Miracle-dz/UniFAR-FTUs huggingface dataset:
Contribution of pitch-accent information to Japanese spoken-word recognition

This paper investigates the contribution of pitch-accent information to Japanese spoken-word recognition. Pitch accent of spoken words was manipulated by controlling F0. First, the present author investigated the relation between word intelligibility in the presence of noise and the adequacy of accent type in those words. In the intelligibility test, participants were presented with speech stimuli and a pink noise together, and were required to identify the word. In the rating test, the same participants were presented with the same speech stimuli and were required to rate the adequacy of the words’ accent types. Results indicated that the spoken words with more adequate accent type were more intelligible in the presence of noise. Next, the present author investigated the relation between reaction time in shadowing words and the adequacy of accent type in those words. In the shadowing task, the participants were required to shadow a word whose accent type was manipulated as soon as they identified it. The same participants participated in the rating test. The reaction time in the case of the words with an adequate accent was shorter than in the case of an inadequate one. These results support the hypothesis that pitch-accent information in Japanese spoken words might facilitate word recognition.
Triaxiality in disk galaxies

Thirty-two bulges of nearby spirals have been observed, to detect misalignment between disk and bulge apparent major axes. Such misalignment is unequivocally present in the majority of observed objects. This may be due to the triaxiality of disks, bulges, or both. The probability distribution function for the axial ratios is derived under the two extreme hypotheses, i.e., that either only disks (case I) or only bulges (cases II) are triaxial : the observational data are equally well fitted by either one. Since dynamical evidence and the internal twisting of isophotes show that bulges are triaxial, it is proposed that case I is unlikely, but an intermediate case cannot be ruled out
Z mode radiation in Jupiter's magnetosphere: The source of Jovian continuum radiation

Voyager spacecraft observations of Z mode waves in Jupiter's magnetosphere are analyzed. The signal appears in wideband spectrograms as an intense narrowband emission separated from the broadband continuum radiation seen at higher frequencies by a deep emission gap. The assumption that the intensity minimum corresponds to the electron plasma frequency organizes the data very well and provides a consistent interpretation of all spectral features in terms of plasma resonances and cutoffs. Several examples are given which demonstrate that the continuum radiation is composed of both left-hand and right-hand polarized waves with distinct cutoffs observed at the plasma frequency and right-hand cutoff frequency, respectively. A survey of a representative sample of events reveals that the Z mode peak frequency lies close to the left-hand cutoff frequency, suggesting that the observed characteristics of the emission are the result of wave reflection at the cutoff layer. In a substantial number of events, another distinct emission occurring near the upper hybrid resonance frequency is detected simultaneously with the Z mode. The entire set of observations gives strong support to the linear mode conversion theory of upper hybrid waves to continuum radiation mediated by the Z mode via the Budden radio window mechanism.
XMM-Newton observatory. I. The spacecraft and operations

The XMM-Newton Observatory is a cornerstone mission of the European Space Agency's Horizon 2000 programme, and is the largest scientific satellite it has launched to date. This paper summarises the principal characteristics of the Observatory which are pertinent to scientific operations. The scientific results appearing in this issue have been enabled by the unprecedentedly large effective area of the three mirror modules, which are briefly described. The in-orbit performance and preliminary calibrations of the observatory are briefly summarised. The observations from the XMM-Newton calibration and performance verification phase, which are public and from which most papers in this issue have been derived, are listed. The flow of data from the spacecraft, through the ground segment, to the production of preliminary science products supplied to users is also discussed.
Rigidity of hyperspaces

Given a metric continuum X, we consider the following hyperspaces of X: 2X , Cn(X) and Fn(X) (n ∈ N). Let F1(X) = {{x} : x ∈ X}. A hyperspace K(X) of X is said to be rigid, provided that for every homeomorphism h : K(X) → K(X), we have h(F1(X)) = F1(X). In this paper, we study conditions under which a continuum X has a rigid hyperspace Cn(X). Among others, we consider families of continua, such as dendroids, Peano continua, hereditarily indecomposable continua and smooth fans.
On the degree of approximation of functions by Fejér means

1. Continuous functions. I t has been proved by S. Bernstein that if f(x) is periodic and of the class Lip a, 0 < a < l , then the (C, 1) means an(x) = <rn(x;f) of the Fourier series of ƒ satisfy the condition (1.1) * * ( * ) ƒ ( * ) O ( f r ) , uniformly in x. The result is false for a = 1. The place of (1.1) is then taken by (1.2) crn(x) ƒ(*) 0(log »/»), and, as simple examples show, the factor log n on the right cannot be removed (see, for example, A. Zygmund, Trigonometrical series, p. 62). I t will be shown here that for power series the inequality (1.1) holds even for a = l . More generally, we have the following theorem. THEOREM 1. Suppose that f (x) is periodic, continuous, and that the Fourier series of f is of power series type,
Lateral Response Comparison of Unbonded Elastomeric Bearings Reinforced with Carbon Fiber Mesh and Steel

The vertical and horizontal stiffness used in design of bearings have been established in the last few decades. At the meantime, applicability of the theoretical approach developed to estimate vertical stiffness of the fiber-reinforced bearings has been verified in different academic studies. The suitability of conventional horizontal stiffness equation developed for elastomeric material, mainly for steel-reinforced elastomeric bearings, has not been tested in detail for use of fiber-reinforced elastomeric bearings. In this research, lateral response of fiber mesh-reinforced elastomeric bearings has been determined through experimental tests and the results have been compared by corresponding values pertaining to the steel-reinforced bearings. Within the test program, eight pairs of fiber mesh-reinforced bearings and eight pairs of steel-reinforced bearings are subjected to different levels of compressive stress and cyclic shear strains. Fiber-reinforced elastomeric bearings may be more favorable to be used in seismic regions due to lower horizontal stiffness that can result in mitigation of seismic forces for levels of 100% shear strain. Damping properties of these types of fiber mesh-reinforced bearings depend mostly on the selection of elastomeric material compounds. Suggestions have been made for the lateral response of fiber-reinforced elastomeric bearings. It has also been determined that the classical equation for lateral stiffness based on linear elastic behavior assumptions developed for elastomeric bearings does not always apply to the fiber-reinforced ones.
Small dc magnetic field response of magnetoelectric laminate composites

We have found that small long-type magnetoelectric (ME) laminate composites of magnetostrictive Tb1−xDyxFe2−y and piezoelectric Pb(Zr,Ti)O3 are quite sensitive to small dc magnetic field (Hdc) variations, when driven by a constant ac magnetic field. The sensitivity limit is Hdc<10−3Oe (10−7Tesla) using a constant amplitude low frequencies drive, and Hdc<10−4Oe (10−8Tesla) under resonant drive. In addition, an unusual ME switching effect—a 180° phase shift—was observed, in response to changes in the sign of a small Hdc.
Working time in Great Britain, 1975–1994: evidence from the New Earnings Survey panel data

Using individual‐based panel data from the New Earnings Survey, this paper provides a detailed analysis of the working time behaviour of British full‐time male and female workers as well as part‐time female workers. We investigate the following: male–female differences in basic and overtime working patterns; extensive overtime working; age‐related patterns of weekly basic and overtime hours; the effects of collective bargaining on hours of work; industrial, public–private sector and occupational breakdowns of basic and total hours. The results for the last three topics are based on estimates from fixed effect regressions with time‐varying parameters.
Finiteness and tenseness theorems for Riemannian foliations

We prove a finiteness theorem for the spectral sequence ( E i (∇), ( d ∇ ) i ) associated to a Riemannian foliation [inline-graphic xmlns:xlink="http://www.w3. org/1999/xlink" xlink:href="01i" /] on a compact manifold M , and to a flat vector bundle E over M with flat connection ∇. Using this result we prove that every Riemannian foliation on a compact manifold is tense (in the sense of [F. W. Kamber and Ph. Tondeur, Foliations and metrics, Progr. Math. , vol. 32, 1983, pp. 103-152]). We also show that the main tautness theorems for Riemannian foliations on compact manifolds, which were proved by several authors, are immediate consequences of our results.
Improved calculations for the C III 1907,1909 and Si III 1883,1892 electron density sensitive emission-line ratios, and a comparison with IUE observations

Atomic data are used in conjunction with the statistical equilibrium code of Dufton (1977) to calculate relative C III and Si III level populations, and hence emission-line strengths for a range of electron temperatures and densities. It is assumed that photoexcitation and deexcitaton rates are negligible in comparison with the corresponding collisional rates, that ionization to and recombination from other ionic levels are slow compared with bound-bound rates, and that all transitions are optically thin. The observed values of R1 and R2 for several planetary nebulae and a symbiotic star, measured from high-resolution spectra obtained with the IUE satellite, lead to electron densities that are compatible, and are also in good agreement with those deduced from line ratios in other species.
The viscous modulation of Lamb’s dipole vortex

A description of the adiabatic decay of the Lamb dipolar vortex is motivated by a variational characterization of the dipole. The parameters in the description are the values of the entrophy and linear momentum integrals, which change in time due to the dissipation. It is observed that the dipole dilates during the decay process [radius R∼(νt)1/2], while the amplitude of the vortex and its translation speed diminish in time proportional to (νt)−3/2 and (νt)−1.
Thermal imaging of standing spin waves

A simple method for the spatial imaging of standing spin-wave modes is demonstrated. We observed instantaneous temperature-rise images on a polycrystalline ferrimagnetic insulator Y3Fe5O12 slab using an infrared camera immediately after exciting magnetostatic standing spin-wave modes. We found that a wavy temperature distribution appears before the temperature distribution on the sample is smoothed by heat conduction. The distribution is consistent with the result of a calculation based on the Landau-Lifshitz-Gilbert equation using the effective demagnetization coefficient of the slab. This result proves that the method can image the spatially distributed patterns of standing spin waves.
Extension of the image model to arbitrary polyhedra

In this paper, the image model is extended to arbitrary polyhedra with any number of sides. This generalization makes it possible to model real concert halls much more accurately. The image positions computed by the method can be reduced to the directional impulse response in order to create audible simulations of the concert hall. Also, the image model can provide insight into the fundamental acoustical properties of different concert hall geometries. For example, the extended image model demonstrates that rectangular halls have an advantage over fan‐shaped halls with regard to spatial impression. We also show why the image model has fundamental advantages over another popular modeling technique, ray tracing.
Motion of transverse domain walls in thin magnetic nanostripes under transverse magnetic fields

The motion of transverse magnetic domain walls (TDW) in thin magnetic nanostripes under transverse magnetic fields (TMF) is investigated. In the absence of axial fields, an approximate static TDW profile is obtained under a TMF with an arbitrary orientation. This profile becomes exact if the TMF is parallel or perpendicular to the stripe plane. Under nonzero axial fields, the TDW becomes asymmetric and twisted, and it moves along the wire axis with two different propagation modes, rigid-body mode and precession mode, depending on the strength of the axial field. The critical strength separating these two modes is called modified Walker limit HW′. The TMF dependence of HW′, the TDW velocity and maximum twisting angle at HW′ were investigated both numerically and analytically. Moreover, it is shown that an early proposed velocity-field relationship fits well to the average velocities of a TDW above HW′. These results should be important for future developments of magnetic nanodevices based on DW propagation.
Stratospheric thermal damping times

Radiative damping of stratospheric temperature waves has wide implications for stratospheric physical processes. Damping is linearly parameterized as proportional to the local temperature. Thermal damping is calculated using the Goddard radiative transfer model and 17 years observations. Damping times of stratospheric temperatures are calculated for each month at all latitudes. These damping times are consistent with previous stratospheric estimates, but show shorter tropical time scales. Damping times range from an annual global average of 28 days (100 hPa) to 4 days (1 hPa). A considerable annual cycle is seen over much of the stratosphere, which is directly related to the annual cycle of temperatures, with longer damping times associated with colder temperatures.
Three-dimensional Interaction between a Planet and an Isothermal Gaseous Disk. II. Eccentricity Waves and Bending Waves

We perform linear calculations to investigate three-dimensional density waves excited by planets on elliptical and inclined orbits in isothermal protoplanetary disks. We consider small planets that have no disk gap around their orbits. Eccentricities and inclinations of planets are assumed to be smaller than the disk aspect ratio. This is reasonable for planets with no disk gap. The density wave excited by a planet with nonzero small eccentricity e and inclination i is decomposed into three components: the waves by a planet with e = i = 0, the eccentricity waves, and the bending waves. The eccentricity waves are related to the noncircular motion of the planet, while the bending waves are excited by the motion normal to the equatorial plane. In our formulation, these waves are described by the same wave equations, and only the perturbing potentials are different. We numerically solve the wave equations and calculate the force exerted on the planet by the waves. The force is not parallel to the velocity of the epicycle motion. From the force obtained, we also find the evolution rates in the eccentricity, the inclination, and the longitudes of the perihelion and the ascending node. The characteristic evolution time of these orbital elements is about 300(r/1 AU)2 yr for Earth-sized planets in the minimum-mass nebula disk. Eccentricity damping is caused by eccentricity waves, while inclination damping is due to bending waves for planets with small eccentricities and inclinations and with no disk gap. This means that to lowest order there is no coupling between the evolutions of the eccentricity and the inclination.
Role of approximate phase functions in Monte Carlo simulation of light propagation in tissues

We examine the phase function dependence of Monte Carlo simulation for light propagation in biomedical tissues. Two discrete particle tissue models are considered. The model phase functions can be obtained using the Mie theory. Dependence on various approximate phase functions is then examined for fluence, angular variation of diffuse reflectance and diffuse transmittance and their average values. The diffuse reflectance as a function of source–detector separation is also examined. The tissue parameters varied are the thickness and the constituent particle size and concentration. The results of this study place the use of the Henyey–Greenstein phase function on a firmer footing.
Dilatation dissipation: The concept and application in modeling compressible mixing layers

In this paper a concept of dilatation dissipation ed for high Reynolds number compressible turbulence is introduced. The concept is predicated on the existence of shocklike structures embedded within energetic turbulent eddies. A parametric expression for ed is found that contains calculable parameters of a turbulent field: turbulence energy and length scale, rms (turbulent) Mach number, and the kurtosis of the fluctuating velocity. The dilatation dissipation is incorporated in a second‐order closure model for compressible mixing layers and model predictions of mean and turbulence quantities are presented and, where possible, compared with experiments. It is shown that the model is capable of predicting the reduction of layer growth rates as a function of the convective Mach number Mc in accordance with Papamoschou–Roshko experiments; the computations are also shown to compare well with available measurements of Reynolds stresses at Mc=0.5–0.86. Finally, the physical implications of the new model and resu.
Properties of cooling flows in a flux-limited sample of clusters of galaxies

An analysis of the mass flow rates of cooling flows in an X-ray flux-limited sample of clusters of galaxies, in which most of the clusters have been observed with both imaging and spectroscopic detectors, is presented. Using high-quality images and constraints from broad-band spectra, it is found that the fraction of clusters with central cooling times less than the Hubble time is high (at least 70 per cent and possibly 90 per cent), indicating that cooling flows are a common and long-lived phenomenon. The fraction is higher than found in previous studies, due to our consideration of the effects of the spatial resolution and the signal-to-noise ratio of the images
THE HEAT EQUATION WITH A SINGULAR POTENTIAL

Of concern is the singular problem du/dt = au + (c/|x|2)iz + /((, x), tz(x,0) = u0(x), and its generalizations. Here c > 0, x G RN, t > 0, and/and t/0 are nonnegative and not both identically zero. There is a dimension dependent constant C (N) such that the problem has no solution for c> Ct(N). For c =S Ct(A/) necessary and sufficient conditions are found for / and u0 so that a nonnegative solution exists.
Synthesis method for simulating snow distribution utilizing remotely sensed data for the Tibetan Plateau

Abstract The complex terrain, shallow snowpack, and cloudy conditions of the Tibetan Plateau (TP) can greatly affect the reliability of different remote sensing (RS) data, and available station data are scarce for simulating and validating the snow distribution. Aiming at these problems, we design a synthesis method for simulating the snow distribution in the TP where the snow is patchy and shallow in most regions. Different RS data are assimilated into the SnowModel, using the ensemble Kalman filter method. The station observations are used for the validation of assimilated snow depth. To avoid the scale effect during validation, we design a random sampling comparison method by constructing a subjunctive region near each station. For years 2000 to 2008, the root-mean-square error of the assimilated results are in the range [0.002 m, 0.008 m], and the range of Pearson product-moment correlation coefficients between the in situ observations and the assimilated results are in the range [0.61, 0.87]. The result suggests that the snow depletion curve is the most important parameter for the simulation of the snow distribution in ungauged regions, especially in the TP where the snow is patchy and shallow.
Gas Chromatography Analysis of Discharge Products in N2‐CH4 Gas Mixture at Atmospheric Pressure: Study of Mimic Titan's Atmosphere

In this paper, we report presence of various organic products formed in a flowing atmospheric glow discharge fed by gas mixture containing 1‐5 % of methane in nitrogen, which mimics the Titan's atmosphere. Gaseous products from the discharge exhaust were analysed by Gas Chromatography with Mass Spectrometry (GC‐MS). The experimental results revealed C2H2, HCN, and CH3CN as the major products. Various hydrocarbons and nitriles were the other determined gaseous products. Whilst many of these compounds have been predicted and/or observed in the Titan atmosphere, the present plasma experiments provide evidence of both the chemical complexity of Titan atmospheric processes and the mechanisms by which larger species grow prior to form the dust that should cover much of the Titan's surface. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Three-dimensional MHD simulation of the evolution of the April 2000 CME event and its induced shocks using a magnetized plasma blob model

A three-dimensional (3-D) time-dependent, numerical magnetohydrodynamic (MHD) model with asynchronous and parallel time-marching method is used to investigate the propagation of coronal mass ejections (CMEs) in the nonhomogenous background solar wind flow. The background solar wind is constructed based on the self-consistent source surface with observed line-of-sight of magnetic field and density from the source surface of 2.5 R-s to the Earth's orbit (215 Rs) and beyond. The CMEs are simulated by means of a very simple flux rope model: a high-density, high-velocity, and high-temperature magnetized plasma blob is superimposed on a steady state background solar wind with an initial launch direction. The dynamical interaction of a CME with the background solar wind flow between 2.5 and 220 Rs is investigated. The evolution of the physical parameters at the cobpoint, which is located at the shock front region magnetically connected to ACE spacecraft, is also investigated. We have chosen the well-defined halo-CME event of 4-6 April 2000 as a test case. In this validation study we find that this 3-D MHD model, with the asynchronous and parallel time-marching method, the self-consistent source surface as initial boundary conditions, and the simple flux rope as CME model, provide a relatively satisfactory comparison with the ACE spacecraft observations at the L1 point.
Walsh-fourier series and the concept of a derivative †

In the theory of Walsh-Fourier series on the dyadic group G developed so far, such essential concepts as continuity, Lipschitz conditions modulus of continuity ,etc., have been employed. However, with the exception of several articles by J. E. Gibbs, no attempt has been made to define a derivative for functions f given on G. In this paper such a derivative D [1] f is defined which has most properties in common with the ordinary derivative. D [1] is a linear, closed operator, the inverse operator or integral is defined, the fundamental theorem of the calculus is valid for these two notions, The derivative enables one to estimate the order of magnitude of the Walsh-Fourier coefficients, the degree of approximation of f by the partial sums of the Walsh-Fourier series of f, etc. Moreover the Walsh functions are the non-trivial eigensolutions of a first-order linear differential equation. The proofs depend upon a Walsh-Fourier "coefficient method".