Miracle-dz/UniFAR-FTUs huggingface dataset:
Effect of Magnetic Braking on Circumstellar Disk Formation in a Strongly Magnetized Cloud

Using resistive magnetohydrodynamics simulation, we consider circumstellar disk formation in a strongly magnetized cloud. As the initial state, an isolated cloud core embedded in a low-density interstellar medium with a uniform magnetic field was adopted. The cloud evolution was calculated until almost all gas inside the initial cloud fell onto either the circumstellar disk or a protostar, and a part of the gas was ejected into the interstellar medium by the protostellar outflow driven by the circumstellar disk. In the early main accretion phase, the disk size is limited to � 10 AU because the angular momentum of the circumstellar disk is effectively transferred by both magnetic braking and the protostellar outflow. In the later main accretion phase, however, the circumstellar disk grows rapidly and exceeds & 100 AU by the end of the main accretion phase. This rapid growth of the circumstellar disk is caused by depletion of the infalling envelope, while magnetic braking is effective when the infalling envelope is more massive than the circumstellar disk. The infalling envelope cannot brake the circumstellar disk when the latter is more massive than the former. In addition, the protostellar outflow weakens and disappears in the later main accretion phase, because the outflow is powered by gas accretion onto the circumstellar disk. Although the circumstellar disk formed in a magnetized cloud is considerably smaller than that in an unmagnetized cloud, a circumstellar disk exceeding 100 AU can form even in a strongly magnetized cloud.
ARE THERE ECHOES FROM THE PRE-BIG-BANG UNIVERSE? A SEARCH FOR LOW-VARIANCE CIRCLES IN THE COSMIC MICROWAVE BACKGROUND SKY

In a recent analysis of Wilkinson Microwave Anisotropy Probe (WMAP) seven-year temperature maps, Gurzadyan and Penrose claim to find concentric circular patterns in the sky with anomalously low variances. These circles are presented as observational evidence for violent processes in a universe preceding our big bang as predicted by Penrose's Conformal Cyclic Cosmology. We reassess the statistical significance of the detection of the claimed concentric low-variance circles by comparing the WMAP data with Monte Carlo simulations of the cosmic microwave background (CMB) sky plus realistic modeling of WMAP's anisotropic noise. We find no anomaly in the variances compared with the ΛCDM cosmological model. The observed variances in the data are consistent with a Gaussian CMB sky as predicted by the inflationary cosmology model at better than 3σ.
Impact of Working Capital Management on Financial Performance of Quoted Consumer Goods Sector in Nigeria

This study examined the impact of working capital management on the financial performance of listed manufacturing firms in Nigeria. The population of this study consisted of all the quoted firms in the consumer goods sector in Nigeria, out of which nine (9) companies were selected based on data availability. For the 10 years spanning 2011-2020, data were gathered from the annual financial reports of the nine quoted companies in the consumer category. Descriptive statistics, correlation, and panel regression analysis methods were employed in data analysis. The outcome of the Hausman test revealed that the estimation of the random effect is the most efficient. The result revealed that inventory turnover had a positive insignificant effect on return on asset. Trade receivable collection period had negative insignificant effect on return on asset. Trade payable payment period had negative insignificant effect on return on asset. Cash conversion cycle had negative insignificant effect on return on asset. The study concluded that working capital management has no significant effect on financial performance of the selected firms over the period of the study. The study recommended that the whole system of the organization should pay more attention to working capital management.
Combination Strategy for the Geocentric Realization of Regional Epoch Reference Frames

For high‐resolution regional geodetic applications, the International Terrestrial Reference Frame (ITRF) is complemented by regional densifications. These are realized either as multi‐year solutions related to a tectonic plate (e.g., EUREF for Europe) or as epoch reference frames (ERFs) to capture nonlinear geophysical station motions caused by, for example, earthquakes or non‐tidal loading (e.g., SIRGAS for Latin America). These Global Navigation Satellite Systems (GNSS)‐only based regional reference frames have in common that their geodetic datum is aligned with the ITRF datum at a specific epoch. The consequence is that their origin represents the Earth's center of figure and does not coincide with the instantaneous center of mass. Here, we present studies on a direct geocentric realization of regional ERFs. We propose to realize the geodetic datum for each epoch by combining global GNSS, Satellite Laser Ranging, and Very Long Baseline Interferometry networks via measured local ties at co‐located sites. A uniformly distributed global GNSS network is used to realize the orientation via a no‐net‐rotation constraint with respect to the ITRF and is densified by the stations of the regional subnetwork. The developed combination and filtering strategy aims to guarantee a stable datum realization for each epoch‐wise solution. Validating our results against global reference frames and geophysical loading models relating to the Earth's centers of mass and figure, we show that the realized displacement time series are geocentric and reflect seasonal geophysical processes. As the approach does not need to rely on co‐location sites in the region of interest, it is conceptually transferable to other regions on the globe.
Variabiity of young stellar objects: Accretion, disks, outflows, and magnetic activity

Variability is a key characteristic of young stars. Two major origins may be distinguished: a scaled-up version of the magnetic activity seen on main-sequence stars and various processes related to circumstellar disks, accretion, and outflows. (© 2015 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
CHANDRA OBSERVATION OF A WEAK SHOCK IN THE GALAXY CLUSTER A2556

Based on a 21.5 ks Chandra observation of A2556, we identify an edge on the surface brightness profile at about 160 h−171 kpc northeast of the cluster center, and it corresponds to a shock front whose Mach number is calculated to be 1.25+0.02−0.03. No prominent substructure, such as sub-cluster, is found in either the optical or X-ray band that can be associated with the edge, suggesting that the conventional supersonic motion mechanism may not work in this case. As an alternative solution, we propose that the nonlinear steepening of an acoustic wave, which is induced by the turbulence of the intracluster medium at the core of the cluster, can be used to explain the origin of the shock front. Although nonlinear steepening weak shock is expected to occur frequently in clusters, why it is rarely observed still remains a question that requires further investigation, including both deeper X-ray observation and extensive theoretical studies.
REDD+: The Opportunity for Sustainable Management in Zagros Forests

ABSTRACT The Reducing Emissions from Deforestation and Degradation (REDD+) projects aim to prevent deforestation and greenhouse gas emissions as a policy to combat climate changes. This article evaluates changes to the Zagros’ Forest cover in 20 years and predicts the implications of implementing the REDD+ project in the next two decades. Using Landsat Forest cover maps and a logistic regression model the potential for forest cover transfer to non-forest regions was modeled to identify regions at risk of deforestation. A Markov chain was implemented to predict the changes. Receiver Operating Characteristics (ROC) was employed for validation, and the Voluntary Carbon Standard (VCS) was utilized to model the REDD+ project baseline to predict the forest cover changes. The findings indicate, 37,809 hectares of forest cover were lost in the past 20 years and with this trend, the amount of greenhouse gas emissions will increase. However, implementing the REDD+ project can prevent the release of 1,714,534.13 tCO2e. Therefore, this deteriorating forest possesses the potential to reduce CO2 emissions by preventing deforestation, identifying deforestation-prone areas and implementing the REDD+ project utilizing the methodology presented. Climate change mitigation, carbon sequestration, and biodiversity protection are just a few of the benefits of REDD+ projects that can aid sustainable forest management
MAGNETIZED GAS IN THE SMITH HIGH VELOCITY CLOUD

We report the first detection of magnetic fields associated with the Smith High Velocity Cloud. We use a catalog of Faraday rotation measures toward extragalactic radio sources behind the Smith Cloud, new H i observations from the Robert C. Byrd Green Bank Telescope, and a spectroscopic map of Hα from the Wisconsin H-Alpha Mapper Northern Sky Survey. There are enhancements in rotation measure (RM) of ≈100 rad m−2 which are generally well correlated with decelerated Hα emission. We estimate a lower limit on the line-of-sight component of the field of ≈8 μG along a decelerated filament; this is a lower limit due to our assumptions about the geometry. No RM excess is evident in sightlines dominated by H i or Hα at the velocity of the Smith Cloud. The smooth Hα morphology of the emission at the Smith Cloud velocity suggests photoionization by the Galactic ionizing radiation field as the dominant ionization mechanism, while the filamentary morphology and high (≈1 Rayleigh) Hα intensity of the lower-velocity magnetized ionized gas suggests an ionization process associated with shocks due to interaction with the Galactic interstellar medium. The presence of the magnetic field may contribute to the survival of high velocity clouds like the Smith Cloud as they move from the Galactic halo to the disk. We expect these data to provide a test for magnetohydrodynamic simulations of infalling gas.
THE EFFECT OF ENVIRONMENT ON SHEAR IN STRONG GRAVITATIONAL LENSES

Using new photometric and spectroscopic data in the fields of nine strong gravitational lenses that lie in galaxy groups, we analyze the effects of both the local group environment and line-of-sight (LOS) galaxies on the lens potential. We use Monte Carlo simulations to derive the shear directly from measurements of the complex lens environment, providing the first detailed independent check of the shear obtained from lens modeling. We account for possible tidal stripping of the group galaxies by varying the fraction of total mass apportioned between the group dark matter halo and individual group galaxies. The environment produces an average shear of γ = 0.08 (ranging from 0.02 to 0.17), significant enough to affect quantities derived from lens observables. However, the direction and magnitude of the shears do not match those obtained from lens modeling in three of the six four-image systems in our sample (B1422, RXJ1131, and WFI2033). The source of this disagreement is not clear, implying that the assumptions inherent in both the environment and lens model approaches must be reconsidered. If only the local group environment of the lens is included, the average shear is γ = 0.05 (ranging from 0.01 to 0.14), indicating that LOS contributions to the lens potential are not negligible. We isolate the effects of various theoretical and observational uncertainties on our results. Of those uncertainties, the scatter in the Faber–Jackson relation and error in the group centroid position dominate. Future surveys of lens environments should prioritize spectroscopic sampling of both the local lens environment and objects along the LOS, particularly those bright (I< 21.5) galaxies projected within 5′ of the lens.
A look into the inside of haloes: a characterization of the halo shape as a function of overdensity in the Planck cosmology

In this paper we study the triaxial properties of dark matter haloes of a wide range of masses extracted from a set of cosmological N-body simulations. We measure the shape at different distances from the halo centre (characterised by different overdensity thresholds), both in three and in two dimensions. We discuss how halo triaxiality increases with mass, redshift and distance from the halo centre. We also examine how the orientation of the different ellipsoids are aligned with each other and what is the gradient in internal shapes for halos with different virial configurations. Our findings highlight that the internal part of the halo retains memory of the violent formation process keeping the major axis oriented toward the preferential direction of the in-falling material while the outer part becomes rounder due to continuous isotropic merging events. This effect is clearly evident in high mass haloes - which formed more recently - while it is more blurred in low mass haloes. We present simple distributions that may be used as priors for various mass reconstruction algorithms, operating in different wavelengths, in order to recover a more complex and realistic dark matter distribution of isolated and relaxed systems.
Nonlinearity-mediated soliton ejection from trapping potentials in nonlocal media

We address the properties of optical solitons in thermal nonlinear media with a local refractive index defect that is capable of trapping solitons launched close to the sample boundary despite the boundary-mediated forces that tend to deflect all beams toward the center of the sample. We show that while such forces become more pronounced with an increasing of the input beam power the defect can trap only light below a critical power above which solitons are ejected. The dynamics of soliton ejection and the subsequent propagation may be controlled.
The shape of emergent quantum geometry from an N=4 SYM minisuperspace approximation

We study numerically various wave functions in a gauged matrix quantum mechanics of six commuting hermitian $N\times N$ matrices. Our simulations span ranges of $N$ up to 10000. This system is a truncated and quenched version of N=4 SYM that serves as a minisuperspace approximation to the full ${\cal N}=4$ SYM system. This setup encodes aspects of the geometry of the AdS dual in terms of joint eigenvalue distributions for the matrices in the large $N$ limit. We analyze the problem of determining geometric measurements from these fluctuating distributions at finite $N$ and how fast they approach to the large N limit. We treat this eigenvalue geometry information as a proxy for geometric calculations in quantum gravity in a description where gravity is an emergent phenomenon. Our results show that care is needed in choosing the observables that measure the geometry: different choices of observables give different answers, have different size fluctuations at finite $N$ and they converge at different rates to the large $N$ limit. We find that some natural choices of observables are pathological at finite $N$ for $N$ sufficiently small. Finally, we note that the approach to the large $N$ limit does not seem to follow the expected convergence in powers of $1/N^2$ from planar diagram arguments. Our evidence suggests that different powers of $N$ appear, but convergence to large $N$ is rather slow so the values of $N$ we have explored might be too small to conclude this unambiguously.
The Effect of Child Spacing on Mothers’ Labor Force Participation in Urban Households of Iran

Background: Short and long birth spacings have negative effects on the health of mothers and children and consequently on the level of mothers’ employment. Objectives: This study aimed to investigate the effect of first and second children spacing on mothers’ labor force participation in Iranian urban households. Methods: This descriptive-analytical cross-sectional study was performed using econometric methods as a probit and probit model with an instrumental variable in Stata version 16 in 2021. The sample size included 8920 urban households in all provinces of Iran, and the data were extracted from the cost and income questionnaire of urban households. Results: The birth spacing of the first and second child had a positive effect equal to 0.16 on the probability of employment of mothers in households with 2 children, which was equal to 0.22 for households with 2 or more children. The coefficients of maternal age, having a private home, father’s education, and father’s age on mothers’ employment were -0.02, -0.09, -0.06, and 0.02 in households with 2 children, respectively. Conclusions: Increasing the birth spacing, especially for the first and second child, led to an increase in the probability of the mother’s employment in the labor market. Therefore, optimal birth spacing is recommended, which improves both the health of the mother and the child and does not reduce job opportunities. In this regard, policies to promote optimal birth spacing through raising awareness, the use of contraceptive methods, and the importance of breastfeeding are also proposed.
Mass-radius relation for neutron stars in f(R) gravity

We discuss the Mass -Radius diagram for static neutron star models obtained by the numerical solution of modified Tolman-Oppenheimer-Volkoff equations in $f(R)$ gravity where the Lagrangians $f(R)=R+\alpha R^2 (1+\gamma R)$ and $f(R)=R^{1+\epsilon }$ are adopted. Unlike the case of the perturbative approach previously reported, the solutions are constrained by the presence of an extra degree of freedom, coming from the trace of the field equations. In particular, the stiffness of the equation of state determines an upper limit on the central density $\rho_c$ above which the the positivity condition of energy-matter tensor trace $T^{\rm m}=\rho - 3 p$ holds. In the case of quadratic f(R)-gravity, we find higher masses and radii at lower central densities with an inversion of the behavior around a pivoting $\rho_c$ which depends on the choice of the equation of state. When considering the cubic corrections, we find solutions converging to the required asymptotic behavior of flat metric only for $\gamma < 0$. A similar analysis is performed for $f(R)=R^{1+\epsilon }$ considering $\epsilon$ as the leading parameter. We work strictly in the Jordan frame in order to consider matter minimally coupled with respect to geometry. This fact allows us to avoid ambiguities that could emerge in adopting the Einstein frame.
Strong electron-phonon coupling in the intermetallic superconductor Mo8Ga41

Crystals of superconducting Mo$_{8}$Ga$_{41}$ ($T_{\text{c}}=9.8$ K) and Mo$_{\text{8-x}}$V$_{\text{x}}$Ga$_{41}$ limited solid solution $(x_{\text{max}}=1.9(2))$ have been grown from the high-temperature Ga flux and confirmed to have the V$_{8}$Ga$_{41}$ type of crystal structure at room temperature. Thermodynamic and transport measurements as well as electronic structure calculations were performed to investigate both normal- and superconducting-state properties of Mo$_{8}$Ga$_{41}$. The discontinuity in the heat capacity at $T_{\text{c}}$, $\Delta{}c_{\text{p}}/\gamma_{\text{N}}T_{\text{c}}=2.83$ in zero magnetic field, indicates a much stronger electron-phonon coupling than in the standard BCS limit. From the heat capacity data, we estimated the electron-phonon coupling constant $\lambda_{\text{ep}}=0.9$. The upper critical field is $\mu_{0}H_{\text{c2}}(0)=8.3$ T, while the lower one is only $\mu_{0}H_{\text{c1}}(0)=131$ Oe. The upper critical field of Mo$_{8}$Ga$_{41}$ exhibits a clear enhancement with respect to the Werthamer-Helfand-Honenberg prediction, consistent with the strong electron-phonon coupling. The Mo$_{\text{8-x}}$V$_{\text{x}}$Ga$_{41}$ limited solid solution also exhibits superconducting properties, and the critical temperature $T_{\text{c}}$ is reduced only slightly with increasing $x$.
Multicenter Italian Study on “In Vitro Activities” of Isavuconazole, Voriconazole, Amphotericin B, and Caspofungin for Aspergillus Species: Comparison between SensititreTM YeastOneTM and MIC Test Strip

Abstract In this study the activity of Isavuconazole, Voriconazole, Amphotericin B, and Caspofungin against 224 clinical isolates of Aspergillus spp. originating from seven Italian hospitals, was comparatively evaluated with two commercial antifungal susceptibility tests (AST): SensititreTM YeastOneTM (SYO) and MIC Test Strip. More attention was focused on Isavuconazole activity, given the new introduction of the drug in widely distributed antifungal susceptibilities methods in the clinical microbiology lab. The minimum inhibitory concentrations of antifungal drug that can inhibit the growth of pathogen by 90% (MIC90) for Isavuconazole detected by SYO were 0.5, 1, 0.25, and 2 µg/mL for Aspergillus fumigatus, Aspergillus flavus, Aspergillus terreus, and Aspergillus niger, respectively, whilst they were 0.25, 0.25, 0.5, and 0.75 µg/mL by MIC Test Strip. Essential agreement between the two tested methods for Isavuconazole is 70% for all the species tested, 75.7% for A. fumigatus, 45.2% for A. flavus, 90.6% for A. terreus, and 40% for A. niger. Although the tested strains do not express any phenotypic resistance, MIC results were quite different if tested with microdilution broth or gradient agar method. This is the first Italian multicenter report on Isavuconazole MIC obtained employing the widely used SensititreTM Yeast OneTM (SYO) and MIC Test Strip on clinical isolates of Aspergillus.
Pairing in neutron matter: New uncertainty estimates and three-body forces

We present solutions of the BCS gap equation in the channels ${}^1S_0$ and ${}^3P_2-{}^3F_2$ in neutron matter based on nuclear interactions derived within chiral effective field theory (EFT). Our studies are based on a representative set of nonlocal nucleon-nucleon (NN) plus three-nucleon (3N) interactions up to next-to-next-to-next-to-leading order (N$^3$LO) as well as local and semilocal chiral NN interactions up to N$^2$LO and N$^4$LO, respectively. In particular, we investigate for the first time the impact of subleading 3N forces at N$^3$LO on pairing gaps and also derive uncertainty estimates by taking into account results for pairing gaps at different orders in the chiral expansion. Finally, we discuss different methods for obtaining self-consistent solutions of the gap equation. Besides the widely-used quasi-linear method by Khodel et al. we demonstrate that the modified Broyden method is well applicable and exhibits a robust convergence behavior. In contrast to Khodel's method it is based on a direct iteration of the gap equation without imposing an auxiliary potential and is straightforward to implement.