjects were selected through purposive sampling method based on inclusion criteria. Results: The results indicated that Cronbach’s alpha coefficient was obtained under the Behavioral Perseverance Scale (α = 0.86), Emotional/Cognitive Positive Thinking Scale (α = 0.93), and the whole Scale (α = 0.94). According to the exploratory factor analysis, this scale explained 65% of the variance of the pain resilience variable. The confirmatory factor analysis results confirmed that a two-factor model is a good fit for the data. Conclusion: According to the results, the pain resilience scale had an acceptable validity in people with cancer.