Miracle-dz/UniFAR-FTUs huggingface dataset:
ON THE EXCESS OF ULTRA-HIGH ENERGY COSMIC RAYS IN THE DIRECTION OF CENTAURUS A

A posteriori anisotropy study of ultra-high energy cosmic rays (UHECRs) with the Pierre Auger Observatory (PAO) has shown evidence of an excess of cosmic-ray particles above 55 EeV within 18° of the direction of the radio galaxy Centaurus A. However, the origin of the excess remains elusive. We simulate the propagation of different species of particles coming from the direction of Centaurus A in the Galactic magnetic fields and find that only particles of nuclear charge Z ≲ 10 can avoid being deflected outside of the 18° window of Centaurus A. On the other hand, considering the increasingly heavy composition of UHECRs at the highest energies measured by PAO, a plausible scenario for cosmic rays from the direction of Centaurus A can be found if they consist of intermediate-mass nuclei. The chemical composition of cosmic rays can be further constrained by lower-energy cosmic rays of the same rigidity. We find that cosmic-ray acceleration in the lobes of Centaurus A is not favored, while acceleration in the stellar winds that are rich in intermediate-mass nuclei could meet the requirement. This suggests that the observed excess may originate from cosmic-ray accelerators induced by stellar explosions in the star-forming regions of Centaurus A and/or the Centaurus cluster located behind Centaurus A.
Survey on Emotion Sensing Using Mobile Devices

The rapid development and ubiquity of mobile and wearable devices promises to enable researchers to monitor users’ granular emotional data in a less intrusive manner. Researchers have used a wide variety of mobile and wearable devices for this purpose, and have proposed various approaches to sense users’ emotional states. In this survey, we utilise three established digital libraries (ACM Digital Library, IEEE Xplore Digital Library, and Springer Nature). We analysed and critically assessed the different approaches used in the three stages (perception, learning, inference) of a typical mobile emotion sensing framework, following a structured paper selection process. The contribution of this survey is three-fold; first, we document all the latest relevant literature on mobile emotion sensing research; second, we describe how mobile and wearable devices use their sensing and computing capabilities to monitor human emotions; third, we discuss challenges and opportunities of mobile emotion sensing to demonstrate the potential of this thriving field of research.
Nonlinear low-frequency collisional quantum Buneman instability

The Buneman instability occurring when an electron population is drifting with respect to the ions is analyzed in the quantum linear and nonlinear regimes. The one-dimensional low-frequency and collisional model of Shokri and Niknam (Phys. Plasmas, 12 (2005) 062110) is revisited introducing the Bohm potential term in the momentum equation. The linear regime is investigated analytically, and quantum effects result in a reduction of the instability. The nonlinear regime is then assessed both numerically and analytically, and pure quantum density oscillations are found to appear during the late evolution of the instability.
Testing for a pure state with local operations and classical communication

We examine the problem of using local operations and classical communication (LOCC) to distinguish a known pure state from an unknown (possibly mixed) state, bounding the error probability from above and below. We study the asymptotic rate of detecting multiple copies of the pure state and show that, if the overlap of the two states is great enough, then they can be distinguished asymptotically as well with LOCC as with global measurements; otherwise, the maximal Schmidt coefficient of the pure state is sufficient to determine the asymptotic error rate.
PITCH ANGLE RESTRICTIONS IN LATE-TYPE SPIRAL GALAXIES BASED ON CHAOTIC AND ORDERED ORBITAL BEHAVIOR

We built models for low bulge mass spiral galaxies (late type as defined by the Hubble classification) using a three-dimensional self-gravitating model for spiral arms, and analyzed the orbital dynamics as a function of pitch angle, ranging from 10° to 60°. Indirectly testing orbital self-consistency, we search for the main periodic orbits and studied the density response. For pitch angles up to approximately ∼20°, the response closely supports the potential readily permitting the presence of long-lasting spiral structures. The density response tends to “avoid” larger pitch angles in the potential by keeping smaller pitch angles in the corresponding response. Spiral arms with pitch angles larger than ∼20° would not be long-lasting structures but would rather be transient. On the other hand, from an extensive orbital study in phase space, we also find that for late-type galaxies with pitch angles larger than ∼50°, chaos becomes pervasive, destroying the ordered phase space surrounding the main stable periodic orbits and even destroying them. This result is in good agreement with observations of late-type galaxies, where the maximum observed pitch angle is ∼50°.
I lack ‘me-time’: The experiences of family caregivers of elders with Diabetes Mellitus in a selected village in South Africa

Background Family caregiving is common in African countries where the family plays a crucial role in caring and supporting a family member in need of care. Most older people who suffer from chronic diseases, including Diabetes Mellitus, stay at home where family members and relatives are responsible for their day-to-day care. Aim The purpose of this study was to explore the experiences of family caregivers of older people living with Diabetes Mellitus in a rural village in South Africa. Setting This study was conducted in a village located in the Thulamela municipality of the Vhembe district, in the Limpopo province. Methods A qualitative exploratory, descriptive research design was used. Purposive sampling was used, and data were collected using a semi-structured interview guide. Data saturation occurred after interviewing 17 participants and were analysed using thematic analysis. Trustworthiness was ensured through strategies of credibility, dependability, conformability, and transferability, and ethical principles were applied. Results Three themes emerged: participants sacrificed time for work, time for self-care, and devised coping strategies. These findings revealed that family caregivers of older adults diagnosed with Diabetes Mellitus sacrificed their time in order to provide care. However, the findings further revealed that family caregivers devised strategies to cope through prayer and acceptance. Conclusion The study revealed several challenges experienced by family caregivers of older people living with Diabetes Mellitus. Contribution The National Department of Health, together with the civil society would gain an in-depth understanding of the burden of Diabetes Mellitus in the family setting and develop strategies to improve the situation.
Bioinformatics analysis identifies ferroptosis‑related genes in the regulatory mechanism of myocardial infarction

Since ferroptosis is considered to be a notable cause of cardiomyocyte death, inhibiting ferroptosis has become a novel strategy in reducing cardiac cell death and improving cardiopathic conditions. Therefore, the aim of the present study was to search for ferroptosis-related hub genes and determine their diagnostic value in myocardial infarction (MI) to aid in the diagnosis and treatment of the disease. A total of 10,286 DEGs were identified, including 6,822 upregulated and 3.464 downregulated genes in patients with MI compared with healthy controls. After overlapping with ferroptosis-related genes, 128 ferroptosis-related DEGs were obtained. WGCNA successfully identified a further eight functional modules, from which the blue module had the strongest correlation with MI. Blue module genes and ferroptosis-related differentially expressed genes were overlapped to obtain 20 ferroptosis-related genes associated with MI. Go and KEGG analysis showed that these genes were mainly enriched in cellular response to chemical stress, trans complex, transferring, phosphorus-containing groups, protein serine/threonine kinase activity, FoxO signaling pathway. Hub genes were obtained from 20 ferroptosis-related genes through the PPI network. The expression of hub genes was found to be down-regulated in the MI group. Finally, the miRNAs-hub genes and TFs-hub genes networks were constructed. The GSE141512 dataset and the use of RT-qPCR assays on patient blood samples were used to confirm these results. The results showed that ATM, PIK3CA, MAPK8, KRAS and SIRT1 may play key roles in the development of MI, and could therefore be novel markers or targets for the diagnosis or treatment of MI.
X-Ray Emissions from Accreting White Dwarfs: A Review

Interacting binaries in which a white dwarf accretes material from a companion—cataclysmic variables (CVs) in which the mass donor is a Roche-lobe filling star on or near the main sequence, and symbiotic stars in which the mass donor is a late type giant—are relatively commonplace. They display a wide range of behaviors in the optical, X-rays, and other wavelengths, which still often baffle observers and theorists alike. Here I review the existing body of research on X-ray emissions from these objects for the benefits of both experts and newcomers to the field. I provide introductions to the past and current X-ray observatories, the types of known X-ray emissions from these objects, and the data analysis techniques relevant to this field. I then summarize of our knowledge regarding the X-ray emissions from magnetic CVs, non-magnetic CVs and symbiotic stars, and novae in eruption. I also discuss space density and the X-ray luminosity functions of these binaries and their contribution to the integrated X-ray emission from the Galaxy. I then discuss open questions and future prospects.
Li – O anti-correlation in NGC 6752: evidence for Li-enriched polluting gas

Context. Elemental correlations and anti-correlations are known to be present in globular clusters (GCs) owing to pollution by CNO cycled gas. Because of its fragility Li is destroyed at the temperature at which the CNO cycling occurs, and this makes Li a crucial study for the nature of the contaminating stars. Aims. We observed 112 un-evolved stars at the Turnoff of the NGC 6752 cluster with FLAMES at the VLT to investigate the presence and the extent of a Li-O correlation. This correlation is expected if there is a simple pollution scenario. Methods. Li (670.8 nm) and O triplet (771 nm) abundances are derived in NLTE. All stars belong to a very narrow region of the color-magnitude diagram, so they have similar stellar parameters (Teff ,l ogg). Results. We find that O and Li correlate, with a high statistical significance that confirms the early results for this cluster. At first glance this is what is expected if a simple pollution of pristine gas with CNO cycled gas (O-poor, Li-poor) occurred. The slope of the relationship, however, is about 0.4, and differs from unity by over 7σ. A slope of one is the value predicted for a pure contamination model. Conclusions. We confirm an extended Li-O correlation in non evolved stars of NGC 6752. At the same time the characteristic of the correlation shows that a simple pollution scenario is not sufficient to explain the observations. Within this scenario the contaminant gas must have been enriched in Li. This would rule out massive stars as main polluters, and favor the hypothesis that the polluting gas was enriched by intermediate or high-mass AGB stars, unless the former can be shown to be able to produce Li. According to our observations, the fraction of polluting gas contained in the stars observed is a considerable fraction of the stellar mass of the cluster.
Star formation in the outer Galaxy: membership and fundamental parameters of the young open cluster NGC 1893

Context. Different environmental conditions can play a crucial role in determining final products of the star formation process, and in this context, less favorable activities of star formation are expected in the external regions of our Galaxy. Aims. We studied the properties of the young open cluster NGC 1893 located about 12 Kpc from the galactic center, to investigate how different physical conditions can affect the process of star formation. Methods. By adopting a multiwavelength approach, we compiled a catalog extending from X-rays to NIR data to derive the cluster membership. In addition, optical and NIR photometric properties are used to evaluate the cluster parameters. Results. We find 415 diskless candidate members and 1061 young stellar objects with a circumstellar disk or class II candidate members, 125 of which are also Hα emitters. Considering the diskless candidate members, we find that the cluster distance is 3.6 ± 0.2 kpc and the mean interstellar reddening is E(B − V) = 0.6 ± 0.1 with evidence of differential reddening in the whole surveyed region. Conclusions. NGC 1893 contains a conspicuous population of pre-main sequence stars, together with the well-studied main sequence cluster population. We found a disk fraction of about 70% similar to the one found in clusters of similar age in the solar neighbor and then, despite expected unfavorable conditions for star formation, we conclude that very rich young clusters can also form in the outer regions of our Galaxy.
Isotope and density profile effects on pedestal neoclassical transport

Cross-field neoclassical transport of heat, particles and momentum is studied in sharp density pedestals, with a focus on isotope and profile effects, using a radially global approach. Global effects—which tend to reduce the peak ion heat flux, and shift it outward—increase with isotope mass for fixed profiles. The heat flux reduction exhibits a saturation with a favorable isotopic trend. A significant part of the heat flux can be convective even in pure plasmas, unlike in the plasma core, and it is sensitive to how momentum sources are distributed between the various species. In particular, if only ion momentum sources are allowed, in global simulations of pure plasmas the ion particle flux remains close to its local value, while this may not be the case for simulations with isotope mixtures or electron momentum sources. The radial angular momentum transport that is a finite orbit width effect, is found to be strongly correlated with heat sources.
Oscillatory localization of quantum walks analyzed by classical electric circuits

Discrete-time quantum walks are well-known for exhibiting localization, a quantum phenomenon where the walker remains at its initial location with high probability. In companion with a joint Letter, we introduce oscillatory localization, where the walker alternates between two states. The walk is given by the flip-flop shift, which is easily defined on non-lattice graphs, and the Grover coin. Extremely simple examples of the localization exist, such as a walker jumping back and forth between two vertices of the complete graph. We show that only two kinds of states, called flip states and uniform states, exhibit exact oscillatory localization. So the projection of an arbitrary state onto these gives a lower bound on the extent of oscillatory localization. Thus we completely characterize the states that oscillate under the quantum walk.
The unperformed experiment as an act of annihilation

Here, we accept the results of quantum experiments at face value and we make no apology for the failure of classical physics. Just as Wheeler has called particle detection an "act of creation", we suggest that, in some circumstances, not detecting the particle might be considered an "act of annihilation". We propose a delayed choice experiment in which we decide to interrupt an experiment after the particle has supposedly passed through the preparation apparatus and is on the verge of being detected. Even with the detection device in place, the particle is nowhere to be found.
A proposal of searching for the $\Upsilon(6S)$ hadronic decays into $\Upsilon(nS)$ plus $\eta^{(\prime)}$

In this work, we propose a possible experimental research topic on the $\Upsilon(6S)\to \Upsilon(nS)\eta^{(\prime)}$ ($n=1,2,3$) transitions. Considering the hadronic loop effect from the intermediate $S$-wave $B_{(s)}$ and $B_{(s)}^*$ mesons, we estimate the partial decay widths and the corresponding branching ratios of the $\Upsilon(6S)\to \Upsilon(nS)\eta^{(\prime)}$ hadronic decays, which become considerably large. With the running of the Belle II experiment, it becomes possible to explore these $\Upsilon(6S)\to \Upsilon(nS)\eta^{(\prime)}$ transitions.
VARIABLE RADIO SOURCES IN THE GALACTIC PLANE

Using three epochs of Very Large Array observations of the Galactic plane in the first quadrant taken ∼15 years apart, we have conducted a search for a population of variable Galactic radio emitters in the flux density range 1–100 mJy at 6 cm. We find 39 variable sources in a total survey area of 23.2 deg2. Correcting for various selection effects and for the extragalactic variable population of active galactic nuclei, we conclude there are ∼1.6 deg−2 Galactic sources which vary by more than 50% on a time scale of years (or shorter). We show that these sources are much more highly variable than extragalactic objects; more than 50% show variability by a factor >2 compared to <10% for extragalactic objects in the same flux density range. We also show that the fraction of variable sources increases toward the Galactic center (another indication that this is a Galactic population), and that the spectral indices of many of these sources are flat or inverted. A small number of the variables are coincident with mid-IR sources and two are coincident with X-ray emitters, but most have no known counterparts at other wavelengths. Intriguingly, one lies at the center of a supernova remnant, while another appears to be a very compact planetary nebula; several are likely to represent activity associated with star formation regions. We discuss the possible source classes which could contribute to the variable cohort and follow-up observations which could clarify the nature of these sources.
Modelling non‐linear redshift‐space distortions in the galaxy clustering pattern: systematic errors on the growth rate parameter

We investigate the ability of state-of-the-art redshift-space distortion models for the galaxy anisotropic two-point correlation function, ξ(r⊥, r∥), to recover precise and unbiased estimates of the linear growth rate of structure f, when applied to catalogues of galaxies characterized by a realistic bias relation. To this aim, we make use of a set of simulated catalogues at z = 0.1 and 1 with different luminosity thresholds, obtained by populating dark matter haloes from a large N-body simulation using halo occupation prescriptions. We examine the most recent developments in redshift-space distortion modelling, which account for non-linearities on both small and intermediate scales produced, respectively, by randomized motions in virialized structures and non-linear coupling between the density and velocity fields. We consider the possibility of including the linear component of galaxy bias as a free parameter and directly estimate the growth rate of structure f. Results are compared to those obtained using the standard dispersion model, over different ranges of scales. We find that the model of Taruya et al., the most sophisticated one considered in this analysis, provides in general the most unbiased estimates of the growth rate of structure, with systematic errors within ±4 per cent over a wide range of galaxy populations spanning luminosities between L > L* and L > 3L*. The scale dependence of galaxy bias plays a role on recovering unbiased estimates of f when fitting quasi-non-linear scales. Its effect is particularly severe for most luminous galaxies, for which systematic effects in the modelling might be more difficult to mitigate and have to be further investigated. Finally, we also test the impact of neglecting the presence of non-negligible velocity bias with respect to mass in the galaxy catalogues. This can produce an additional systematic error of the order of 1–3 per cent depending on the redshift, comparable to the statistical errors the we aim at achieving with future high-precision surveys such as Euclid.
Trust, Power, and Tax Risk into the “Slippery Slope”: A Corporate Tax Compliance Model

(1) Background: There are still few studies that discuss corporate tax risk, especially those related to tax compliance and the Slippery Slope Framework. Meanwhile, in practice, tax risk, which is tax uncertainty, is essential in corporate tax compliance. Tax risk has not been discussed in the Slippery Slope Framework in previous research, which has become a reference in various tax compliance studies. Therefore, this study aims to analyze the effect of tax risk induced into the slippery slope framework at corporate taxpayer compliance. Dynamic interactions between power, trust, and tax risk (TPR) in one framework are essential to see the tax compliance model’s determinants comprehensively; (2) Methods: We defined our model using a mathematical and economic approach with a Likert scale, as well as geometrical inferences based on the Slippery Slope Framework. (3) Results: This study found that tax risk affects the effort and tendency of corporate taxpayers to comply. The level of tax risk will make it easier or more difficult for corporate taxpayers to comply. Tax risk will affect the level of tax compliance regardless of the quality of trust and existing power; (4) Conclusions: This research’s theoretical contributions are that trust and power are determinants of tax compliance and that tax risk influences companies to be more compliant. This model is to complete the conceptual gap of the determinants of tax compliance from the perspective of the Slippery Slope Framework. The practical implication is that corporate taxpayers should manage tax risk to avoid unexpected tax outcomes in the future and be more compliant. Therefore, the government needs to help companies reduce compliance risks that cannot be controlled by companies but can be influenced by tax authorities.
A Joint Acceleration Estimation Method Based on a High-Order Disturbance Observer

Joint acceleration feedback is widely used in the design of controllers and observers since joint accelerations reflect the joint dynamics of robots, especially in physical human-robot interaction. However, joint acceleration acquisition is a technical difficulty for robots. The dynamics-based methods can achieve joint acceleration estimation using only a nominal model. Still, the performance of these methods is limited by the fast time-varying disturbances in the system. This letter proposes a joint acceleration estimation method based on a high-order disturbance observer. This method can observe and compensate for fast time-varying lumped disturbances in the observer while maintaining joint acceleration estimation performance at low frequencies. The finite-time stability of the proposed estimation method is proved using the Lyapunov theory. Simulations and experiments with a lower limb rehabilitation robot are implemented to verify the performance of the proposed method.