Miracle-dz/UniFAR-FTUs huggingface dataset:
Multiobjective RFID Network Optimization Using Multiobjective Evolutionary and Swarm Intelligence Approaches

The development of radio frequency identification (RFID) technology generates the most challenging RFID network planning (RNP) problem, which needs to be solved in order to operate the large-scale RFID network in an optimal fashion. RNP involves many objectives and constraints and has been proven to be a NP-hard multi-objective problem. The application of evolutionary algorithm (EA) and swarm intelligence (SI) for solving multiobjective RNP (MORNP) has gained significant attention in the literature, but these algorithms always transform multiple objectives into a single objective by weighted coefficient approach. In this paper, we use multiobjective EA and SI algorithms to find all the Pareto optimal solutions and to achieve the optimal planning solutions by simultaneously optimizing four conflicting objectives in MORNP, instead of transforming multiobjective functions into a single objective function. The experiment presents an exhaustive comparison of three successful multiobjective EA and SI, namely, the recently developed multiobjective artificial bee colony algorithm (MOABC), the nondominated sorting genetic algorithm II (NSGA-II), and the multiobjective particle swarm optimization (MOPSO), on MORNP instances of different nature, namely, the two-objective and three-objective MORNP. Simulation results show that MOABC proves to be more superior for planning RFID networks than NSGA-II and MOPSO in terms of optimization accuracy and computation robustness.
Oscillation of the magnetic moment in modulated martensites in Ni2MnGa studied by ab initio calculations

We have revealed the oscillations in the distribution of the magnetic moments in modulated martensites in Ni2MnGa ferromagnetic shape memory alloy, by first-principles density-functional calculations. It is demonstrated that the oscillation of Ni magnetic moment that depends on the atomic shuffling in the superstructure dominates the distribution of the total magnetic moment per Ni2MnGa unit. The structure change-associated total magnetic moment has been found to increase for Ni2MnGa unit from the cubic austenite to the tetragonal nonmodulated (NM) martensite through the monoclinic modulated martensites.
The Supernova Remnant CTA1 and the Surrounding Interstellar Medium

Dominion Radio Astrophysical Observatory aperture synthesis observations, in the continuum at 1420 MHz and in the 21 cm line of H I, are presented of the supernova remnant (SNR) CTA 1. The angular resolution is 1 arcmin. Full sensitivity to structures of all angular sizes down to this scale has been achieved by combining the aperture synthesis observations with single-antenna data. In the continuum, in addition to the well-known bright arcs giving the SNR the appearance of an incomplete shell structure, diffuse emission can be traced to the north and northeast of the remnant and also in the southwest. Some of these faint features coincide with diffuse [O III] emission. A comparison with the 100 μm coadded IRAS image shows the presence of two cavities of low infrared emissivity adjacent to these regions
The conjugate connection of a Yang-Mills connection

In general, the properties of a given connection and the conjugate connection in a vector bundle E over a closed Riemannian manifold (M, g) are different. It is interesting to find whether or not the conjugate connection of a Yang-Mills connection in a vector bundle E over (M, g) is a Yang-Mills connection. In this paper, we get the fact that a connection D in a vector bundle E over (M, g) is a Yang-Mills connection if and only if the conjugate connection is a Yang-Mills connection.
Temporal order identification: Some parameter dependencies

Temporal order identification thresholds (TOT) for auditory stimuli have long been believed to be independent of the parameters of the stimuli as long as the judgment of order is (apparently) based directly upon the temporal difference rather than modality‐specific stimulus interactions associated with the temporal difference. We have found that TOT is a direct function of stimulus duration and, at least for longer rise times, is also a function of the rise time of the stimuli. Finally, adding a new tone to the end of the stimulus complex alters TOT only for short duration stimulus complexes. The relationship between TOT and the perception of speech stimuli contrasted in initial onset characteristics is discussed.
Factors influencing cloud area at the capping inversion for shallow cumulus clouds

Large‐eddy simulations of marine cumulus clouds are performed. Aspects of the simulations are varied in order to identify those parameters that play a role in determining when the cumulus clouds spread out under the capping inversion into stratocumulus. These include the strength of the surface fluxes, which also affects the strength of the cumulus mass transport, the strength of the capping inversion, the moisture content of the free atmosphere, the strength of cloud‐top radiative cooling and whether there is significant precipitation or sedimentation of cloud drops. Tests are also performed to evaluate sensitivity to the model resolution.
BILU implicit multiblock Euler/Navier–Stokes simulation for rotor tip vortex and wake convection

In this paper, a block incomplete lower–upper (BILU) decomposition method is incorporated with a multiblock three‐dimensional Euler/Navier–Stokes solver for simulation of hovering rotor tip vortices and rotor wake convection. Results of both Euler and Navier–Stokes simulations are obtained and compared with experimental observations. The comparisons include surface pressure distributions and tip vortex trajectories. The comparisons suggest that resolution of the boundary layer is important for the accurate evaluation of the blade surface loading, but is less so for the correct prediction of the vortex trajectory. Numerical tests show that, using Courant–Friedrichs–Lewy (CFL) number of 10 or 30 with the developed BILU implicit scheme can be 6–7 times faster than an explicit scheme. The importance of solution acceleration schemes that increase the permitted time‐step is illustrated by comparing the evolving wake structures at different stages of the calculation. In contrast to fixed wing simulations, the extent of the wake structures is shown to require resolution of large physical time. This observation explains the poor performance that is obtained when employing convergence acceleration strategies originally intended for solution of equilibrium problems, such as the multigrid methods. Copyright © 2007 John Wiley & Sons, Ltd.
Speckle noise reduction in digital holography by use of multiple polarization holograms

A novel speckle reduction technique for digital holography is proposed. Multiple off-axis holograms are recorded using a circularly polarized illumination beam and a rotating linearly polarized reference beam. The speckle noise in the reconstructed images is suppressed by averaging these fields. We demonstrate the effectiveness of this technique experimentally and conduct additional statistical evaluation.
A seamless weather–climate multi‐model intercomparison on the representation of a high impact weather event in the western Mediterranean: HyMeX IOP12

High Impact Weather (HIW), particularly Heavy Precipitation Events (HPE), are common phenomena affecting the western Mediterranean (WMED) especially in the autumn period. Understanding and evaluating the capability to adequately represent such events in model simulations is one of the main goals of the Hydrological cycle in the Mediterranean Experiment (HyMeX) and the main motivation of this investigation.
The Position of Sagittarius A*: Accurate Alignment of the Radio and Infrared Reference Frames at the Galactic Center

We present a novel approach to the long-standing problem of locating the position of the compact nonthermal radio source Sgr A* on infrared images of the Galactic center region. Using the Very Large Array, we have detected SiO and H2O maser emission toward several sources within the central parsec of our Galaxy. These masers arise from the innermost parts of circumstellar envelopes of giant and supergiant stars that are members of the nuclear star cluster and appear as compact infrared sources in a diffraction-limited 2.2 μm infrared image. One of the SiO masers is associated with the M-type supergiant IRS 7, the most prominent 2.2 μm point source in the Galactic center region. The radio data allow measurements of the maser positions relative to the compact nonthermal radio continuum source Sgr A* with milliarcsecond accuracy. Because stellar SiO masers near the Galactic center trace their host stars to within a few milliarcseconds, these relative positions can be used to calibrate the plate scale and rotation of the infrared image. Our method allows registration of the radio relative to the infrared reference frame with an estimated accuracy of 0. ″03. Using the improved position accuracy we put a stringent upper limit on the 2.2 μm flux density of Sgr A* that is significantly lower than values predicted by recent theoretical model calculations.
Spatiotemporal Correlations and Turbulent Photospheric Flows from SOHO/MDI Velocity Data

Time series of high-resolution and full-disk velocity images obtained with the Michelson Doppler Imager (MDI) instrument on board SOHO have been used to calculate the spacetime spectrum of photospheric velocity flow. The effects of different methods for filtering acoustic oscillations have been carefully studied. It is found that the spectra show contributions both from organized structures that have their origin in the convection zone and from the turbulent flow. By considering time series of different duration and cadence in solar regions with different line-of-sight projections, it is possible to distinguish the contributions of the spectra from the two different kinds of flows. The spectra associated with the turbulent velocity fields obey power laws characterized by two scaling parameters whose values can be used to describe the type of diffusion. The first parameter is the spectral exponent of the spatial correlation function and the second is a scaling parameter of the time correlation function. Inclusion of the time parameter is an essential difference between the present work and other solar studies. Within the confidence limits of the data, the values of the two parameters indicate that the turbulent part of the flow in the scale range 16-120 Mm produces superdiffusive transport.
Research Design for Program Evaluation: The Regression-Discontinuity Approach

An electric power source system for a gyroscopic instrument in which the kinetic energy of the gyro rotor revolving at high speed is used as an induction generator during times when the normal electrical power source for the gyroscopic instrument fails and to maintain the gyroscopic instrument in its normal operative condition during the time the electrical power source is disconnected.
The chemical compositions of nine southern supergiant stars

A fine analysis of nine southern supergiants of spectral types F through K, including the bright Cepheid variable l Car, is presented. The average metal-to-hydrogen ratio is found to be twice the solar value. No essential differences are found between the nonvariable stars and the Cepheid variable.In an initial attempt to determine the spatial distribution of abundances within the local region of the Sun (r< or approx. =0.5 kpc), the abundances of this study are combined with abundances from previous studies. The data are consistent with a homogeneous distribution of metallicity in supergiants within 0.5 kpc of the Sun.
Heat Conduction Equation Finite Volume Method to Achieve on MATLAB

Diffusion only, two dimensional heat conduction has been described on partial differential equation. Based on Finite Volume Method, Discretized algebraic Equation of partial differential equation have been deduced. different coefficients and source terms have been discussed under different boundary conditions, which include prescribed heat flux, prescribed temperature, convection and insulated. Transient heat conduction analysis of infinite plate with uniform thickness and two dimensional rectangle region are realized by programming using MATLAB. It is useful to make the heat conduction equation more understandable by its solution with graphical expression, feasibility and stability of numerical method have been demonstrated by running result.
Graphene active plasmonic metamaterials for new types of terahertz lasers

This paper reviews recent advances in graphene active plasmonic metamaterials for new types of terahertz lasers. We theoretically discovered that when the population of Dirac Fermionic carriers in graphene are inverted by optical or electrical pumping the excitation of graphene plasmons by the THz photons results in propagating surface plasmon polaritons with giant gain in a wide THz range. Furthermore, when graphene is patterned in a micro- or nano-ribbon array by grating gate metallization, the structure acts as an active plasmonic metamaterial, providing a super-radiant plasmonic lasing with giant gain at the plasmon modes in a wide THz frequency range.
Hydrodynamics of X-ray induced stellar winds.

We present new theoretical models for X-ray induced stellar winds in binary systems. We numerically solve the hydrodynamic equations in one dimension, utilizing a simplified model of the physics of an X-ray heated plasma. The character of the solutions depends on three dimensionless parameters: (1) the ratio of the X-ray spectral temperature to the photospheric temperature; (2) the ratio of the X-ray temperature to a temperature characterizing the escape energy from the stellar surface; and (3) the ratio of the flow time to the heating time. Holding the first parameter fixed at a high value ( = 100), we explore the complete range of solutions produced by variations in the other two parameters.
Looking inside the butterfly diagram

The suitability of Maunder's butterfly diagram to give a realistic picture of the photospheric magnetic flux large scale distribution is discussed. The evolution of the sunspot zone in cycle 20 through 23 is described. To reduce the noise which covers any structure in the diagram, a smoothing algorithm has been applied to the sunspot data. This operation has eliminated any short period fluctuation, and given visibility to long duration phenomena. One of these phenomena is the fact that the equatorward drift of the spot zone center of mass results from the alternation of several prograde (namely, equatorward) segments with other stationary or poleward segments. The long duration of the stationary/retrograde phases as well as the similarities among the spot zone alternating paths in the cycles under examination prevent us from considering these features as meaningless fluctuations, randomly superimposed on the continuous equatorward migration. On the contrary, these features should be considered physically meaningful phenomena, requiring adequate explanations. Moreover, even the smoothed spotted area markedly oscillates. The compared examination of area and spot zone evolution allows us to infer details about the spotted area distribution inside the butterfly diagram. Links between the changing structure of the spot zone and the tachocline rotation rate oscillations are proposed. (© 2007 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)
Elastic electron scattering from helium: absolute experimental cross sections, theory and derived interaction potentials

The authors report new differential cross section measurements (E0=1.5-50 eV) and coupled channel optical model calculations for elastic scattering of electrons from helium. The experimental results, from a crossed electron-atomic beam apparatus are analysed via a complex phaseshift technique with the derived phaseshifts, and their associated errors, then being used to derive total elastic, total reaction, total momentum transfer and grand total cross sections, and their respective errors, in a mathematically rigorous manner. Further, the authors applied fixed-energy inverse scattering techniques to the present data in order to deduce the interaction potential between the colliding particles.
Publications ofthe Astronomical Society ofthe Pacific 98:246-251, February 1986 THROUGH THE INFRARED WITH LOGBOOK AND LANTERN SLIDES A HISTORY OF INFRARED ASTRONOMY FROM 1868 TO 1960*

Only nine years after Kirchoff published his radiation laws and eleven years before Stefan published the fourth power of absolute-temperature law, the fourth Earl of Rosse made the first infrared measurements of any astronomical body other than the Sun. He observed the Moon with a thermopile and the three-foot reflector at Birr Castle in 1868 (Rosse 1869, 1870, 1873). I begin this history of infrared astronomy with his work because he introduced two techniques, one of which was used for 80 years and the other, in modified form, is still used today. Filters that isolated infrared wave bands and were opaque to visible light did not exist, and so he conceived of using a plate of glass as a filter. By differencing the galvanometer readings with and without the glass and suitably correcting the glass readings for reflection losses, he measured the infrared flux from the Moon. This technique I will call subtractive filtering, and it was used until 1950. His first measurements were made with a single thermopile, and he discovered immediately that the galvanometer deflections were strongly influenced by changing telescope temperatures and air temperatures. He then conceived of using two identical thermopiles, one connected in opposition to the other, both side by side in the focal plane of the telescope. Only one thermopile was exposed to the Moon; the other saw only sky. This compensation technique is replaced today by the ac equivalent of “chopping” between the object and the sky. Lord Rosse compared his lunar deflections with those from blackened cans containing water of different temperatures, and he made extinction measurements at different elevations of the Moon. From these he derived a temperature of the full Moon of400°-500° F, presumably by linear extrapolation of the water-can deflections. His same measurements can now be interpreted with Stefan’s law and they do give the correct temperature of the Moon (Sinton 1958). He measured the lunation curve of the Moon, and he also observed a total eclipse. He noted that the infrared deflections from the Moon during the eclipse were closely proportional to the visible light, and he deduced that the Moon’s surface cooled extremely rapidly. His apparatus was not sufficiently sensitive to
Crack detection in beam-type structures using frequency data

A practical method to non-destructively locate and estimate size of a crack by using changes in natural frequencies of a structure is presented. First, a crack detection algorithm to locate and size cracks in beam-type structures using a few natural frequencies is outlined. A crack location model and a crack size model are formulated by relating fractional changes in modal energy to changes in natural frequencies due to damage such as cracks or other geometrical changes. Next, the feasibility and practicality of the crack detection scheme are evaluated for several damage scenarios by locating and sizing cracks in test beams for which a few natural frequencies are available. By applying the approach to the test beams, it is observed that crack can be confidently located with a relatively small localization error. It is also observed that crack size can be estimated with a relatively small size error.
Fluorescence lifetime imaging using light emitting diodes

We demonstrate flexible use of low cost, high-power light emitting diodes as illumination sources for fluorescence lifetime imaging (FLIM). Both time-domain and frequency-domain techniques have been implemented at wavelengths spanning the range 450–640 nm. Additionally, we demonstrate optically sectioned fluorescence lifetime imaging by combining structured illumination with frequency-domain FLIM.
An analytical model of sub‐Alfvénic moon‐plasma interactions with application to the hemisphere coupling effect

We develop a new analytical model of the Alfvén wing that is generated by the interaction between a planetary moon's ionosphere and its magnetospheric environment. While preceding analytical approaches assumed the obstacle's height‐integrated ionospheric conductivities to be spatially constant, the model presented here can take into account a continuous conductance profile that follows a power law. The electric potential in the interaction region, determining the electromagnetic fields of the Alfvén wing, can then be calculated from an Euler‐type differential equation. In this way, the model allows to include a realistic representation of the “suspension bridge”‐like conductance profile expected for the moon's ionosphere. The major drawback of this approach is its restriction to interaction scenarios where the ionospheric Pedersen conductance is large compared to the Hall conductance, and thus, the Alfvénic perturbations are approximately symmetric between the planet‐facing and the planet‐averted hemispheres of the moon. The model is applied to the hemisphere coupling effect observed at Enceladus, i.e., to the surface currents and the associated magnetic discontinuities that arise from a north‐south asymmetry of the obstacle to the plasma flow. We show that the occurrence of this effect is very robust against changes in the conductance profile of Enceladus' plume, and we derive upper limits for the strength of the magnetic field jumps generated by the hemisphere coupling effect. During all 11 reported detections of the hemisphere coupling currents at Enceladus, the observed magnetic field jumps were clearly weaker than the proposed limits. Our findings are also relevant for future in situ studies of putative plumes at the Jovian moon Europa.
Transfer printing methods for the fabrication of flexible organic electronics

A transfer printing method for fabricating organic electronics onto flexible substrates has been developed. The method relies primarily on differential adhesion for the transfer of a printable layer from a transfer substrate to a device substrate. The works of adhesion and cohesion for successful printing are discussed and developed for a model organic thin-film transistor device consisting of a polyethylene terephthalate (PET) substrate, gold (Au) gate and source/drain electrodes, a polymethylmethacrylate (PMMA) [or poly(4-vinylphenol)] dielectric layer, and a pentacene (Pn) organic semiconductor layer. The device components are sequentially printed onto the PET device substrate with no mixed processing steps performed on the device substrate. Optimum printing conditions for the Pn layer were determined to be 600psi and 120°C for 3min. A set of devices with a PMMA dielectric layer was measured as a function of channel length and exhibited a contact resistance corrected mobility of 0.237cm2∕Vs. This is la.
Propagating behavior of rectangular waveguide loaded with dissipative magnetic slab by using new algorithm

Propagating constants of rectangular waveguide loaded with dissipative slab obey complex transcendental equation, of which the property of multiroot and the dependence of modes on those roots often make people puzzled, especially for dissipative magnetic materials in an asymmetrically filling situation. An effective new algorithm combining Genetic Algorithm (GA) with Parameter Tracking Scheme (PTS) and Dynamic Searching Area (DSA) technique is developed. By using the algorithm, the propagating constants of waveguide symmetrically or asymmetrically loaded with dissipative magnetic slab are solved successfully and tightly linked to certain designated modes. The results also reveal some interesting phenomena, such as for some high‐order modes and certain thickness of loaded slab, the negative phase velocity may occur.