Miracle-dz/UniFAR-FTUs huggingface dataset:
A transient solution for vesicle electrodeformation and relaxation

A transient analysis for vesicle deformation under direct-current electric fields is developed. The theory extends from a droplet model, with the additional consideration of a lipid membrane separating two fluids of arbitrary properties. For the latter, both a membrane-charging and a membrane-mechanical model are supplied. The vesicle is assumed to remain spheroidal in shape for all times. The main result is an ordinary differential equation governing the evolution of the vesicle aspect ratio. The effects of initial membrane tension and pulse length are examined. The model prediction is extensively compared with experimental data, and is shown to accurately capture the system behavior in the regime of no or weak electroporation. More importantly, the comparison reveals that vesicle relaxation obeys a similarity law regardless of the means of deformation. The process is governed by a single time scale that is a function of the vesicle initial radius, the fluid viscosity, and the initial membrane tension. This similarity scaling law can be used to calculate membrane properties from experimental data.
Non-thermal Processes in Black-Hole-Jet Magnetospheres

The environs of supermassive black holes are among the universe's most extreme phenomena. Understanding the physical processes occurring in the vicinity of black holes may provide the key to answer a number of fundamental astrophysical questions including the detectability of strong gravity effects, the formation and propagation of relativistic jets, the origin of the highest energy gamma-rays and cosmic rays, and the nature and evolution of the central engine in active galactic nuclei (AGN). As a step towards this direction, this paper reviews some of the progress achieved in the field based on observations in the very high energy domain. It particularly focuses on nonthermal particle acceleration and emission processes that may occur in the rotating magnetospheres originating from accreting, supermassive black hole systems. Topics covered include direct electric field acceleration in the black hole's magnetosphere, ultra-high energy cosmic ray production, Blandford–Znajek mechanism, centrifugal acceleration and magnetic reconnection, along with the relevant efficiency constraints imposed by interactions with matter, radiation and fields. By way of application, a detailed discussion of well-known sources (Sgr A*; Cen A; M87; NGC1399) is presented.
THE PERIOD–LUMINOSITY RELATION OF RED SUPERGIANT STARS IN THE SMALL MAGELLANIC CLOUD

The characteristics of light variation of red supergiant (RSG) stars in the Small Magellanic Cloud (SMC) are analyzed based on the nearly 8–10 year data collected by the ASAS and MACHO projects. The 126 identified RSGs are classified into five categories accordingly: 20 with poor photometry, 55 with no reliable period, 6 with semi-regular variation, 15 with a long secondary period (LSP) and distinguishable short period, and 30 with only an LSP. For the semi-regular variables and the LSP variables with distinguishable short period, the KS-band period–luminosity (P–L) relation is analyzed and compared with that of the Galaxy, the Large Magellanic Cloud, and M33. It is found that the RSGs in these galaxies obey a similar P–L relation except for those in the Galaxy. In addition, the P–L relations in the infrared bands, namely, the 2MASS JHKS, Spitzer/IRAC, and Spitzer/MIPS 24 μm bands, are derived with high reliability. The best P–L relation occurs in the Spitzer/IRAC [3.6] and [4.5] bands. Based on the comparison with the theoretical calculation of the P–L relation, the mode of pulsation of RSGs in the SMC is suggested to be the first-overtone radial mode.
Bias-Based Soft Label Learning for Facial Expression Recognition

Facial Expression Recognition (FER) suffers from misrecognition due to the similarities between expressions. To address this issue, popular works replace original annotations with soft labels to reflect expression similarities. However, existing soft label learning (SLL) modules are independent of FER modules. In this article, inspired by automatic control theory, we propose a bias-based soft label learning network for FER named EC-Net. For optimizing FER and SLL modules jointly, EC-Net constitutes the closed-loop feedback between the two modules by designing a module measuring and transmitting the bias between FER module predictions and target labels. Specifically, EC-Net contains three modules: E-subNet, C-subNet, and L-Transmitter. First, E-subNet, i.e., the FER module, attempts to converge to target labels under the supervision of soft labels, acting as the executor. Then, L-Transmitter measures the bias between E-subNet predictions and target labels. It converts multiple discrete biases to the bias-based label through spectral clustering and transmits it to C-subNet. Finally, C-SubNet, i.e., the SLL module, generates soft labels from the bias-based label with a cascaded learner and progressively distinguishes similar expressions. It updates the learned soft labels for E-subNet, performing like the controller. Supervised by the bias-based soft label, E-subNet effectively reduces the dominant bias caused by similar expressions. We conduct extensive experiments on four popular benchmarks, demonstrating the effectiveness of applying closed-loop feedback in the FER task.
ALMA MULTI-LINE OBSERVATIONS OF THE IR-BRIGHT MERGER VV 114

We present Atacama Large Millimeter/submillimeter Array cycle 0 observations of the molecular gas and dust in the IR-bright mid-stage merger VV 114 obtained at 160–800 pc resolution. The main aim of this study is to investigate the distribution and kinematics of the cold/warm gas and to quantify the spatial variation of the excitation conditions across the two merging disks. The data contain 10 molecular lines, including the first detection of extranuclear CH3OH emission in interacting galaxies, as well as continuum emission. We map the 12CO(3–2)/12CO(1–0) and the 12CO(1–0)/13CO(1–0) line ratio at 800 pc resolution (in the units of K km s−1), and find that these ratios vary from 0.2–0.8 and 5–50, respectively. Conversely, the 200 pc resolution HCN(4–3)/HCO+(4–3) line ratio shows low values (<0.5) at a filament across the disks except for the unresolved eastern nucleus which is three times higher (1.34 ± 0.09). We conclude from our observations and a radiative transfer analysis that the molecular gas in the VV 114 system consists of five components with different physical and chemical conditions, i.e., (1) dust-enshrouded nuclear starbursts and/or active galactic nuclei, (2) widespread star-forming dense gas, (3) merger-induced shocked gas, (4) quiescent tenuous gas arms without star formation, and (5) H2 gas mass of (3.8 ± 0.7) × 107 M ⊙ ? > (assuming a conversion factor of αCO = 0.8 M ⊙ ( K km s − 1 pc 2 ) − 1 ? > ) at the tip of the southern tidal arm, as a potential site of tidal dwarf galaxy formation.
The structure of TeV-bright shell-type supernova remnants

Aims. Two-dimensional magnetohydrodynamic (MHD) simulations are used to model the emission properties of TeVbright shell-type supernova remnants (SNRs) and to explore their nature. Methods. In the leptonic scenario for the TeV emission, the -ray emission is produced via Inverse Compton scattering of background soft photons by high-energy electrons accelerated by the shocks of the SNRs. Since the energy density of the Cosmic Microwave Background (CMB) radiation and that of the IR/Optical background photons are much higher than that of the photons produced by the same high-energy electrons via the synchrotron process, in a previous paper, we showed that the observed correlation between X-ray and TeV brightness of SNR RX J1713.7-3946 can be readily explained with the assumption that the energy density of relativistic electrons is proportional to that of the magnetic eld. The TeV emissivity is therefore proportional to the magnetic eld energy density and MHD simulations can be used to model the TeV structure of such remnants directly. 2D MHD simulations for SNRs are then performed under the assumption that the ambient interstellar medium is turbulent with the magnetic eld and density
A Preliminary VLBA Distance to the Core of Ophiuchus, with an Accuracy of 4%

The nonthermal 3.6 cm radio continuum emission from the young stars S1 and DoAr 21 in the core of Ophiuchus has been observed with the Very Long Baseline Array (VLBA) at 6 and 7 epochs, respectively, between June 2005 and August 2006. The typical separation between successive observations was 2-3 months. Thanks to the remarkably accurate astrometry delivered by the VLBA, the trajectory described by both stars on the plane of the sky could be traced very precisely, and modeled as the superposition of their trigonometric parallax and a uniform proper motion. The best fits yield distances to S1 and DoAr 21 of 116.9−6.4+7.2 and 121.9−5.3+5.8 pc, respectively. Combining these results, we estimate the mean distance to the Ophiuchus core to be 120.0−4.2+4.5 pc, a value consistent with several recent indirect determinations, but with a significantly improved accuracy of 4%. Both S1 and DoAr 21 happen to be members of tight binary systems, but our observations are not frequent enough to properly derive the corresponding orbital parameters. This could be done with additional data, however, and would result in a significantly improved accuracy on the distance determination.
Optimization of Wire Electric Discharge Machining (WEDM) Process Parameters for AISI 1045 Medium Carbon Steel Using Taguchi Design of Experiments

With the growth of the manufacturing industry, the demand for alloy materials with high hardness, toughness, and impact strength has increased. Since products from such alloy materials are extremely difficult to manufacture with high accuracy and reduced surface roughness using traditional machining techniques, wire electric discharge machining can be used to machine such complex parts with more precision. In this case-study-based research, machining factors such as current, pulse-on time, and voltage are studied to determine their effects on the material removal rate for AISI 1045 medium carbon steel. The Taguchi L9 orthogonal array is used in the design of experiments for optimization. Statistical techniques such as analysis of variance and signal-to-noise ratio are used to identify the control parameters that matter most in bringing about optimal results. Based on the results, the current is the most crucial control variable in this investigation. Moreover, the maximum material removal rate obtained was 0.7112 mm3/min with the obtained optimized values of current (I) = 16 A, voltage (V) = 50 V, and pulse-on time (Ton) = 100 µs.
KEPLER OBSERVATIONS OF RAPID OPTICAL VARIABILITY IN THE BL LACERTAE OBJECT W2R1926+42

We present the first Kepler monitoring of a strongly variable BL Lac, W2R1926+42. The light curve covers 181 days with ∼0.2% errors, 30 minute sampling and >90% duty cycle, showing numerous δI/I > 25% flares over timescales as short as a day. The flux distribution is highly skewed and non-Gaussian. The variability shows a strong rms-flux correlation with the clearest evidence to date for nonlinearity in this relation. We introduce a method to measure periodograms from the discrete autocorrelation function, an approach that may be well-suited to a wide range of Kepler data. The periodogram is not consistent with a simple power-law, but shows a flattening at frequencies below 7 × 10−5 Hz. Simple models of the power spectrum, such as a broken power law, do not produce acceptable fits, indicating that the Kepler blazar light curve requires more sophisticated mathematical and physical descriptions than currently in use.
STELLAR ABUNDANCES IN THE SOLAR NEIGHBORHOOD: THE HYPATIA CATALOG

We compile spectroscopic abundance data from 84 literature sources for 50 elements across 3058 stars in the solar neighborhood, within 150 pc of the Sun, to produce the Hypatia Catalog. We evaluate the variability of the spread in abundance measurements reported for the same star by different surveys. We also explore the likely association of the star within the Galactic disk, the corresponding observation and abundance determination methods for all catalogs in Hypatia, the influence of specific catalogs on the overall abundance trends, and the effect of normalizing all abundances to the same solar scale. The resulting stellar abundance determinations in the Hypatia Catalog are analyzed only for thin-disk stars with observations that are consistent between literature sources. As a result of our large data set, we find that the stars in the solar neighborhood may reveal an asymmetric abundance distribution, such that a [Fe/H]-rich group near the midplane is deficient in Mg, Si, S, Ca, Sc ii, Cr ii, and Ni as compared to stars farther from the plane. The Hypatia Catalog has a wide number of applications, including exoplanet hosts, thick- and thin-disk stars, and stars with different kinematic properties.
All-electrical generation and control of odd-frequency s-wave Cooper pairs in double quantum dots

We propose an all-electrical experimental setup to detect and manipulate the amplitude of odd-frequency pairing in a double quantum dot. Odd-frequency pair amplitude is induced from the breakdown of orbital symmetry when Cooper pairs are injected in the double dot with electrons in different dots. When the dot levels are aligned with the Fermi energy, i.e., on resonance, nonlocal Andreev processes are directly connected to the presence of odd-frequency pairing. Therefore, their amplitude can be manipulated by tuning the level positions. Detection of nonlocal Andreev processes by conductance measurements contributes a direct proof of the existence of odd-frequency pair amplitude and is available using current experimental techniques.
Revisiting the Redshift Distribution of Gamma-Ray Bursts in the Swift Era

Le & Dermer developed a gamma-ray burst (GRB) model to fit the redshift and the jet opening angle distributions measured with pre-Swift and Swift missions and showed that GRBs do not follow the star formation rate. Their fitted results were obtained without the opening angle distribution from Swift with an incomplete Swift sample, and the calculated jet opening angle distribution was obtained by assuming a flat spectrum. In this paper, we revisit the work done by Le & Dermer with an assumed broken power law GRB spectrum. Utilizing more than 100 GRBs in the Swift sample that include both the observed estimated redshifts and jet opening angles, we obtain a GRB burst rate functional form that gives acceptable fits to the pre-Swift and Swift redshift and jet opening angle distributions with an indication that an excess of GRBs exists at low redshift below . The mean redshifts and jet opening angles for pre-Swift (Swift) are (1.7) and ( ), respectively. Assuming a GRB rate density (SFR9), similar to the Hopkins & Beacom star formation history and as extended by Li, the fraction of high-redshift GRBs is estimated to be below 10% and 5% at and , respectively, and below 10% at .
Non-split and split deformations of AdS 5

The η deformation of the AdS 5 × S 5 superstring depends on a non-split r matrix for the superalgebra psu ( 2 , 2 ∣ 4 ) . Much of the investigation into this model has considered one particular choice, however there are a number of inequivalent alternatives. This is also true for the bosonic sector of the theory with su ( 2 , 2 ) , the isometry algebra of AdS 5 , admitting one split and three non-split r matrices. In this article we explore these r matrices and the corresponding geometries. We investigate their contraction limits, comment on supergravity backgrounds and demonstrate their relation to gauged-WZW deformations. We then extend the three non-split cases to AdS 5 × S 5 and compute four separate bosonic two-particle tree-level S-matrices based on inequivalent BMN-type light-cone gauges. The resulting S-matrices, while different, are related by momentum-dependent one-particle changes of basis.
PULSE INTENSITY MODULATION AND THE TIMING STABILITY OF MILLISECOND PULSARS: A CASE STUDY OF PSR J1713+0747

Most millisecond pulsars, like essentially all other radio pulsars, show timing errors well in excess of what is expected from additive radiometer noise alone. We show that changes in amplitude, shape, and pulse phase for the millisecond pulsar J1713+0747 cause this excess error. These changes appear to be uncorrelated from one pulse period to the next. The resulting time of arrival (TOA) variations are correlated across a wide frequency range and is observed with different backend processors on different days, confirming that they are intrinsic in origin and not an instrumental effect or caused by strongly frequency-dependent interstellar scattering. Centroids of single pulses show an rms phase variation ≈40 μs, which dominates the timing error and is the same phase jitter phenomenon long known in slower spinning, canonical pulsars. We show that the amplitude modulations of single pulses are modestly correlated with their arrival time fluctuations. We also demonstrate that single-pulse variations are completely consistent with arrival time variations of pulse profiles obtained by integrating N pulses such that the arrival-time error decreases proportional to . We investigate methods for correcting TOAs for these pulse-shape changes, including multi-component TOA fitting and principal component analysis. These techniques are not found to improve the timing precision of the observations. We conclude that when pulse-shape changes dominate timing errors, the timing precision of PSR J1713+0747 can be only improved by averaging over a larger number of pulses.
The effect of different fillers, loads, and sliding distance on adhesive wear in woven e-glass fabric composites

In this study, adhesive wear of woven E-Glass fabric reinforced composites filled with aramid, B4C and mica particles at 0.5% wt. and 1.5% wt. ratios were carried out under dry sliding conditions. The effects of filler type, applied loads (5, 10 and 15 N) and sliding distances (250, 500 and 750 m) on the tribological behavior of the composites were investigated on the pin-on-disc device. As a result of the studies, it was determined that the friction coefficient in aramid reinforced composites was lower than the other reinforced composites. In wear volume due to wear, it was observed that the aramid wear volume was less. In addition, Wear volume increased with increasing load for all particle reinforcements. But, the highest wear volume occurred in the neat wear sample at 15 N load conditions. For the wear rate and wear volume, the fillers have shown improvement up to 1.5% wt. in the composite. 1.5% wt. aramid-filled glass fiber woven composites showed the lowest wear rate: 2.82 × 10−4 mm3/N-m (at 15 N normal load). In addition, in the scanning electron microscope images taken, it was observed that there were breaks in the size of 15.07 µm in the epoxy and 61.11 µm in the fibers. The use of aramid with particle reinforcement rather than fiber is important for wear. In addition, the lowest wear volume was 65% more resistant at 1.5% wt aramid reinforcement and at 15 N load compared to the unreinforced composite in the abrasion tests.
Evaluation of Specific Cementation Criteria on Total Elbow Arthroplasty – A Mono-Center Analysis of 31 Cases, with Minimum Follow-up of 4 Years

Background and study aim: Total elbow arthroplasty (TEA) has gained popularity in recent years, with most surgeons favoring cemented elbow prostheses. The objective of this study was to evaluate the outcome of our series and if specific radiological cementation criteria may predict clinical outcome. Material and methods: All patients submitted to cemented TEA were retrospectively reviewed over a 10-year period in an institution. All radiographs performed in the immediate postoperative period were blindly evaluated and classified according to specific cementation criteria. The radiographs of the last medical appointment were also blindly evaluated for possible signs of loosening, with a minimum follow-up of 4 years. The complication rate, revision rate, average prosthesis survival and QuickDASH Score were also evaluated. Statistical analysis was then performed to evaluate whether cementation quality had an influence on clinical and radiological results. Results: A total of 31 TEA were identified. Patients with an inadequate or marginal ulnar cementation were 9.2 times more likely of having a cubital loosening (p=0.032; OR=9.2[95% CI 1-91]). However, inadequate or marginal humeral cementation did not have a statistically significant association with the presence of humeral loosening (p=0.27). In our sample, there were 4 cases of aseptic loosening requiring revision. In all of them there were marginal or inadequate cementations in one of the components. Conclusions: This work highlighted the importance of adequate cementation and radiological evaluation. From this study, we can conclude that poor ulnar cementation may predict radiological loosening and eventual need for revision. However, this loosening does not correlate with the patient’s clinical outcomes or the need for revision.
THE NEW MODEL OF CHEMICAL EVOLUTION OF r-PROCESS ELEMENTS BASED ON THE HIERARCHICAL GALAXY FORMATION. I. Ba AND Eu

We investigate the chemical enrichment of r-process elements in the early evolutionary stages of the Milky Way halo within the framework of hierarchical galaxy formation using a semi-analytic merger tree. In this paper, we focus on heavy r-process elements, Ba and Eu, of extremely metal-poor (EMP) stars and give constraints on their astronomical sites. Our models take into account changes of the surface abundances of EMP stars by the accretion of interstellar medium (ISM). We also consider metal-enrichment of intergalactic medium by galactic winds and the resultant pre-enrichment of proto-galaxies. The trend and scatter of the observed r-process abundances are well reproduced by our hierarchical model with ∼10% of core-collapse supernovae in low-mass end (∼10 M☉) as a dominant r-process source and the star formation efficiency of ∼10−10 yr−1. For neutron star mergers as an r-process source, their coalescence timescale has to be ∼107 yr, and the event rates ∼100 times larger than currently observed in the Galaxy. We find that the accretion of ISM is a dominant source of r-process elements for stars with [Ba/H] < −3.5. In this model, a majority of stars at [Fe/H] < −3 are formed without r-process elements, but their surfaces are polluted by the ISM accretion. The pre-enrichment affects ∼4% of proto-galaxies, and yet, is surpassed by the ISM accretion in the surface of EMP stars.
Transit Time Estimation in Catchments: Recent Developments and Future Directions

Water transit time is now a standard measure in catchment hydrological and ecohydrological research. The last comprehensive review of transit time modeling approaches was published 15+ years ago. But since then the field has largely expanded with new data, theory and applications. Here, we review these new developments with focus on water‐age‐balance approaches and data‐based approaches. We discuss and compare methods including StorAge‐Selection functions, well/partially mixed compartments, water age tracking through spatially distributed models, direct transit time estimates from controlled experiments, young water fractions, and ensemble hydrograph separation. We unify some of the heterogeneity in the literature that has crept in with these many new approaches, in an attempt to clarify the key differences and similarities among them. Finally, we point to open questions in transit time research, including what we still need from theory, models, field work, and community practice.