Miracle-dz/UniFAR-FTUs huggingface dataset:
Observations of Extreme ICME Ram Pressure Compressing Mercury’s Dayside Magnetosphere to the Surface

Mercury’s magnetosphere is known to be affected by the enhanced ram pressure and magnetic fields inside interplanetary coronal mass ejections (ICMEs). Here we report detailed observations of an ICME compressing Mercury’s dayside magnetosphere to the surface. A fast CME launched from the Sun on 2013 November 29 impacted first the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) spacecraft, which was orbiting Mercury, on November 30 and later STEREO-A near 1 au on December 1. Following the ICME impact, MESSENGER remained in the solar wind as the spacecraft traveled inwards and northwards toward Mercury’s surface until it reached and passed its closest approach to the planet (at 371 km altitude) without crossing into the magnetosphere. The magnetospheric crossing finally occurred 1 minute before reaching the planet’s nightside at 400 km altitude and 84°N latitude, indicating the lack of dayside magnetosphere on this orbit. In addition, the peak magnetic field measured by MESSENGER at this time was 40% above the values measured in the orbits just prior to and after the ICME, a consequence of the magnetospheric compression. Using both a proxy method at Mercury and measurements at STEREO-A, we show that the extremely high ram pressure associated with this ICME was more than high enough to collapse Mercury’s weak magnetosphere. As a consequence, the ICME plasma likely interacted with Mercury’s surface, evidenced by enhanced sodium ions in the exosphere. The collapse of Mercury’s dayside magnetosphere has important implications for the habitability of close-in exoplanets around M dwarf stars, as such events may significantly contribute to planetary atmospheric loss in these systems.
Positive helicity Einstein-Yang-Mills amplitudes from the double copy method

All positive helicity four-point gluon-graviton amplitudes in Einstein-Yang-Mills theory coupled to a dilaton and axion field are computed at the leading one-loop order using colour-kinematics duality. In particular, all relevant contributions in the gravitational and gauge coupling are established. This extends a previous generalized unitarity based computation beyond the leading terms in the gravitational coupling $\kappa$. The resulting purely rational expressions take very compact forms. The previously seen vanishing of the single-graviton-three-gluon amplitude at leading order in $\kappa$ is seen to be lifted at order $\kappa^{3}$.
Inferring physical parameters in solar prominence threads

Context. High resolution observations have permitted the resolution of solar prominences/filaments into sets of threads/fibrils. However, the values of the physical parameters of these threads and their structuring remain poorly constrained. Aims. We use prominence seismology techniques to analyse transverse oscillations in threads by comparing magnetohydrodynamic (MHD) models and observations. Methods. We applied Bayesian methods to obtain two different types of information. We first inferred the marginal posterior distribution of physical parameters such as the magnetic field strength or length of the thread, when a totally filled tube, partially filled tube, and three damping models are considered as certain; the three damping models are resonant absorption in the Alfvén continuum, resonant absorption in the slow continuum, and Cowling’s diffusion. Then, we compared the relative plausibility between alternative MHD models by computing the Bayes factors. Results. Well-constrained probability density distributions can be obtained for the magnetic field strength, length of the thread, density contrast, and parameters associated with the damping models. In a comparison of the damping models of resonant absorption in the Alfvén continuum, resonant absorption in the slow continuum, and Cowling’s diffusion due to partial ionisation of prominence plasma, the resonant absorption in the Alfvén continuum is the most plausible mechanism to explain the existing observations. Relations between periods of fundamental and first overtone kink modes with values around 1 are better explained by expressions of the period ratio in the long thread approximation, while the rest of the values are more probable in the short thread limit for the period ratio. Conclusions. Our results show that Bayesian analysis offers valuable methods to perform parameter inference and a model comparison in the context of prominence seismology.
Hall Effect in the Abrikosov Lattice of Type-II Superconductors

We study vortex charging caused by the Lorentz force on supercurrent based on the augmented quasiclassical equations of superconductivity. Our numerical study on an s-wave vortex lattice in the range Hc1 < H < Hc2 reveals that each vortex core with a single flux quantum also accumulates charge due to the circulating supercurrent and has a Hall voltage across the core. The field dependence of the charge density at the core center is well described by ρ(0) ∝ H(Hc2 − H) with a peak near Hc2/2 originating from competition between the increasing magnetic field and the decreasing pair potential. The peak value of the accumulated charge in a core region of radius 0. 5ξ0 is estimated to be about ηΔ0/(kFξ0) × |e| C per Δz = 10 A along the flux line at low temperatures, where η ≡ πϵ0Δz/|e|2 = 1.09 × 1018 J−1 with e < 0 the charge of an electron, Δ0 the energy gap at T = 0, kF the Fermi wave number, and ξ0 the coherence length at T = 0.
Competition, Firm Size and Returns to Skills: Evidence from Currency Shocks and Market Liberalisations

The authors investigate the impact of exogenous product market competition shocks on returns to skills in Italy using a new longitudinal dataset on individual working histories. This impact is identified using three exogenous shocks affecting competition: the unforeseen devaluation of the Lira in 1992, its return to a fixed exchange regime in 1996 and the market liberalisation in the utility and transport sectors in the late 1990s‐early 2000s. This paper extends the analysis of Guadalupe (2007) by investigating how firm heterogeneity and shocks of different types and signs affect the impact of competition on skill premia. The authors find that opposite shocks have opposite effects: an increase (resp. decrease) in international competition increases (resp. decreases) returns to skills. Moreover, international shocks have greater effects on medium‐sized firms, while domestic liberalisation shocks have greater effects on large incumbents previously sheltered from any entry threat.
Direct numerical simulation of particle dispersion in a spatially developing turbulent boundary layer

We have performed direct numerical simulation (DNS) of a particle-laden spatially developing, zero-pressure-gradient turbulent boundary layer at Reθ = 1000− 2750. We computed the Lagrangian trajectories of uid points and solid particles of three di erent Stokes numbers (St = 0.1, 1, and 5). The particles were released in the computational domain from a line source at three di erent distances from the wall, in the viscous sublayer, the bu er layer, and the loglayer (z inj = 2, 10, and 100). The uid points mean-displacement obtained from the DNS is analyzed and compared to the theory of Batchelor (1964). Also, the time development of uid point and solid particle mean-square displacement (or dispersion) and turbulent di usivity are analyzed. Dispersion statistics are generally found to be strongly in uenced by particle inertia. Such dependence is mostly caused by the particles tendency to preferentially concentrate in the viscous sublayer. Furthermore, for very long times (several integral timescales), the DNS results show that the streamwise dispersion of uid points and particles with St= 0.1 is nearly ∝ t, while that of particles with St= 1 and 5 is nearly ∝ t. For all cases studied, the long-time wall-normal dispersion is nearly ∝ t.
3He in Planetary Nebulae: A Challenge to Stellar Evolution Models

The discrepancy between the observed abundances of 3He in the interstellar medium and those predicted by stellar and Galactic chemical evolution remains largely unexplained. In this paper, we attempt to shed some light on this unsolved problem by presenting a quantitative comparison of the 3He abundances recently measured in six planetary nebulae (IC 289, NGC 3242, NGC 6543, NGC 6720, NGC 7009, NGC 7662) with the corresponding predictions of stellar evolution theory. The determination of the mass of the planetary nebulae progenitors allows us to dismiss, with a good degree of confidence, the hypothesis that the abundance of 3He in the envelopes of all low-mass stars (M ≲ 2.5 M☉) is strongly reduced with respect to the standard theoretical values by some mixing mechanism acting in the latest phases of stellar evolution. The abundance versus mass correlation, with allowance made for the limitation of the sample, is in fact found to be fully consistent with the classical prediction of stellar evolution. We examine the implications of this result on the Galactic evolution of 3He with the help of a series of models with standard and nonstandard (i.e.,3He-depleted) nucleosynthesis prescriptions in varying percentages of low-mass stars. The results are found to be consistent with the abundances determined in the presolar material and in the local interstellar medium only if the vast majority of low-mass stars (more than 70%-80%) follow nonstandard prescriptions. This implies that either the sample of planetary nebulae under examination is highly biased and therefore not representative of the whole population of low-mass stars, or the solution to the 3He problem lies elsewhere.
A Comparison of Absorption- and Emission-Line Abundances in the Nearby Damped Lyα Galaxy SBS 1543+593

We have used STIS aboard HST to measure a sulfur abundance of [S/H] = -0.41 ± 0.06 in the ISM of the nearby DLA galaxy SBS 1543+593. A direct comparison between this QSO absorption line abundance and abundances measured from H II region emission line diagnostics yields the same result: the abundance of sulfur in the neutral ISM is in good agreement with that of oxygen measured in an H II region 3 kpc away. Our result contrasts with those of other recent studies that have claimed order-of-magnitude differences between H I (absorption) and H II (emission) region abundances. We also derive a nickel abundance of [Ni/H] < -0.81, some 3 times less than that of sulfur, and suggest that the depletion is due to dust, although we cannot rule out an overabundance of α-elements as the cause of the lower metallicity. It is possible that our measure of [S/H] is overestimated if some S II arises in ionized gas; adopting a plausible star formation rate for the galaxy along the line of sight and a measurement of the C II* λ1335. 7 absorption line detected from SBS 1543+593, we determine that the metallicity is unlikely to be smaller than we derive by more than 0.25 dex. We estimate that the cooling rate of the cool neutral medium is log[lc(ergs s-1 H atom-1)] ≈ -27.0, the same value as that seen in the high-redshift DLA population.
Collective Properties of Quasar Narrow Associated Absorption Lines

This paper statistically investigates the properties of C iv and Mg ii narrow absorption lines (NALs) to look for velocity cuts that can constrain quasar-associated NALs. The coverage fraction (fc) is defined as the ratio between the number of quasars exhibiting at least one detected absorber and the total number of quasars that can be used to detect absorptions with given criteria. We find that, for both C iv and Mg ii absorbers, both the number density of absorbers in given velocity intervals ( ) and the fc show very significant excess at the low-velocity offset from the quasars, relative to the random occurrence that is expected for cosmologically intervening absorbers. These relative excess extensions for Mg ii absorptions are not only evidently related to absorption strength but also to quasar luminosity, while they are mainly constrained within 2000 no matter what quasar luminosity and absorption strength are. In addition, we find that the redshift number density (dn/dz) evolution of Mg ii absorbers with vabs < 2000 evidently differs from that with vabs > 2000 . Turning to C iv absorptions, the relative excess extensions of both and fc are mainly limited within vabs < 4000 , and depend neither on absorption strength nor on quasar luminosity. And also, the absorbers with vabs < 4000 show obviously different redshift number density evolution from those with vabs > 4000 . We suggest velocity cuts of 4000 and 2000 to define quasar C iv and Mg ii associated NALs, respectively.
Classification of topological insulators and superconductors in three spatial dimensions

We systematically study topological phases of insulators and superconductors (or superfluids) in three spatial dimensions. We find that there exist three-dimensional (3D) topologically nontrivial insulators or superconductors in five out of ten symmetry classes introduced in seminal work by Altland and Zirnbauer within the context of random matrix theory, more than a decade ago. One of these is the recently introduced ${\mathbb{Z}}_{2}$ topological insulator in the symplectic (or spin-orbit) symmetry class. We show that there exist precisely four more topological insulators. For these systems, all of which are time-reversal invariant in three dimensions, the space of insulating ground states satisfying certain discrete symmetry properties is partitioned into topological sectors that are separated by quantum phase transitions. Three of the above five topologically nontrivial phases can be realized as time-reversal invariant superconductors. In these the different topological sectors are characterized by an integer winding number defined in momentum space. When such 3D topological insulators are terminated by a two-dimensional surface, they support a number (which may be an arbitrary nonvanishing even number for singlet pairing) of Dirac fermion (Majorana fermion when spin-rotation symmetry is completely broken) surface modes which remain gapless under arbitrary perturbations of the Hamiltonian that preserve the characteristic discrete symmetries, including disorder. In particular, these surface modes completely evade Anderson localization from random impurities. These topological phases can be thought of as three-dimensional analogs of well-known paired topological phases in two spatial dimensions such as the spinless chiral $({p}_{x}\ifmmode\pm\else\textpm\fi{}i{p}_{y})$-wave superconductor (or Moore-Read Pfaffian state). In the corresponding topologically nontrivial (analogous to ``weak pairing'') and topologically trivial (analogous to ``strong pairing'') 3D phases, the wave functions exhibit markedly distinct behavior. When an electromagnetic U(1) gauge field and fluctuations of the gap functions are included in the dynamics, the superconducting phases with nonvanishing winding number possess nontrivial topological ground-state degeneracies.
Values Education or Religious Education? An Alternative View of Religious Education in the Secular Age, the Case of Turkey

Debates about the teaching of religion date back to the formation of the modern education system, when religion was first compartmentalized as a distinct subject within a broader curriculum. In many places, they continue to rage today. In Turkey, they are inextricably tied to the creation of the country’s system of secular public instruction in the 1920s and the transition to multi-party government in the 1940s. On 30 March 2012, Turkey passed a new law that revamped the country’s public educational system, mandating twelve years of instruction divided into three four-year periods (roughly corresponding to elementary, middle, and high school). This law led to the opening of many new religious schools—known as Imam-Hatip schools (i.e., schools for the training of imams and hatips, or preachers)—across the country, especially at the middle-school level. The number of students studying in these schools rose from 70,000 in 2002 to 1,300,000 after the new law. New elective courses on religion were also added to the curriculum, and curricular and extra-curricular religious-education activities offered by government-sponsored Islamic civil society organizations became more prevalent. All of this has reignited old debates about religious instruction in the country. This article begins with an overview of the history of secularism in Turkey. It then focuses on the history of religious education and the model of religious education in Turkey. It concludes with a discussion of how religious education centering on values education operates within the secular framework of public education in confessional and non-confessional formats.
Chaotic cold accretion on to black holes in rotating atmospheres

Chaotic cold accretion (CCA) profoundly differs from classic black hole accretion models. Using 3D high-resolution simulations, we probe the impact of rotation on the hot and cold accretion flow in a typical massive galaxy. In the hot mode, with or without turbulence, the pressure-dominated flow forms a geometrically thick rotational barrier, suppressing the accretion rate to ~1/3 of the Bondi rate. When radiative cooling is dominant, the gas loses pressure support and quickly circularizes in a cold thin disk. In the more common state of a turbulent and heated atmosphere, CCA drives the dynamics if the gas velocity dispersion exceeds the rotational velocity, i.e., turbulent Taylor number < 1. Extended multiphase filaments condense out of the hot phase via thermal instability and rain toward the black hole, boosting the accretion rate up to 100 times the Bondi rate. Initially, turbulence broadens the angular momentum distribution of the hot gas, allowing the cold phase to condense with prograde or retrograde motion. Subsequent chaotic collisions between the cold filaments, clouds, and a clumpy variable torus promote the cancellation of angular momentum, leading to high accretion rates. The simulated sub-Eddington accretion rates cover the range inferred from AGN cavity observations. CCA predicts inner flat X-ray temperature and $r^{-1}$ density profiles, as recently discovered in M 87 and NGC 3115. The synthetic H{\alpha} images reproduce the main features of cold gas observations in massive ellipticals, as the line fluxes and the filaments versus disk morphology. Such dichotomy is key for the long-term AGN feedback cycle. As gas cools, filamentary CCA develops and boosts AGN heating; the cold mode is thus reduced and the rotating disk remains the sole cold structure. Its consumption leaves the atmosphere in hot mode with suppressed accretion and feedback, reloading the cycle.
Axisymmetric Dynamical Models of the Central Regions of Galaxies

We present axisymmetric, orbit superposition models for 12 galaxies using data taken with the Hubble Space Telescope (HST) and ground-based observatories. In each galaxy, we detect a central black hole (BH) and measure its mass to accuracies ranging from 10% to 70%. We demonstrate that in most cases the BH detection requires both the HST and ground-based data. Using the ground-based data alone does provide an unbiased measure of the BH mass (provided that they are fitted with fully general models), but at a greatly reduced significance. The most significant correlation with host galaxy properties is the relation between the BH mass and the velocity dispersion of the host galaxy; we find no other equally strong correlation and no second parameter that improves the quality of the mass-dispersion relation. We are also able to measure the stellar orbital properties from these general models. The most massive galaxies are strongly biased to tangential orbits near the BH, consistent with binary BH models, while lower mass galaxies have a range of anisotropies, consistent with an adiabatic growth of the BH.
Stokes IQUV mapping of $α^2$ CVn & other Ap stars using ESPaDOnS and NARVAL

New spectral line polarisation observations of 7 bright Ap stars have been obtained with the ESPaDOnS and Narval high resolution spectropolarimeters (Silvester et al. 2012). The aim of this data set is produce a series of surface magnetic field and surface chemistry maps for these Ap stars. We present new magnetic maps for the Ap star α2 CVn using these new data and the MDI inversion code INVERS10. α2 CVn is the first Ap star to be observed during two separate epochs using high resolution phase resolved spectropolarimetric IQUV observations and as such allows us an insight into how stable the surface magnetic structure is over a decade timescale. We show that the new maps give a magnetic field structure consistent with the previous maps obtained by Kochukhov and Wade (2010) from lower quality MuSiCoS spectra taken a decade ago and that the field topology cannot be described by a dipolar or quadrupolar field.
Human Nutrition and Metabolism Supplementation with Aromatic Amino Acids Improves Leucine Kinetics but Not Aromatic Amino Acid Kinetics in Infants with Infection , Severe Malnutrition , and Edema 1 , 2

We investigated whether supplementation with an aromatic amino acid (AAA) cocktail consisting of 0.5 mmol each of phenylalanine, tryptophan, and tyrosine compared with isonitrogenous amounts of alanine (Ala) would improve measures of protein kinetics in 14 (8 with AAA, 6 Ala) children with edematous malnutrition (aged 6–24 mo) during the infected acute malnourished state. Supplementation started immediately after the baseline experiment, 2 d postadmission and continued to the end of the acute phase of treatment. The second (postsupplementation) experiment was done 12 d postadmission. We measured leucine kinetics, phenylalanine and tyrosine fluxes, using an i.g. 8-h prime continuous infusion of H3-leucine, and an i.v. 6-h prime continuous infusion of C-leucine, H2-tyrosine, and H5-phenylalanine in the fed state. Leucine flux tended to be faster (P 0.06) in the AAA group compared with Ala group after supplementation (mean difference SEM): 22.6 10.9 mol/ (kg h). The rate of leucine appearance from protein breakdown [28.1 9.4 mol/(kg h)] and the nonoxidative disposal of leucine [i.e., leucine to protein synthesis; 35.4 12.9 mol/(kg h)] were faster (P 0.02) in the AAA group than in the Ala group. There was no significant effect of supplementation on leucine splanchnic metabolism, phenylalanine, and tyrosine fluxes. These findings are consistent with the hypothesis that the blunting of the protein catabolic response to infection in children with edematous malnutrition syndrome is due to limited availability of aromatic amino acids. J. Nutr. 134: 3004–3010, 2004.
The Fisheries Biology of the Big-Eye Scad, Selar crumenophthalmus (Bloch) in the Philippines

Age and growth of Selar crumenophthalmus (Pisces, Carangidae) from the Philippines were determined through the use of otolith daily growth increments and fish length-frequency data. The methods showed good agreement for computed growth parameters. Ages estimated from otoliths agreed well with those of the same species from the Mariana Islands, also determined by otolith microstructure. Apparent mortality rates, lengths at first capture and recruitment patterns were established from length-frequency data. Mortality rates and exploitation rates were high; sources of bias are discussed. Recruitment appears to occur in two pulses during the year, between four and five months apart. Catch rates of S. crumenophthalmus are highly seasonal, reflecting not only changes in biomass but also certain behavior associated with life-history stages.