Miracle-dz/UniFAR-FTUs huggingface dataset:
The XUV irradiation and likely atmospheric escape of the super-Earth π Men c

π Men c was recently announced as the first confirmed exoplanet from the TESS mission. The planet has a radius of just 2 R⊕ and it transits a nearby Sun-like star of naked-eye brightness, making it the ideal target for atmospheric characterization of a super-Earth. Here we analyse archival ROSAT and Swift observations of π Men in order to determine the X-ray and extreme-ultraviolet irradiation of the planetary atmosphere and assess whether atmospheric escape is likely to be on-going. We find that π Men has a similar level of X-ray emission to the Sun, with L_X/L_bol = (4.84^{+0.92}_{-0.84})× 10^{-7}. However, due to its small orbital separation, the high-energy irradiation of the super-Earth is around 2000 times stronger than suffered by the Earth. We show that this is sufficient to drive atmospheric escape at a rate greater than that readily detected from the warm Neptune GJ 436b. Furthermore, we estimate π Men to be four times brighter at Ly α than GJ 436. Given the small atmospheric scale heights of super-Earths, together with their potentially cloudy atmospheres, and the consequent difficulty in measuring transmission spectra, we conclude that ultraviolet absorption by material escaping π Men c presents the best opportunity currently to determine the atmospheric composition of a super-Earth.
A direct algorithm for state deadbeat control

The authors propose a novel method for computing state deadbeat feedback gains from systems given in the staircase form. The proposed method uses only manipulations of given matrices, and hence is more direct than the existing method, which requires orthogonal transformations repeatedly. It is shown that the obtained gain is linear quadratic optimal for some weighting matrices. <<ETX>>
GaAs-based two-dimensional photonic crystal slab ring resonator consisting of a directional coupler and bent waveguides

We experimentally demonstrated a GaAs-based air-bridge-type photonic crystal ring resonator that has a triangular lattice pattern of air holes. The fabricated photonic crystal ring resonator is composed of bent waveguides and an asymmetric directional coupler that has three rows of air holes between neighboring line-defect waveguides. We successfully demonstrated ring resonant spectral response in the fabricated devices and experimentally made clear the dependence of the oscillation period on the optical path length of the ring resonator and the dependence of ring resonant spectral response on the coupling properties of the directional coupler. In addition, we theoretically and experimentally discuss the group-velocity dispersion in the photonic crystal slab waveguide.
Ccd photometry of the globular cluster m5. I. the color-magnitude diagram and luminosity functions

We present new BV I photometry for the halo globular cluster M5 (NGC 5904 = C1516+022), and examine the B- and I-band luminosity functions (LFs), based on over 20,000 stars — one of the largest samples ever gathered for a cluster luminosity function. Extensive artificial star tests have been conducted to quantify incompleteness as a function of magnitude and cluster radius. We do not see evidence in the LF of a “subgiant excess” or of a discrepancy in the relative numbers of stars on the red-giant branch and main sequence, both of which have been claimed in more metal-poor clusters. Enhancements of �-element have been taken into account in our analysis. This improves the agreement between the observed and predicted positions of the “red-giant bump”. Depending on the average �-element enhancement among globular clusters and the distance calibration, the observed discrepancy between the theoretical and observed position for a large number of clusters (Fusi Pecci et al. 1990) can be almost completely removed. The helium abundance of M5, as determined by the population ratio R, is found to be Y = 0.19 ± 0.02. However, there is no other indication that the helium abundance is different from other clusters of similar metallicity, and values calculated for other helium indicators are consistent with Y ≈ 0.23. The relative ages of M5, Palomar 5, M4, NGC 288, NGC 362, NGC 1261, NGC 1851 and � , , !
Prediction of loss in silicon steel from distorted waveforms

Using a simple formula, iron losses in oriented 3% silicon steel are predicted for nonsinusoidal flux density waveforms. The formula is based on the concept of frequency independent and dependent parts of the total loss and also includes anomalous loss. It is found that the accuracy of loss prediction depends upon the method of inserting values into this formula. If the values are based on experimental measurements from nonsinusoidal waveforms, then an accuracy of 2% is possible when the third harmonic content is 0 to 30% of the fundamental and the peak flux density is 1.4 to 1.8 T.
Excitation of short-wavelength spin waves in magnonic waveguides

By using phase-resolved micro-focus Brillouin light scattering spectroscopy, we demonstrate experimentally a phenomenon of wavelength conversion of spin waves propagating in tapered Permalloy waveguides. We show that this phenomenon enables efficient excitation of spin waves with sub-micrometer wavelengths being much smaller than the width of the microstrip antenna used for the excitation. The proposed excitation mechanism removes restrictions on the spin-wave wavelength imposed by the size of the antenna and enables improvement of performances of integrated magnonic devices.
Modal wave-front estimation from phase derivative measurements

Modal estimation of wave-front phase from phase derivatives is discussed. It is shown that it is desirable to minimize the number of modes estimated and the number of measurements used to maintain the quality of the estimates of low-order modes. It is also shown that mode cross coupling occurs when one tries to estimate modes higher than astigmatism.
Combination Tones and Their Origin

Combination tones corresponding to f1 − k (f2 − f1), with k a small positive integer, are often audible during stimulation by the two frequency components f1 and f2 (f1 < f2). In this paper primarily the cubic difference tone (CDT) 2f1 − f2 (k = 1) is studied. The research reported is directed at the type of nonlinearity generating the CDT, and at the site of CDT generation. The first experiment shows that the generation of the CDT is affected by a dip (a threshold elevation in a narrow frequency region). The CDT was perceived only when the level of f2 exceeded the elevated threshold. In the second experiment the cancellation method is used. The results suggest that the high‐frequency slope of the pattern of stimulation upon which the nonlinearity operates is comparable with the slope revealed in masking experiments. In the last experiments the cancellation method is reconsidered. Estimates of the CDT level found by various other measuring methods, in which the probe tone was presented nonsimultaneously w.
Terahertz gain in optically excited biased semiconductor superlattices

We investigate the terahertz-driven dynamics of excitons in an undoped optically excited biased semiconductor superlattice, including exciton-LO phonon scattering. We calculate the THz gain spectrum for a 820fsTHz pulse when the superlattice is excited by a 590fs optical pulse. The gain arises because, in contrast to the single-electron case, the excitonic Wannier-Stark ladder is asymmetric with respect to absorption and emission. We find that gain coefficients greater than 100cm−1 can be achieved at excitation densities for which domain formation should not occur.
Comparison of the accuracy of classification models to estimate healthcare use and costs associated with COPD exacerbations in Saskatchewan, Canada: A retrospective cohort study

Objective COPD is a high-cost disease and results in frequent contacts with the healthcare system. The study objective was to compare the accuracy of classification models with different covariates for classifying COPD patients into cost groups. Methods Linked health administrative databases from Saskatchewan, Canada, were used to identify a cohort of newly diagnosed COPD patients (April 1, 2007 to March 31, 2011) and their episodes of healthcare encounters for disease exacerbations. Total costs of the first and follow-up episodes were computed and patients were categorized as persistently high cost, occasionally high cost, and persistently low cost based on cumulative cost distribution ranking using the 75th percentile cutoff for high-cost status. Classification accuracy was compared for seven multinomial logistic regression models containing socio-demographic characteristics (i.e., base model), and socio-demographic and prior healthcare use characteristics (i.e., comparator models). Results Of the 1182 patients identified, 8.5% were classified as persistently high cost, 26.1% as occasionally high cost, and the remainder as persistently low cost. The persistently high-cost and occasionally high-cost patients incurred 10 times ($12 449 vs $1263) and seven times ($9334 vs $1263) more costs in their first exacerbation episode than persistently low-cost patients, respectively. Classification accuracy was 0.67 for the base model, whereas the comparator model containing socio-demographic and number of prior hospital admissions had the highest accuracy (0.72). Conclusions Costs associated with COPD exacerbation episodes are substantial. Adding prior hospitalization to socio-demographic characteristics produced the highest improvements in classification accuracy. Accurate classification models are important for identifying potential healthcare cost management strategies.
Colors of Luminous Bulges in Cluster MS 1054–03 and Field Galaxies at Redshifts z ~ 0.83

Using Hubble Space Telescope images, we separate the bulgelike (dubbed "pbulge") and disklike ("pdisk") components of 71 galaxies in the rich cluster MS 1054-03 and of 21 in the field. Our key finding is that luminous pbulges are very red, with rest-frame U-B ~ 0.45, while predicted colors are bluer by 0.20 mag. Moreover, these very red colors appear to be independent of environment, pbulge luminosity, pdisk color, and pbulge fraction. These results challenge any model of hierarchical galaxy formation that predicts the colors of distant (z ~ 0.8) luminous field and cluster bulges will differ. Our findings also disagree with other claims that 30% to 50% of bright bulges and elliptical galaxies at z ~ 1 are very blue (U-B ≤ 0).
On the Progenitor of the Type II‐Plateau Supernova 2003gd in M74

Hubble Space Telescope (HST) WFPC2 archival F606W and F300W images obtained within 1 year prior to the explosion of the nearby Type II supernova (SN) 2003gd in M74 (=NGC 628) have been analyzed to isolate the progenitor star. The SN site was located using precise astrometry applied to the HST images. Two plausible candidates are identified within 0 . ″6 of the SN position in the F606W image. Neither candidate was detected in the F300W image. SN 2003gd appears to be of Type II‐plateau (II‐P), with age ≈87 days on June 17 UT and with low reddening [E(B−V) = 0.13 mag]. The most likely of the two progenitor candidates has MV0 ≈ -3.5 mag (for an extinction‐corrected distance modulus of 29.3 mag), and on the basis of additional color information derived from a high‐quality, archival ground‐based I‐band image, we estimate that this star was a red supergiant with initial (zero‐age main sequence) mass MZAMS ≈ 8–9 M⊙. This mass estimate is somewhat lower than, but relatively consistent with, recent limits placed on the progenitor masses of other SNe II‐P, using HST data. Future HST imaging with the HST Advanced Camera for Surveys, when the SN has faded considerably, will be very useful in pinpointing the exact SN location and securing identification of the progenitor. If our proposed candidate is confirmed, it will be only the sixth SN progenitor ever directly identified.
Revisiting the stellar velocity ellipsoid-Hubble-type relation: observations versus simulations

The stellar velocity ellipsoid (SVE) in galaxies can provide important information on the processes that participate in the dynamical heating of their disc components (e.g. giant molecular clouds, mergers, spiral density waves, bars). Earlier findings suggested a strong relation between the shape of the disc SVE and Hubble type, with later-type galaxies displaying more anisotropic ellipsoids and early-types being more isotropic. In this paper, we revisit the strength of this relation using an exhaustive compilation of observational results from the literature on this issue. We find no clear correlation between the shape of the disc SVE and morphological type, and show that galaxies with the same Hubble type display a wide range of vertical-to-radial velocity dispersion ratios. The points are distributed around a mean value and scatter of $\sigma_z/\sigma_R=0.7\pm 0.2$. With the aid of numerical simulations, we argue that different mechanisms might influence the shape of the SVE in the same manner and that the same process (e.g. mergers) does not have the same impact in all the galaxies. The complexity of the observational picture is confirmed by these simulations, which suggest that the vertical-to-radial axis ratio of the SVE is not a good indicator of the main source of disc heating. Our analysis of those simulations also indicates that the observed shape of the disc SVE may be affected by several processes simultaneously and that the signatures of some of them (e.g. mergers) fade over time.
Thermo-optic photonic crystal light modulator

A device concept is proposed for modulating light in silicon-based photonic crystal devices by using highly localized high-temperature modulation of a compact device to vary the position of the cutoff frequency in a photonic crystal waveguide and modulate light. The position of the cutoff frequency can be varied by up to 60nm at the telecommunication wavelength of 1550nm by locally increasing the temperature of the device. Modulators of a few to several micrometers in width can be designed that can modulate light with extinction ratios up to 50dB and low insertion loss.
Extraction of bare form factors for Bs →Kℓν decays in nonperturbative HQET

We discuss the extraction of the ground state [Formula: see text] matrix elements from Euclidean lattice correlation functions. The emphasis is on the elimination of excited state contributions. Two typical gauge-field ensembles with lattice spacings 0.075, 0.05 fm and pion masses 330, 270 MeV are used from the O[Formula: see text]-improved CLS 2-flavor simulations and the final state momentum is [Formula: see text] GeV. The b-quark is treated in HQET including the [Formula: see text] corrections. Fits to two-point and three-point correlation functions and suitable ratios including summed ratios are used, yielding consistent results with precision of around 2% which is not limited by the [Formula: see text] corrections but by the dominating static form factors. Excited state contributions are under reasonable control but are the bottleneck towards precision. We do not yet include a specific investigation of multi-hadron contaminations, a gap in the literature which ought to be filled soon.
The SIRTF First-Look Survey. I. VLA Image and Source Catalog

The First-Look Survey (FLS) of the Space Infrared Telescope Facility (SIRTF) will cover about 5 deg2 centered on J2000.0 α = 17h18m, δ = +59°30′ in order to characterize the extragalactic infrared sky 2 orders of magnitude deeper than the IRAS survey. We expect that most of the FLS far-infrared (λ = 160, 70, and 24 μm) sources will be star-forming galaxies obeying the very tight far-infrared/radio correlation and will be continuum radio sources with flux densities S ≳ 100 μJy at ν = 1.4 GHz. Conversely, radio sources stronger than 100 μJy are usually powered by star-forming galaxies, plus some active galactic nuclei, and most should be detectable by the SIRTF FLS. Thus, a sensitive radio survey can be used to select and identify most of the SIRTF FLS source population before launch. We used the B configuration of the VLA to make an image of the FLS area at ν = 1.4 GHz with σ ≈ 23 μJy beam-1 rms fluctuations, θ = 5. ″0 resolution, and σα ≈ σδ ≲ 0. ″5 rms uncertainties in right ascension and declination. The resulting radio image and catalog of 3565 radio components with peak flux densities Sp ≥ 5 σ = 115 μJy beam-1 have been released via the Web to expedite follow-up optical identification and spectroscopy.
Influence of surfactant on drop deformation in an electric field

The deformation of a surfactant-covered, viscous drop suspended in a viscous fluid under the influence of an electric field is investigated using numerical simulations. The full Navier–Stokes equations are solved in both fluid phases, and the motion of the interface and the interfacial discontinuities are handled using the level-set method. The leaky-dielectric model is used to take into account the effect of an electric field. The surfactant is assumed to be insoluble, and an evolution equation for the motion of surfactant is solved along the drop surface. The surfactant concentration and the interfacial tension are coupled through a nonlinear equation of state. The numerical results show that the effect of surfactant strongly depends on the relative permittivity and conductivity between the fluids. The presence of surfactant can both increase and reduce the deformation, depending on the shape of the deformation and the direction of the electrically induced circulation.
Evolution of the Kinematic Structure and Precipitation Characteristics of a Mesoscale Convective System on 20,May 1979

Abstract The relationship of vertical motion to the occurrence of precipitation from the convective and stratiform regions of a mesoscale convective system (MCS) is presented. On 20–21 May 1979, an MCS developed over portions of Oklahoma, Texas, and Arkansas. The uniqueness of this system was its lack of squall-line characteristics and development of a large stratiform precipitation region. The evolution of the system is detailed by rawinsonde observations, radar cross sections, 15-min composite analyses of six NWS WSR-57 radars, and by raingages. The genesis stage of the MCS was described by strong convection along an east-west cold front that was reinforced by outflow generated by two mesoscale convective complexes (MCCS) that formed tile night before in Kansas and Missouri. The mature stage of the MCS was characterized by the development of a large stratiform precipitation region while convection was limited to the southern and eastern flanks of the system. Finally, in the dissipative stage, a moderate.
Theory of Multipole Solutions to the Sourceless Grad-Shafranov Equation in Plasma Physics

The rules to write out any one of the linearly independent functions belonging to the infinite set of those in polynomial form that satisfy the sourceless Grad-Shafranov equation as stated in the toroidal-polar coordinate system are established. It is found that a polynomial solution even in the poloidal angle is given by the product of an integral power of the radial coordinate variable by a complete polynomial of equal degree in this same variable with angular-dependent coefficient functions that are linear combinations of a finite number of Chebyshev polynomials in the cosine of the poloidal angle, the numerical coefficients of these being expressed in terms of the binomial numbers of Pascal's arithmetic triangle. Tables of the ten polynomial solutions of the lowest degrees are provided in variables of the toroidal-polar and of the cylindrical coordinate systems.
Understanding disk galaxy rotation velocities without dark matter contribution--a physical process for MOND?

An impact model of gravity designed to emulate Newton's law of gravitation is applied to the radial acceleration of disk galaxies. Based on this model (Wilhelm et al. 2013), the rotation velocity curves can be understood without the need to postulate any dark matter contribution. The increased acceleration in the plane of the disk is a consequence of multiple interactions of gravitons (called "quadrupoles" in the original paper) and the subsequent propagation in this plane and not in three-dimensional space. The concept provides a physical process that relates the fit parameter of the acceleration scale defined by McGaugh et al. (2016) to the mean free path length of gravitons in the disks of galaxies. It may also explain the modification of the gravitational interaction at low acceleration levels in MOND (Milgrom 1983, 1994, 2015, 2016). Three examples are discussed in some detail: The spiral galaxies NGC 7814, NGC 6503 and M 33.
Cost-benefit analysis of two-unit parallel system with administrative delay in repair

The analysis of parallel systems with two dissimilar units is examined. Each unit has two modes—‘normal’ or ‘total failure’. Whenever an operative unit fails, an administrative delay occurs in locating the repairman and making him available at the system location. A system is observed at suitable regenerative epochs in order to obtain various economic related reliability characteristics. The explicit results are obtained in few particular cases.
Bimodality and Gaps on Globular Cluster Horizontal Branches. II. The Cases of NGC 6229, NGC 1851, and NGC 2808

The outer halo globular cluster NGC 6229 has a peculiar horizontal-branch (HB) morphology, with clear indications of a bimodal HB and a "gap" on the blue HB. In this paper, we present extensive synthetic HB simulations to determine whether peculiar distributions in the underlying physical parameters are needed to explain the observed HB morphology. We find that a unimodal mass distribution along the HB can satisfactorily account for the observed HB bimodality, provided the mass dispersion is substantially larger than usually inferred for the Galactic globular clusters. In this case, NGC 6229 should have a well-populated, extended blue tail. A truly bimodal distribution in HB masses can also satisfactorily account for the observed HB morphology, although in this case the existence of an extended blue tail is not necessarily implied. The other two well-known bimodal-HB clusters, NGC 1851 and NGC 2808, are briefly analyzed. While the HB morphology of NGC 1851 can also be reproduced with a unimodal mass distribution assuming a large mass dispersion, the same is not true of NGC 2808, for which a bimodal, and possibly multimodal, mass distribution seems definitely required. The problem of gaps on the blue HB is also discussed. Applying the standard Hawarden and Newell χ2 test, we find that the NGC 6229 gap is significant at the 99.7% level. However, in a set of 1000 simulations, blue-HB gaps comparable to the observed one are present in ~6%-9% of all cases. We employ a new and simple formalism, based on the binomial distribution, to explain the origin of this discrepancy, and conclude that Hawarden's method, in general, substantially overestimates the statistical significance of gaps.