Miracle-dz/UniFAR-FTUs huggingface dataset:
A new method to measure the virial factors in the reverberation mapping of active galactic nuclei

Based on the gravitational redshift, one prediction of Einstein's general relativity theory, of broad optical emission lines in active galactic nuclei (AGNs), a new method is proposed to estimate the virial factors $f$ in measuring black hole masses $M_{\rm{RM}}$ by the reverberation mapping of AGNs. The factors $f$ can be measured on the basis of two physical quantities, i.e. the gravitational redshifts $z_{\rm{g}}$ and full widths at half maxima $v_{\rm{FWHM}}$ of broad lines. In the past it has been difficult to determine the factors $f$ for individual AGNs. We apply this new method to several reverberation mapped Seyfert 1 galaxies. There is a correlation between $f$ and broad-line region (BLR) radius $r_{\rm{BLR}}$, $f=5.4 r_{\rm{BLR}}^{0.3}$, for the gravitationally redshifted broad lines He II, He I, H$\beta$ and H$\alpha$ in narrow-line Seyfert 1 galaxy (NLS1) Mrk 110. This correlation results from the radiation pressure influence of the accretion disc on the BLR clouds. The radiation pressure influence seems to be more important than usually thought in AGNs. Mrk 110 has $f \approx$ 8--16, distinctly larger than the mean $\langle f\rangle \approx 1$, usually used to estimate $M_{\rm{RM}}$ in the case of $v_{\rm{FWHM}}$. NGC 4593 and NLS1 Mrk 486 has $f\approx 3$ and $f\approx 9$, respectively. Higher $f$ values of several tens are derived for three other NLS1s. There is a correlation between $f$ and accretion rate $\mathscr{\dot M}_{f=1}$, $f=6.8\mathscr{\dot M}^{0.4}_{f=1}$ for five objects, where $\mathscr{\dot M}_{f=1}=\dot M_{\bullet}/L_{\rm{Edd}}c^{-2}$ as $f=1$ is assumed to estimate $M_{\rm{RM}}$ used in the Eddington luminosity $L_{\rm{Edd}}$, $\dot M_{\bullet}$ is the mass accretion rate, and $c$ is the speed of light. These larger $f$ values will produce higher $M_{\rm{RM}}$ values and lower Eddington ratios.
DUST TRANSPORT IN PROTOSTELLAR DISKS THROUGH TURBULENCE AND SETTLING

We apply ionization balance and magnetohydrodynamical (MHD) calculations to investigate whether magnetic activity moderated by recombination on dust grains can account for the mass accretion rates and the mid-infrared spectra and variability of protostellar disks. The MHD calculations use the stratified shearing-box approach and include grain settling and the feedback from the changing dust abundance on the resistivity of the gas. The two-decade spread in accretion rates among solar-mass T Tauri stars is too large to result solely from variations in the grain size and stellar X-ray luminosity, but can plausibly be produced by varying these parameters together with the disk magnetic flux. The diverse shapes and strengths of the mid-infrared silicate bands can come from the coupling of grain settling to the distribution of the magnetorotational turbulence, through the following three effects. First, recombination on grains 1 μm or smaller yields a magnetically inactive dead zone extending more than two scale heights from the midplane, while turbulent motions in the magnetically active disk atmosphere overshoot the dead zone boundary by only about one scale height. Second, grains deep in the dead zone oscillate vertically in wave motions driven by the turbulent layer above, but on average settle at the rates found in laminar flow, so that the interior of the dead zone is a particle sink and the disk atmosphere will become dust-depleted unless resupplied from elsewhere. Third, with sufficient depletion, the dead zone is thinner and mixing dredges grains off the midplane. The last of these processes enables evolutionary signatures such as the degree of settling to sometimes decrease with age. The MHD results also show that the magnetic activity intermittently lifts clouds of small grains into the atmosphere. Consequently the photosphere height changes by up to one-third over timescales of a few orbits, while the extinction along lines of sight grazing the disk surface varies by factors of 2 over times down to a tenth of an orbit. We suggest that the changing shadows cast by the dust clouds on the outer disk are a cause of the daily to monthly mid-infrared variability found in many young stars.
Microscopic Evidence of Direct Coupling between Magnetic and Superconducting Order Parameters in BaFe2(As1-xPx)2

The coexistence of magnetism and superconductivity in the isovalent-P-substituted BaFe 2 (As 1- x P x ) 2 has been investigated microscopically by 31 P-NMR measurements. We found that superconducting (SC) transition occurs in a magnetic region with static ordered moments and that the moments are reduced below the SC transition temperature T c in the samples near the phase boundary of magnetism and superconductivity. Our results indicate that magnetism and superconductivity coexist spatially but compete with each other on the same Fermi surfaces. The coexistence state is qualitatively different from that observed in other unconventional superconductors and gives a strict constraint on the theoretical model for superconductivity in BaFe 2 (As 1- x P x ) 2 .
Painting galaxies into dark matter haloes using machine learning

We develop a machine learning (ML) framework to populate large dark matter-only simulations with baryonic galaxies. Our ML framework takes input halo properties including halo mass, environment, spin, and recent growth history, and outputs central galaxy and halo baryonic properties including stellar mass ($M_*$), star formation rate (SFR), metallicity ($Z$), neutral ($\rm HI$) and molecular ($\rm H_2$) hydrogen mass. We apply this to the MUFASA cosmological hydrodynamic simulation, and show that it recovers the mean trends of output quantities with halo mass highly accurately, including following the sharp drop in SFR and gas in quenched massive galaxies. However, the scatter around the mean relations is under-predicted. Examining galaxies individually, at $z=0$ the stellar mass and metallicity are accurately recovered ($\sigma\lesssim 0.2$~dex), but SFR and $\rm HI$ show larger scatter ($\sigma\gtrsim 0.3$~dex); these values improve somewhat at $z=1,2$. Remarkably, ML quantitatively recovers second parameter trends in galaxy properties, e.g. that galaxies with higher gas content and lower metallicity have higher SFR at a given $M_*$. Testing various ML algorithms, we find that none perform significantly better than the others, nor does ensembling improve performance, likely because none of the algorithms reproduce the large observed scatter around the mean properties. For the random forest algorithm, we find that halo mass and nearby ($\sim 200$~kpc) environment are the most important predictive variables followed by growth history, while halo spin and $\sim$Mpc scale environment are not important. Finally we study the impact of additionally inputting key baryonic properties $M_*$, SFR and $Z$, as would be available e.g. from an equilibrium model, and show that particularly providing the SFR enables $\rm HI$ to be recovered substantially more accurately.
Stability of toroidal magnetic fields in stellar interiors

We present 3D MHD simulations of purely toroidal and mixed poloidal-toroidal magnetic field configurations to study the behavior of the Tayler instability. For the first time the simultaneous action of rotation and magnetic diffusion are taken into account and the effects of a poloidal field on the dynamic evolution of unstable toroidal magnetic fields is included. In the absence of diffusion, fast rotation (rotation rate compared to Alfv\'en frequency) is able to suppress the instability when the rotation and magnetic axes are aligned and when the radial field strength gradient p 1.5, rapid rotation does not suppress the instability but instead introduces a damping factor to the growth rate in agreement with the analytic predictions. For the mixed poloidal-toroidal fields we find an unstable axisymmetric mode, not predicted analytically, right at the stability threshold for the non-axisymmetric modes; it has been argued that an axisymmetric mode is necessary for the closure of the Tayler-Spruit dynamo loop.
Kinetically determined shapes of grain boundaries in CVD graphene

Predicting the shape of grain boundaries is essential to control results of the growth of large graphene crystals. A global energy minimum search predicting the most stable final structure contradicts experimental observations. Here we present Monte Carlo simulation of kinetic formation of grain boundaries (GB) in graphene during collision of two growing graphene flakes. Analysis of the resulting GBs for the full range of misorientation angles $\alpha$ allowed us to identify a hidden (from post facto analysis such as microscopy) degree of freedom - the edge misorientation angle $\beta$. Edge misorientation characterizes initial structure rather than final structure and therefore provides more information about growth conditions. Use of $\beta$ enabled us to explain disagreements between the experimental observations and theoretical work. Finally, we report an analysis of an interesting special case of zero-tilt GBs for which structure is determined by two variables describing the relative shift of initial islands. We thereby present analysis of the full range of tilt GB ( $\beta\neq$ 0) and translational GB ( $\beta$ = 0). Based on our findings we propose strategies of controlling the GB morphology in experiments, which paves the way to a better control over graphene structure and properties for advanced applications.
Exact Foldy-Wouthuysen transformation for gravitational waves and magnetic field background

We consider an exact Foldy-Wouthuysen transformation for the Dirac spinor field on the combined background of a gravitational wave and constant uniform magnetic field. By taking the classical limit of the spinor field Hamiltonian, we arrive at the equations of motion for the nonrelativistic spinning particle. Two different kinds of gravitational fields are considered and in both cases the effect of the gravitational wave on the spinor field and on the corresponding spinning particle may be enforced by a sufficiently strong magnetic field. This result can be relevant for astrophysical applications and, in principle, useful for creating the gravitational wave detectors based on atomic physics and precise interferometry.
On the determination of the spin and disc truncation of accreting black holes using X-ray reflection

We discuss the application of simple relativistically-blurred X-ray reflection models to the determination of the spin and the inner radius of the disc in accreting black holes. Observationally, the nature of the corona is uncertain a priori, but a robust determination of the inner disk radius can be made when the disc emissivity index is tightly constrained. When the inner disc is well illuminated, the black hole spin can also be determined. Using reflection modelling derived from ray tracing, we show that robust determination of disc truncation requires that the location of the coronal source is quasi-static and at a height and radius less than the truncation radius of the disc. Robust spin measurements require that at least part of the corona lies less than about 10 gravitational radii above the black hole in order that the innermost regions, including the innermost stable circular orbit, are well illuminated. The width of the blurring kernel (e.g., the iron line) has a strong dependence on coronal height. These limitations may be particularly applicable at low Eddington fractions (e.g. the low/hard state, and low-luminosity AGN) where the height of the corona may be relatively large, or outflowing, and tied to jet production.
Inclusive Leadership in Relationship with Psychological Distress, Organizational Climate and Social Intelligence: A Theoretical Framework Study

The chain of global change phenomena occurring in life today has resulted in the urgent need to place world-class education as outlined in the Malaysia Blueprint 2013-2025. Hence, the Ministry of Education installed high-performing leaders in all schools by adopting the Transformative leadership style. The post-pandemic crisis is still haunting the lives of everyone, including teachers1 in schools. The urgency of change makes many teachers experience psychological distress. Therefore, the call to conduct research holistically in leadership, management, and resources to overcome the issue. Hence, this article describes a theoretical framework based on gaps and limitations in most past literature. The theoretical lens of social exchange theory contributes to the relationship between Inclusive Leadership, psychological stress, organizational climate and Social Intelligence. Eventually, the Inclusive Leadership style is not yet widely practiced in schools compared to the Transformational leadership style practiced since 2013. Based on literature reviews, this theoretical framework study uses to investigate Inclusive Leadership in curbing psychological distress among school teachers through organizational Climate and Social intelligence mediation. Therefore, the study of this theory aims to contribute to the field of Educational Leadership and Crisis management. And also beneficial not only to the Ministry of Education and to humankind.
Geometric Morphometric Wing Analysis of Avian Malaria Vector, Culiseta longiareolata, from Two Locations in Algeria

Simple Summary Culiseta longiareolata (Macquart 1838) is a cosmopolitan mosquito species and is considered to be an important vector in the transmission of avian malaria, tularemia, and arboviruses. The present study investigates the population structure of Cs. longiareolata from different bioclimatic and larval habitat types using a wing geometric morphometric approach. The main findings of our study showed that these environmental factors shape the population structure of Cs. longiareolata, most especially in male mosquitoes. This further deepens our understanding of how vector mosquitoes such as Cs. longiareolata adapt and thrive in different environmental conditions. Abstract The application of geometric morphometry on mosquito wings (Culicidae) is considered a powerful tool for evaluating correlations between the phenotype (e.g., shape) and environmental or genetic variables. However, this has not been used to study the wings of the avian malaria vector, Culiseta longiareolata. Therefore, the goal of this study is to investigate the intra-specific wing variations between male and female Cs. longiareolata populations in different types of larval habitats and climatic conditions in Algeria. A total of 256 Cs. longiareolata mosquito samples were collected from January 2020 to July 2021 in three cities (Annaba, El-Tarf, and Guelma) of northeastern Algeria that have two distinct climatic condition levels (sub-humid and sub-arid) and different types of larval habitats (artificial and natural). Nineteen (19) wing landmarks (LMs) were digitized and analyzed based on geometric morphometry. Our results revealed differences in the wing shape of female and male mosquito populations, indicating sexual dimorphism. Moreover, canonical variance analysis (CVA) showed that factors, such as climatic conditions and type of larval habitats, also affect the wing shape of female and male Cs. longiareolata mosquito populations. Furthermore, the wing shape of male populations was more distinct compared with female populations.
On the validation and use of high-fidelity numerical simulations for gust response analysis.

Specific gust response is considered as one of the most important loads encountered by an aircraft. The Certification Specification (CS) 25, defined by the European Aviation Safety Agency (EASA), and the Federal Aviation Regulations (FAR) 25, defined by the Federal Aviation Administration (FAA), describe the critical gusts that an aircraft must withstand. They must be analyzed for a large range of flight points (Altitude and Equivalent Air speed) and mass configurations. For some load cases, the standard tools could not be accurate enough to correctly predict the gust response and the use of high-fidelity computation could be required. Therefore, ONERA has implemented in its in-house Computational Fluid Dynamics (CFD) code elsA (ONERA-Airbus-Safran property) the capability to compute the high-fidelity aeroelastic gust response, directly in the time-domain, for different discrete gust shapes.This paper presents some recent work achieved at ONERA concerning high-fidelity simulations for gust response. First, a physical validation of the gust response simulation is performed by comparing the results to those obtained experimentally on a scaled model. Second, numerical comparisons are performed using various techniques, in order to model the gust. Finally, an application for generic regional aircraft is shown.
Tracking Cluster Debris (TraCD) – I. Dissolution of clusters and searching for the solar cradle

Having the ability of reconstructing dissolved stellar systems in dynamical and chemical space is a key factor to understand the evolution of the Milky Way. Here we focus on the dynamical aspect and given that most of the stars in the Milky Way have been born in stellar associations or clusters that have lived a few Myr up to several Gyr, we focus on the evolution of star clusters. We have carried out our simulations in two steps: 1) we have created a Galactic disc dynamically as close to observations as possible and 2) we have evolved three sets of stellar clusters with masses of 400, 1000 and 15000 M⊙ to dissolution. The birth location of these sets was 4, 6, 8 and 10 kpc for the 400 and 1000 M⊙ clusters and 4, 6, 8, 10 and 12 kpc for the 15000 M⊙. We have focussed our efforts on studying the state of these escapers after 4.5 Gyr of evolution in the Solar annulus, i.e. 7.5 6 Rgc 6 8.5 kpc. We found that the contribution of binary systems represents 30 per cent of the total number of system from these dissolved star clusters present in the Solar annulus. For single stars ending in the Solar annulus we have studied two distinct families: Solar twins and Solar siblings. The contribution of Solar twins from clusters born at 8 kpc is 17 per cent higher than for the clusters born at 6 kpc and 35 per cent higher than clusters at 10 kpc. We have also analysed the possibility of a given star escaping from our clusters with a mass close to the mass of the Sun to end in the Solar orbit. We found by using dynamical arguments that for our 400 M⊙ clusters there is a 49 per cent higher chance of the Sun being born from a cluster at 8 kpc than at 6 kpc while only a 38 per cent higher chance to come from a cluster born at 10 kpc. For our 1000 M⊙ clusters it becomes a 50 per cent higher chance of the Sun being born from a cluster at 8 kpc than at 6 kpc while only a 25 per cent higher chance to come from a cluster born at 10 kpc. Finally for our 15000 M⊙ clusters there is a 70 per cent higher chance of the Sun coming from a cluster born at 8 kpc than at either 6 or 10 kpc while this reduces to 59 per cent relative to clusters born at 12 kpc. We have concluded our analysis by calculating magnitudes and colours of our single stars in order to make predictions about the samples that the Gaia, Gaia-ESO and GALAH-AAO surveys will obtain. In terms of reconstructing dissolved star clusters we find that on short timescales we cannot rely on kinematic evolution alone and thus it will be necessary to extend our study to include information on chemical space.
Street-Level Workers and the Construction of Social Infrastructure in Suburban Neighbourhoods

The article examines the provision of social infrastructures in suburban neighbourhoods from the perspective of street-level workers. The concept of infrastructure is usually related to material and structural conditions but can equally apply to social infrastructures that are continuously constructed and maintained in social practices. These social infrastructures are embedded in structures and social arrangements and are related to past decisions. Our research focuses on the social infrastructures of two high-rise suburbs in Finland, built in the 1960s and 1970s. Since the 1990s, these neighbourhoods have experienced socioeconomic decline and transformation into a multicultural milieu. While suburbs have often been overlooked in urban politics and public discourses, a wide range of social infrastructures have also evolved in these districts and are continuously maintained. The main research data consists of interviews with street-level workers who participate in the production of such local social infrastructures. The article identifies and analyses the essential factors and preconditions as well as the challenges and contradictions of the provision of social infrastructure in these suburban contexts. This understanding is needed in order to foster an extensive social infrastructure and to deter counterforces from exacerbating socio-spatial inequalities and social polarisation in cities.
A diagrammatic calculation of the energy spectrum of quantum impurity in degenerate Bose–Einstein condensate

In this paper we consider a quantum particle moving through dilute Bose–Einstein condensate at zero temperature. In our formulation the impurity particle interacts with the gas of uncoupled Bogoliubov's excitations. The perturbation theory for the Green's function of the impurity particle with respect to the impurity–condensate interaction is constructed by employing the coherent-state path integral approach. The perturbative expansion for the Green's function is resumed into the expansion for its self-energy part with the help of the diagrammatic technique developed in this work. The dispersion relation for the impurity clothed by condensate excitations is obtained and effective mass is evaluated beyond the Golden rule approximation.
A Novel Analytical LRPSM for Solving Nonlinear Systems of FPDEs

This article employs the Laplace residual power series approach to study nonlinear systems of time-fractional partial differential equations with time-fractional Caputo derivative. The proposed technique is based on a new fractional expansion of the Maclurian series, which provides a rapid convergence series solution where the coefficients of the proposed fractional expansion are computed with the limit concept. The nonlinear systems studied in this work are the Broer-Kaup system, the Burgers’ system of two variables, and the Burgers’ system of three variables, which are used in modeling various nonlinear physical applications such as shock waves, processes of the wave, transportation of vorticity, dispersion in porous media, and hydrodynamic turbulence. The results obtained are reliable, efficient, and accurate with minimal computations. The proposed technique is analyzed by applying it to three attractive problems where the approximate analytical solutions are formulated in rapid convergent fractional Maclurian formulas. The results are studied numerically and graphically to show the performance and validity of the technique, as well as the fractional order impact on the behavior of the solutions. Moreover, numerical comparisons are made with other well-known methods, proving that the results obtained in the proposed technique are much better and the most accurate. Finally, the obtained outcomes and simulation data show that the present method provides a sound methodology and suitable tool for solving such nonlinear systems of time-fractional partial differential equations.