Miracle-dz/UniFAR-FTUs huggingface dataset:
Synchronous Computer-mediated Corrective Feedback and EFL Learners’ Grammatical Knowledge Development: A Sociocultural Perspective

Recent discussions in language communication indicate the effectiveness of technology and computer-mediated communication. Research also highlights the central role of synchronous and asynchronous modes of interaction in second and foreign language development. Gaining insights from Vygotskyan sociocultural theory of mind, the present study employed a mixed methods approach to explore the effect of synchronous computer-mediated corrective feedback on EFL learners’ grammatical knowledge development. The participants were 40 Iranian EFL learners selected through a grammar-based pretest. Employing Skype software, the experimental group (N = 20) was exposed to online text-based chatting. The purpose was to provide the participants with online technology-based corrective feedback on their grammatical errors. However, the control group (N = 20) did not receive technology-enhanced corrective feedback during the experiment. The results highlighted: (a) the technology-enhanced, experimental group outperformed their counterpart with regard to grammatical accuracy, (b) the online Skype-based text chatting context played a mediating role in reinforcing the experimental group’s grammatical knowledge, and (c) the participants displayed a high level of motivation to initiate and engage in L2 communication. The participants’ experience of the Skype-based classroom emphasized themes of overcoming emotional problems in communication and fostering interpersonal relationship and rapport with the teacher and peers. Pedagogical implications focus on the potential of synchronous computer-mediated communication-based contexts as useful spaces for active collaborative learning and task engagement.
Polarized Deep Inelastic Scattering Off the Neutron From Gauge/String Duality

We investigate deep inelastic scattering off the polarized 'neutron' using gauge/string duality. The 'neutron' corresponds to a supergravity mode of the neutral dilatino. Through introducing the Pauli interaction term into the action in AdS{sub 5} space, we calculate the polarized deep inelastic structure functions of the 'neutron' in supergravity approximation at large t' Hooft coupling {lambda} and finite x with {lambda}{sup -1/2}<<x<1. In comparison with the charged dilatino-''proton,'' which has been obtained in the previous work by Gao and Xiao, we find the structure functions of the 'neutron' are power suppressed at the same order as the ones of the ''proton. '' Especially, we find the Burkhardt-Cottingham-like sum rule, which is satisfied in the work by Gao and Xiao, is broken due to the Pauli interaction term. We also illustrate how such a Pauli interaction term can arise naturally from higher dimensional fermion-graviton coupling through the usual Kaluza-Klein reduction.
Precursory moment release scales with earthquake magnitude

Today, observations of earthquake precursors remain widely debated. While precursory slow slip is an important feature of earthquake nucleation, foreshock sequences are not always observed and their temporal evolution remains unconstrained. Here, we report on stick-slip experiments (laboratory earthquakes) conducted under seismogenic stresses in dry and fluid pressure conditions. We show that the precursory moment release scales with mainshock magnitude irrespective of the slip behavior (seismic or aseismic), the presence of fluid and the fault's slip history. Importantly, this observation is supported by earthquake nucleation theory and holds for natural earthquakes in a magnitude range from M_w 6.0 to M_w 9.0. Even though a large gap remains between laboratory and natural observations, moderate to large earthquakes may be foresighted through integrated seismological and geodetic measurements of both seismic and aseismic slip during earthquake nucleation.
Spectral variation in the supergiant fast X-ray transient SAX J1818.6-1703 observed by XMM-Newton and INTEGRAL

We present the results of a 30ks XMM-Newton observation of the supergiant fast X-ray transient (SFXT) SAX J1818.6-1703 - the first in-depth soft X-ray study of this source around periastron. INTEGRAL observations shortly before and after the XMM-Newton observation show the source to be in an atypically active state. Over the course of the XMM-Newton observation, the source shows a dynamic range of ~100 with a luminosity greater than 1$\times$10$^{35}$ erg s$^{-1}$ for the majority of the observation. After an ~6 ks period of low luminosity (~10$^{34}$ erg s$^{-1}$) emission, SAX J1818.6-1703 enters a phase of fast flaring activity, with flares 250 s long, separated by ~2ks. The source then enters a larger flare event of higher luminosity and ~8 ks duration. Spectral analysis revealed evidence for a significant change in spectral shape during the observation with a photon index varying from {\Gamma} ~ 2.5 during the initial low luminosity emission phase, to {\Gamma} ~ 1.9 through the fast flaring activity, and a significant change to {\Gamma} ~ 0.3 during the main flare. The intrinsic absorbing column density throughout the observation (n$_H$ ~ 5$\times$10$^{23}$ cm$^{-2}$) is among the highest measured from an SFXT, and together with the XMM-Newton and INTEGRAL luminosities, consistent with the neutron star encountering an unusually dense wind environment around periastron. Although other mechanisms cannot be ruled out, we note that the onset of the brighter flares occurs at 3$\times$10$^{35}$ erg s$^{-1}$, a luminosity consistent with the threshold for the switch from a radiative-dominated to Compton cooling regime in the quasi-spherical settling accretion model.
Modular Quantum Information Processing by Dissipation

Dissipation can be used as a resource to control and simulate quantum systems. We discuss a modular model based on fast dissipation capable of performing universal quantum computation, and simulating arbitrary Lindbladian dynamics. The model consists of a network of elementary dissipation-generated modules and it is in principle scalable. In particular, we demonstrate the ability to dissipatively prepare all single qubit gates, and the CNOT gate; prerequisites for universal quantum computing. We also show a way to implement a type of quantum memory in a dissipative environment, whereby we can arbitrarily control the loss in both coherence, and concurrence, over the evolution. Moreover, our dissipation-assisted modular construction exhibits a degree of inbuilt robustness to Hamiltonian, and indeed Lindbladian errors, and as such is of potential practical relevance.
Testing the Molecular-Hydrogen Kennicutt-Schmidt Law in the Low-Density Environments of Extended Ultraviolet Disk Galaxies

Studying star formation beyond the optical radius of galaxies allows us to test empirical relations in extreme conditions with low average gas density and low molecular fraction. Previous studies discovered galaxies with extended ultraviolet (XUV) disks, which often contain star forming regions with lower Halpha-to-far-UV (FUV) flux ratios compared to inner disk star forming regions. However, most previous studies lack measurements of molecular gas, which is presumably the component of the interstellar medium out of which stars form. We analyzed published CO measurements and upper limits for fifteen star forming regions in the XUV or outer disk of three nearby spiral galaxies and a new CO upper limit from the IRAM 30 m telescope in one star forming region at r = 3.4 r_25 in the XUV disk of NGC 4625. We found that the star forming regions are in general consistent with the same molecular-hydrogen Kennicutt-Schmidt law that applies within the optical radius, independent of whether we used Halpha or FUV as the star formation rate (SFR) tracer. However, a number of the CO detections are significantly offset towards higher SFR surface density for their molecular hydrogen surface density. Deeper CO data may enable us to use the presence or absence of molecular gas as an evolutionary probe to break the degeneracy between age and stochastic sampling of the initial mass function as the explanation for the low Halpha-to-FUV flux ratios in XUV disks.
conceived of aspirations as impacted by daily states, such as the sense of exhaustion and crankiness following a night

conceived of aspirations as impacted by daily states, such as the sense of exhaustion and crankiness following a night of poor sleep. Instead, most of the literature treats aspirations as something akin to a personality trait (e.g., Huang et al., 2014), or at least a ‘mid-level’ characteristic – not quite as stable as personality but certainly not as situational as behavioral intentions (e.g., Judge & Kammeyer-Mueller, 2012). Despite this general tendency in the literature, some research has shown that even temporary situational factors can impact career aspirations. Indeed, Steffens et al. (2018) found that participants’ aspirations fluctuated as a function of being randomly assigned to receive either positive or negative feedback about their leadership potential, thereby lending support to the notion that aspirations might also fluctuate daily in response to various events or emotional states. The opening quote, in referencing Sheryl Sandberg’s work on women and leadership, implies that women’s career aspirations might be differentially impacted by situational factors relative to men’s, a suggestion that receives support from a recent collection of research. For example, Fritz & van Knippenberg (2017) found that both women’s and men’s leadership aspirations were positively impacted by the presence of a cooperative organizational climate, but “Years ago, Sheryl [Sandberg] famously told us to ‘lean in’ but as comedian Ali Wong quips, many of us are tired, and just want to “lie down’” (Ly, 2017). This tongue-in-cheek quote taken from a professional woman’s LinkedIn blog suggests that intentions to pursue more status and responsibility at work fluctuate as a function of physical or affective states, one of which is the state of exhaustion. Though this is an intuitive notion – that the energy one has on any given day to devote to achieving their goals will shape their daily persistence and engagement at work (Ilies & Judge, 2005) – scholars have generally not
Automodel solutions for Lévy flight-based transport on a uniform background

A wide class of non-stationary superdiffusive transport on a uniform background with a power-law decay at large distances of the step-length probability distribution function (PDF) is shown to possess an approximate automodel solution. The solution for the Green’s function is constructed using the scaling laws for the propagation front (relevant-to-superdiffusion average displacement) and asymptotic solutions far beyond and far in advance of the propagation front. These scaling laws are determined essentially by the long-free-path carriers (Lévy flights). The validity of the suggested automodel solution is proved by its comparison with numerical solutions in the one-dimensional (1D) case of the transport equation with a simple long-tailed PDF with various power-law exponents and in the 3D case of the Biberman–Holstein equation of the resonance radiation transfer for various (Doppler, Lorentz, Voigt and Holtsmark) spectral line shapes.
Sakharov's induced gravity on the AdS background: SM scale as inverse mass parameter of the Schwinger-DeWitt expansion

One loop quantum effective action W of scalar field 'living' on the AdS background of the Randall-Sundrum model is defined here by now popular way which excludes bulk UV divergencies; thus induced Planck mass is given not by the UV regularization parameter, like in Sakharov's pioneer work, but by the location of the UV-cut of AdS space. Resummation of Schwinger-DeWitt expansion of the action W is performed by the novel 'auxiliary mass' method. The inverse mass squared parameter of this expansion is determined by the location of the 'visible' IR-brane of the RS-model. Obtained expression for induced vacuum energy density coincides with the independently calculated VEV of the stress-energy tensor. Corresponding potential in 4 dimensions possesses a non-trivial extremum which hopefully will permit us to stabilize IR brane and hence to fix the observed small value of mass hierarchy in analogy with the Coleman-Weinberg mechanism. It is demonstrated that naive equating of values of the induced Planck mass and vacuum energy density to those of the RS-model determines otherwise arbitrary constants of the model. A principle of quantum self-consistency generalizing this approach is proposed.
COLLISIONLESS ELECTRON–ION SHOCKS IN RELATIVISTIC UNMAGNETIZED JET–AMBIENT INTERACTIONS: NON-THERMAL ELECTRON INJECTION BY DOUBLE LAYER

The course of non-thermal electron ejection in relativistic unmagnetized electron–ion shocks is investigated by performing self-consistent particle-in-cell simulations. The shocks are excited through the injection of a relativistic jet into ambient plasma, leading to two distinct shocks (referred to as the trailing shock and leading shock) and a contact discontinuity. The Weibel-like instabilities heat the electrons up to approximately half of the ion kinetic energy. The double layers formed in the trailing and leading edges then accelerate the electrons up to the ion kinetic energy. The electron distribution function in the leading edge shows a clear, non-thermal power-law tail which contains ∼1% of electrons and ∼8% of the electron energy. Its power-law index is −2.6. The acceleration efficiency is ∼23% by number and ∼50% by energy, and the power-law index is −1.8 for the electron distribution function in the trailing edge. The effect of the dimensionality is examined by comparing the results of three-dimensional simulations with those of two-dimensional simulations. The comparison demonstrates that electron acceleration is more efficient in two dimensions.
ORTHO-TO-PARA RATIO STUDIES OF SHOCKED H2 GAS IN THE TWO SUPERNOVA REMNANTS IC 443 AND HB 21

We present near-infrared (2.5–5.0 μm) spectral studies of shocked H2 gas in two supernova remnants, IC 443 and HB 21, which are well known for their interactions with nearby molecular clouds. The observations were performed with the Infrared Camera aboard the AKARI satellite. At the energy range 7000 K ≲ ≲ 20,000 K, the shocked H2 gas in IC 443 shows an ortho-to-para ratio (OPR) of 2.4+0.3− 0.2, which is significantly lower than the equilibrium value 3, suggesting the existence of non-equilibrium OPR. The shocked gas in HB 21 also indicates a potential non-equilibrium OPR in the range of 1.8–2.0. The level populations are well described by the power-law thermal admixture model with a single OPR, where the temperature integration range is 1000–4000 K. We conclude that the obtained non-equilibrium OPR probably originates from the reformed H2 gas of dissociative J-shocks, considering several factors such as the shock combination requirement, the line ratios, and the possibility that H2 gas can form on grains with a non-equilibrium OPR. We also investigate C-shocks and partially dissociative J-shocks as the origin of the non-equilibrium OPR. However, we find that they are incompatible with the observed ionic emission lines for which dissociative J-shocks are required to explain. The difference in the collision energy of H atoms on grain surfaces would give rise to the observed difference between the OPRs of IC 443 and HB 21, if dissociative J-shocks are responsible for the H2 emission. Our study suggests that dissociative J-shocks can produce shocked H2 gas with a non-equilibrium OPR.
Second law of quantum complexity

We give arguments for the existence of a thermodynamics of quantum complexity that includes a “second law of complexity. ” To guide us, we derive a correspondence between the computational (circuit) complexity of a quantum system of K qubits, and the positional entropy of a related classical system with 2K degrees of freedom. We also argue that the kinetic entropy of the classical system is equivalent to the Kolmogorov complexity of the quantum Hamiltonian. We observe that the expected pattern of growth of the complexity of the quantum system parallels the growth of entropy of the classical system. We argue that the property of having less-than-maximal complexity (uncomplexity) is a resource that can be expended to perform directed quantum computation. Although this paper is not primarily about black holes, we find a surprising interpretation of the uncomplexity resource as the accessible volume of spacetime behind a black hole horizon.
Distribution and evolution of galaxy groups in the Ursa Major supercluster

Context. We study an SDSS sample of galaxies within 50 Mpc of the nominal center of the Ursa Major supercluster. Aims. Our aim is to study galaxy distribution around groups in the supercluster and the link between the distribution of relaxed and nonrelaxed galaxy systems with respect to the supercluster environment. Methods. Using the FoF algorithm, 40 galaxy groups were identified in this region. Velocity distributions for these groups were studied after applying a 3 -clipping routine for outlier removal. We classified the systems according to the results of normality and substructure tests applied to member galaxies. Then, we studied the relative distribution of relaxed and nonrelaxed systems across the supercluster. Results. We find that 68% of galaxy groups are Gaussian and that all the non-Gaussian systems have substructures and probably correspond to multimodal systems in redshift space. We also find that the Gaussian systems inhabit the denser regions of the supercluster, with higher densities of both red and blue galaxies within 2.5 h 1 Mpc, and have smaller group-group pairwise separations. Conclusions. Our results suggest a spatial segregation of dynamical states, where relaxed systems may have formed and evolved earlier and faster around high-density peaks, while nonrelaxed systems may be growing slower on the peripheries of lower density peaks. In this picture, galaxy clustering seems to be prompting a continuous internal evolution in the supercluster, with several groups collapsing into the more evolved and contracted regions.
THE SUPER-LINEAR SLOPE OF THE SPATIALLY RESOLVED STAR FORMATION LAW IN NGC 3521 AND NGC 5194 (M51a)

We have conducted interferometric observations with the Combined Array for Research in Millimeter Astronomy (CARMA) and an on-the-fly mapping with the 45 m telescope at Nobeyama Radio Observatory (NRO45) in the CO (J = 1–0) emission line of the nearby spiral galaxy NGC 3521. Using the new combined CARMA + NRO45 data of NGC 3521, together with similar data for NGC 5194 (M51a) and archival SINGS Hα, 24 μm THINGS H i, and Galaxy Evolution Explorer/Far-UV (FUV) data for these two galaxies, we investigate the empirical scaling law that connects the surface density of star formation rate (SFR) and cold gas (known as the Schmidt–Kennicutt law or S-K law) on a spatially resolved basis and find a super-linear slope for the S-K law when carefully subtracting the background emissions in the SFR image. We argue that plausibly deriving SFR maps of nearby galaxies requires the diffuse stellar and dust background emission to be subtracted carefully (especially in the mid-infrared and to a lesser extent in the FUV). Applying this approach, we perform a pixel-by-pixel analysis on both galaxies and quantitatively show that the controversial result whether the molecular S-K law (expressed as ) is super-linear or basically linear is a result of removing or preserving the local background. In both galaxies, the power index of the molecular S-K law is super-linear () at the highest available resolution (∼230 pc) and decreases monotonically for decreasing resolution. We also find in both galaxies that the scatter of the molecular S-K law () monotonically increases as the resolution becomes higher, indicating a trend for which the S-K law breaks down below some scale. Both and are systematically larger in M51a than in NGC 3521, but when plotted against the de-projected scale (δdp), both quantities become highly consistent for the two galaxies, tentatively suggesting that the sub-kpc molecular S-K law in spiral galaxies depends only on the scale being considered, without varying among spiral galaxies. A logarithmic function and a linear relation are obtained through fitting to the M51a data, which describes both galaxies impressively well on sub-kpc scales. A larger sample of galaxies with better sensitivity, resolution, and broader field of view are required to test the general applicability of these relations.
GLOBAL STAR FORMATION RATES AND DUST EMISSION OVER THE GALAXY INTERACTION SEQUENCE

We measured and modeled spectral energy distributions (SEDs) in 28 bands from the ultraviolet to the far-infrared (FIR) for 31 interacting galaxies in 14 systems. The sample is drawn from the Spitzer Interacting Galaxy Survey, which probes a range of galaxy interaction parameters at multiple wavelengths with an emphasis on the infrared bands. The subset presented in this paper consists of all galaxies for which FIR Herschel SPIRE observations are publicly available. Our SEDs combine the Herschel photometry with multi-wavelength data from Spitzer, GALEX, Swift UVOT, and 2MASS. While the shapes of the SEDs are broadly similar across our sample, strongly interacting galaxies typically have more mid-infrared emission relative to their near-infrared and FIR emission than weakly or moderately interacting galaxies. We modeled the full SEDs to derive host galaxy star formation rates (SFRs), specific star formation rates (sSFRs), stellar masses, dust temperatures, dust luminosities, and dust masses. We find increases in the dust luminosity and mass, SFR, and cold (15–25 K) dust temperature as the interaction progresses from moderately to strongly interacting and between non-interacting and strongly interacting galaxies. We also find increases in the SFR between weakly and strongly interacting galaxies. In contrast, the sSFR remains unchanged across all the interaction stages. The ultraviolet photometry is crucial for constraining the age of the stellar population and the SFR, while dust mass is primarily determined by SPIRE photometry. The SFR derived from the SED modeling agrees well with rates estimated by proportionality relations that depend on infrared emission.
Free Magnetic Energy in Solar Active Regions above the Minimum-Energy Relaxed State

To understand the physics of solar flares, including the local reorganization of the magnetic field and the acceleration of energetic particles, we have first to estimate the free magnetic energy available for such phenomena, which can be converted into kinetic and thermal energy. The free magnetic energy is the excess energy of a magnetic configuration compared to the minimum-energy state, which is a linear force-free field if the magnetic helicity of the configuration is conserved. We investigate the values of the free magnetic energy estimated from either the excess energy in extrapolated fields or the magnetic virial theorem. For four different active regions, we have reconstructed the nonlinear force-free field and the linear force-free field corresponding to the minimum-energy state. The free magnetic energies are then computed. From the energy budget and the observed magnetic activity in the active region, we conclude that the free energy above the minimum-energy state gives a better estimate and more insights into the flare process than the free energy above the potential field state.