Miracle-dz/UniFAR-FTUs huggingface dataset:
Surface abundances of light elements for a large sample of early B‐type stars – III. An analysis of helium lines in spectra of 102 stars

Non-local thermodynamic equilibrium analysis of He I lines in spectra of 102 B stars is implemented in order to derive the helium abundance He/H, the microturbulent parameter V t and the projected rotation velocity v sin i. A simultaneous determination of He/H and V t for the stars is effected by analysing equivalent widths of the 4471- and 4922-A lines primarily as indicators of He/H and the 4713-, 5016-, 5876- and 6678-A lines primarily as indicators of V t . The rotation velocities v sin i are found from profiles of the same lines. It is shown that, when V t > 7 km s -1 , the V t (He I) values determined from He I lines are systematically overestimated as compared with the V t (O II, N II) values derived from O II and N II lines. This discrepancy is especially appreciable for hot evolved B giants with V t (He i) = 16-23 km s -1 and may indicate a failure of classical model atmospheres to represent the strong He I lines for these stars. Two programme stars, HR 1512 and 7651, are found to be helium-weak stars. The remaining 100 stars are divided into three groups according to their masses M. The microturbulent parameter V t (He i) is low for all stars of group A (M = 4.1-6.9 M ○. ) and for all stars with the relative ages t/t MS 0.8), show V t (He I) up to 11 km s -1 . The helium abundance He/H is correlated with the relative age t/t MS in both groups; the averaged He/H enhancement during the MS phase is 26 per cent. For group C, containing the most massive stars (M = 12.4-18.8 M ○. ), the V t (He I) values display a correlation with t/t MS , varying from 4 to 23 km s -1 . The He/H determination for hot evolved B giants of the group with V t (He I) > 15 km s -1 depends on a choice between the V t (He i) and V t (O II, N II) scales. The mean He/H enrichment by 67 per cent during the MS phase is found, if the abundances He/H are based on the V t (O II, N II) scale; however, two evolved giants with especially high v sin i, HR 7446 and 7993, show the He/H enhancement by about a factor of 2.5. When using the same V t scale, we found a trend of He/H with projected rotational velocities v sin i; a large dispersion for v sin i > 150 km s -1 can result from differences in masses M. A comparison with the stellar model computations with rotationally induced mixing shows that the observed helium enrichment during the MS phase can be explained by rotation with initial velocities 250-400 km s -1 . The He/H distribution on M and v sin i based on the V t (O II, N II) scale seems to be in better agreement with the theory than one based on the V t (He i) scale. The mean value He/H = 0.10 derived for stars in the zero age main sequence (ZAMS) vicinity can be adopted as the typical initial helium abundance for early B stars in the solar neighbourhood.
Experimental observations on the links between surface perturbation parameters and shock-induced mass ejection

We have assembled together our ejecta measurements from explosively shocked tin acquired over a period of about ten years. The tin was cast at 0.99995 purity, and all of the tin targets or samples were shocked to loading pressures of about 27 GPa, allowing meaningful comparisons. The collected data are markedly consistent, and because the total ejected mass scales linearly with the perturbations amplitudes they can be used to estimate how much total Sn mass will be ejected from explosively shocked Sn, at similar loading pressures, based on the surface perturbation parameters of wavelength and amplitude. Most of the data were collected from periodic isosceles shapes that approximate sinusoidal perturbations. Importantly, however, we find that not all periodic perturbations behave similarly. For example, we observed that sawtooth (right triangular) perturbations eject more mass than an isosceles perturbation of similar depth and wavelength, demonstrating that masses ejected from irregular shaped perturbatio.
Percy W. Bridgman's second century

Percy Williams Bridgman's impact on science began in 1909 with his first three experimental papers. These publications on high pressure calibration, techniques, and compressibility, together with the many articles that followed, established his influence on the course of modern high pressure research. Grounded in classical thermodynamics and practical mechanics, his developments showed how the variable of pressure leads to myriad transformations in materials. Studies carried out under a broader range of conditions now provide unprecedented insights into chemical and physical properties at multimegabar pressures and temperatures from millikelvins to thousands of degrees, where novel electronic, magnetic, and superconducting phases are now being discovered. With careful attention to experimental techniques and material performance, Bridgman extended the available pressure range that could be achieved in the laboratory with the development of new devices. We are now witness to continued refinement of static and dynamic compression methods and in situ measurement techniques, including the marriage of high pressure methods with large facilities such as synchrotron, neutron, and laser sources. Bridgman showed the broad range of implications of this work; the modern field of high pressure research now spans physics and chemistry, geosciences and planetary science, materials science and technology, and biology. Selected examples illustrate Bridgman's impact and legacy in this, his second century. For dense hydrogen, new insights have been obtained from high P–T measurements as well as studies of alloys and compounds of hydrogen, leading to the creation of new metallic and superconducting phases. Studies of other hydrogen-rich systems provide both tests of fundamental theory and potentially useful materials for hydrogen storage. High pressure studies of oxides have led to new ferroelectric and multiferroic materials and phases with remarkable properties that guide the design and fabrication of new devices. With the discovery of super-Earths outside our solar system, the high pressure properties of silicates, oxides, volatiles, and the full complement of planetary materials are now problems of cosmic importance well beyond the conditions found on and within the Earth. Developments in high pressure biology are addressing the question of the depth of the biosphere, the processes and reservoirs of carbon in our planet, and new insights into the origins of life as we know it, as well as the possibility of extraterrestrial life. Improved materials that can withstand high P–T conditions and other extreme environments include new forms of diamond, which are advancing experimental methods and finding numerous applications in advanced technology. These developments dovetail with synergetic advances in a broad spectrum of radiation techniques including coherent X-ray, intense neutron, and ultrabright laser sources.
Polarizability of a pair of touching dielectric spheres

The electrostatic problem of two touching dielectric spheres in a uniform field is analyzed as an eigenfunction expansion in the tangent sphere frame. The spectrum of eigenfunctions is continuous; therefore, the scattered potential is expressed as a weighted integral of those eigenfunctions. It is shown that the weighting function satisfies a second-order ordinary differential equation, which contains only elementary functions. In particular, the longitudinal and transverse polarizabilities of the tangent sphere are being considered. We are also dealing with the plasmonic resonances (electrostatic resonances) that appear at the negative values of the permittivity e. Some years ago Paley, Radchik, and Smith [A. V. Paley, A. V. Radchik, and G. B. Smith, J. Appl. Phys. 73, 3446 (1993)] claimed to have found an exact solution for the problem of two touching dielectric spheres in a uniform field. In light of the present study, it seems that their result is incorrect.
Structures and Magnetic Properties of Grain‐Oriented 3.2% Silicon—Iron

After almost 30 years of use, grain‐oriented silicon—iron remains the most important soft ferromagnetic material where high permeability and low core loss are required.In this paper we show how grain structures which the metallurgist has learned to produce affect permeability at H=10 Oe and core loss at B=15 kG. Deviations from the ideal (110) [001] and (100) [001] are compared. The effect of thickness for both textures is shown over a range of about 1 to 25 mil. Ascertainment of the true effect depends on maintaining other factors constant, such as degree of texture and grain size. The effect of grain size on core loss of Epstein test specimens is shown over a wide range from 0.03‐ to 20‐mm diameter for a relatively constant degree of texture and chemical purity. For very small grain sizes, small grain diameter is detrimental to core loss but the effect is reversed for large grains near 10 mm diameter.Attainment of superior magnetic properties depends on combination of a high degree of crystal texture to.
Solar wind flow about the outer planets - Gas dynamic modeling of the Jupiter and Saturn bow shocks

Pioneer 10 and 11 and Voyager 1 and 2 observations are used to study global aspects of the solar wind interaction with Jupiter and Saturn. Solar wind measurements before and after the encounters are used to determine average upstream flow parameters at 5 and 9 AU. Bow shock and magnetopause position are found to vary as the fourth root of dynamic pressure at Jupiter and the sixth root at Saturn. The average distances to the nose of the magnetopause based upon the Pioneer and Voyager boundary crossings for Jupiter and Saturn are 68 RJ and 19 RS, respectively, after correction for varying solar wind pressure. In shape, the Jovian bow shock and magnetopause surfaces are similar to their terrestrial counterparts, but the width of the magnetosheath is 45% less than predicted by axisymmetric gas dynamic theory. This result is interpreted as evidence for strong polar flattening of the Jovian magnetosphere. The Saturnian magnetopause and bow shock boundaries are significantly more flared than at the earth with a subsolar magnetosheath that is 20% thinner than predicted by gas dynamic theory. On the basis of these results it is suggested that Saturn is intermediate between the earth and Jupiter in terms of polar flattening, with the unusual flaring of the Saturn magnetopause being due to the low ratio of static to dynamic pressure in the distant heliosphere.
Further photometry of LSI + 61°303

We report on further photometric observations of the highly variable radio binary star LSI +61°303 performed during 1987-1990. The data obtained in these observations, together with our previously published data, show a 26.5-d modulation in the stellar intensity as well as in the stellar colour. These findings are discussed in terms of the three models suggested for the radio outbursts of the system
A note on using the accelerated convergence method in climate models

Application of the accelerated convergence (or asynchronous integration) method of Bryan(1984) to climate problems with time-dependent forcing is investigated using an ocean generalcirculation model (GCM), with an idealized box ocean and forced with an idealized seasonalrestoring surface temperature. Numerical experiments consist of a control experiment, which isintegrated synchronously for 9000 years, and 2 experiments with asynchronous integration, onewith depth dependent acceleration and one with depth independent acceleration. The latter 2cases were integrated synchronously for 9000 years after asynchronous equilibria are reached.It is found that a few thousand years of synchronous integration is needed to reach a newequilibrium after asynchronous equilibrium is obtained, consistent with a scaling argument.However, at the new equilibrium, temperature in the deep ocean only differs from that of theearly stage of synchronous adjustment by about 0.01°C. So for practical purposes, 50 years ofsynchronous integration beyond asynchronous equilibrium is sufficient. A simple interpretationof the accelerated convergence method of Bryan is also presented.
Multivariate analogue of generalized Mittag-Leffler function

Following the results of Saxena and Kalla [Solutions of Volterra-type integro-differential equations with a generalized Lauricella confluent hypergeometric function in the kernels, Int. J. Math. Math. Sci. 8 (2005), pp. 1155–1170], we introduce and develop here a theory of multivariate generalization of the Mittag-Leffler function, which is defined as: where λ, γ j , ρ j ∈C, Re (ρ j )>0, j=1, …, m. Certain properties of this multivariate generalized Mittag-Leffler function associated with fractional calculus are established. Further, an integral operator with this function as a kernel, in the following form: is studied in the space L(a, b). An analogy of the semi-group property for the composition of two such operators with different indices is proved. A composition of the Riemann–Liouville fractional integral operator with two such operators with different indices is established. The results derived in this paper provide generalization of the results given earlier by Kilbas et al. [Generalized Mittag-Leffler function and generalized fractional calculus operators, Integral Transforms Spec. Funct. 15 (2004), 31–49].
Journal of Quantitative Analysis in Sports Skill Evaluation in Women ' s Volleyball

The Brigham Young University Women's Volleyball Team recorded and rated all skills (pass, set, attack, etc.) and recorded rally outcomes (point for BYU, rally continues, point for opponent) for the entire 2006 home volleyball season. Only sequences of events occurring on BYU's side of the net were considered. Events followed one of these general patterns: serve-outcome, pass-setattack-outcome, or block-dig-set-attack-outcome. These sequences of events were assumed to be first-order Markov chains where the quality of each contact depended only on the quality of the previous contact but not explicitly on contacts further removed in the sequence. We represented these sequences in an extensive matrix of transition probabilities where the elements of the matrix were the probabilities of moving from one state to another. Each row of the count matrix, consisting of the number of times play moved from one transition state to another during the season, was assumed to have a multinomial distribution. A Dirichlet prior was formulated for each row, so posterior estimates of the transition probabilities were then available using Gibbs sampling. The different paths in the transition probability matrix were followed through the possible sequences of events at each step of the MCMC process to compute the posterior probability density that a perfect pass results in a point, a perfect set results in a point, etc. These posterior probability densities are used to address questions about skill performance in BYU Women's Volleyball.
Ultrafast electron dynamics in gold nanoshells

We present ultrafast optical studies on nanoshells, which consist of a nanoscale Au2S dielectric core surrounded by an ultrathin Au shell. The plasmon frequency of these nanoparticles can be controlled by varying the ratio of the core diameter to shell thickness. By tuning this plasmon peak, we have observed both transient bleaching and transient absorption for Au nanoshells embedded in polyvinyl alcohol. We relate the induced change in transmission of gold nanoshell films to the electron dynamics in the thin gold shell. Our results indicate that even when the plasmon frequency is shifted below the onset of interband transitions, interband effects are still of primary importance in determining the nonlinear optical response. An electron relaxation time of 1.6560. 10 ps is measured that corresponds to an electron-phonon coupling constant of 2.2 310 W/~m K! , smaller than that observed in bulk Au films. @S0163-1829~98! 50740-0#
Low energy (0.01-20 eV) electron scattering from acetylene

We report elastic differential, integral and momentum transfer cross sections for the electron-C2H2 system in the energy range of 0.01-20 eV. A parameter-free model potential approach is employed under the fixed-nuclei, single-centre, and close-coupling formalism. The electron exchange interaction is treated via a modified version of the semi-classical exchange model, while the short range correlation and long range polarization effects are included under the correlation-polarization approximation. This local and non-empirical potential, for both the exchange and charge distortion effects, is very successful in describing the 2 Pi g shape-resonance phenomenon around 2 eV. Our final results for both the differential and integral cross section compare very well with recent measurements. A Ramsauer-Townsend minimum is found around 0.2 eV in the total and momentum transfer cross sections.
The Small Magellanic Cloud, Supersoft X-Ray Binary 1E 0035.4–7230 (SMC 13)

Details of simultaneous photometric and spectroscopic observations of the optical counterpart of the "supersoft" X-ray source in the Small Magellanic Cloud, 1E 0035.4-7230 (SMC 13), are presented. Although the spectrum is dominated by emission lines of He II, the Balmer series of hydrogen is also present in emission with a strong decrement, and Balmer lines are seen as broad absorptions. Several high-ionization emission features are also present, including O VI (at 3811, 3834, and 5290 Å). Radial velocities and photometry confirm that the binary period is ~0. ͩ1719, and an improved value of the period is derived from 4 years of photometry and analysis of ROSAT HRI X-ray data. The orbital light variation is primarily due to an eclipse of the extensive accretion disk. X-ray and optical minima occur together. The UBV light curves are similar to each other, and no clear phase-related color variations are found. He II emission-line velocities show a semiamplitude of K ~ 100 km s-1, and maximum velocity occurs when the light curve indicates that the compact star would be moving away from the observer, suggesting that this emitting region may trace the orbital motion of the compact star. The range of possible masses implied for the X-ray source lies between 0.5 and 1.5 M☉ if the mass donor is a main-sequence star filling its Roche lobe. The light curve suggests values at the high end of this range. The broad H absorption lines appear to have a much larger velocity amplitude and a lower systemic velocity, making it difficult to understand their origin. We discuss possible models for the system.
The Effect of Micro Pin-Fin Shape on Thermal and Hydraulic Performance of Micro Pin-Fin Heat Sinks

Single micro pin-fin configurations having the same chord thickness/diameter but different shapes are numerically modeled to assess their heat transfer and hydraulic performances for Reynolds number values changing between 20 and 120. The configurations are three-dimensionally modeled based, and their heat transfer performances are evaluated using commercially available software COMSOL Multiphysics 3.5a. Navier–Stokes equations and continuity and energy equations are solved under steady-state conditions for single-phase water flows. To increase the computational efficiency, half of the domain consisting of a micro pin-fin located inside a microchannel is modeled using a symmetry plane. To validate the model, experimental data available in the literature are compared to simulation results obtained from the model of the same geometrical configuration as the experimental one. Accordingly, the numerical and experimental results show good agreement. Furthermore, performance evaluation study is performed using three-dimensional (3D) numerical models in the light of flow morphologies around micro pin-fins of various shapes. According to the results obtained from this study, the rectangular-shaped micro pin-fin configuration has the highest Nusselt number and friction factor over the whole Reynolds number range. However, the cone-shaped micro pin-fin configuration has the best thermal performance index, indicating that it could be more preferable to use micro pin-fins of unconventional shapes in micro pin-fin heat sinks.
Weed Management Strategies for Tomato Plasticulture Production in Florida

Florida is the top producer of fresh market tomatoes in the U.S., with an average production of 0.4 million metric tons. Tomatoes are commercially grown on plastic mulched raised beds in Southwest Florida, the primary production region in the state. Low tomato yield in plasticulture production is often associated with the poor control of nutsedge species. Nutsedge management, therefore, remains a critical production challenge for tomato growers in Florida. Sandy soil in this region promotes herbicide movement after heavy rainfall or irrigation, affecting weed suppression. This will also potentially impact the timely establishment of new tomato transplants and, consequently, the crop vigor if the herbicides get into the root zone. This review aims to present and discuss an overview of available options to safely manage major weeds of tomatoes, including nutsedge species, in plasticulture production. In addition, this review seeks to discuss an approach for utilizing herbicide adjuvants, such as spray deposition agents or oil binding agents, to improve herbicides’ efficacy and tomato crop safety by enhancing their retention in plastic mulched raised beds.
WOMEN’S AUTONOMY AND UNINTENDED PREGNANCY: AN IDHS 2017 DATA ANALYSIS

Unintended pregnancy impacts hugely on maternal and child health. This study aimed to examine the influence of women’s autonomy on unintended pregnancies including unwanted and mistimed pregnancies. Using the Indonesia Demographic and Health Survey (IDHS) 2017, this study analyzed 12,624 currently married women who had birth within five years preceding the survey. Women’s autonomy was constructed from several variables related to women’s decision on obtaining health care, visiting family, and spending large household purchase. The result of logistic regression analysis showed that women’s autonomy affected significantly on unintended pregnancy after controlling other variables. However, it implied a negative correlation in which autonomous women were 1.3 more likely to experience unintended pregnancy than their counterparts. Both parity and birth interval showed the biggest influences on unintended pregnancy; the odds ratios were 2.7 and 3.1 respectively. Women who married at age 21 years and above, lived in rural areas and decided the number of children to have with husbands tended to have a lower risk facing an unintended pregnancy. Improving IEC and counseling about family planning and reproductive health is expected to increase couples’ knowledge. Therefore, the decisions on the number of children and contraceptive use can be made jointly and unintended pregnancy will be prevented.