Miracle-dz/UniFAR-FTUs huggingface dataset:
MORPHOLOGICAL EVOLUTION OF A THREE-DIMENSIONAL CORONAL MASS EJECTION CLOUD RECONSTRUCTED FROM THREE VIEWPOINTS

The propagation properties of coronal mass ejections (CMEs) are crucial to predict its geomagnetic effect. A newly developed three-dimensional (3D) mask fitting reconstruction method using coronagraph images from three viewpoints has been described and applied to the CME ejected on 2010 August 7. The CME's 3D localization, real shape, and morphological evolution are presented. Due to its interaction with the ambient solar wind, the morphology of this CME changed significantly in the early phase of evolution. Two hours after its initiation, it was expanding almost self-similarly. The CME's 3D localization is quite helpful to link remote sensing observations to in situ measurements. The investigated CME was propagating to Venus with its flank just touching STEREO B. Its corresponding interplanetary CME in the interplanetary space shows a possible signature of a magnetic cloud with a preceding shock in Venus Express (VEX) observations, while from STEREO B only a shock is observed. We have calculated three principal axes for the reconstructed 3D CME cloud. The orientation of the major axis is, in general, consistent with the orientation of a filament (polarity inversion line) observed by SDO/AIA and SDO/HMI. The flux rope axis derived by the Minimal Variance Analysis from VEX indicates a radial-directed axis orientation. It might be that locally only the leg of the flux rope passed through VEX. The height and speed profiles from the Sun to Venus are obtained. We find that the CME speed possibly had been adjusted to the speed of the ambient solar wind flow after leaving the COR2 field of view and before arriving at Venus. A southward deflection of the CME from the source region is found from the trajectory of the CME geometric center. We attribute it to the influence of the coronal hole where the fast solar wind emanated from.
Inner functions in polydiscs

exist for almost all z in the distinguished boundary T of U. Here rz=(rzh • • • , rzN). An inner function in U is, by definition, a function gŒH^ÇU*) such that |g*(s)| = 1 for almost all zET. The present note contains partial answers to questions such as the following: Is every fE:HTM(U) (other than / ^ 0 ) a product ƒ—g& where g is inner and both h and 1/h are holomorphic in U? (In this case we say that ƒ and g have the same zeros in U.) If not, what are some sufficient conditions on ƒ which guarantee the existence of such a factorization? If ƒ does have the same zeros as some inner function g, does it follow that g can be chosen so that f/gCzH°°(U)? A special role is played by those inner functions which (for lack of a better name) I propose to call good: An inner function g is good if
Measuring Skewness with Respect to the Mode

Abstract There are several measures employed to quantify the degree of skewness of a distribution. These have been based on the expectations or medians of the distributions considered. In 1964, van Zwet showed that all the standardized odd central moments of order 3 or higher maintained the convex or c-ordering of distributions that he introduced. This ordering has been widely accepted as appropriate for ordering two distributions in relation to skewness. More recently, measures based on the medians have been shown to honor the convex ordering. The measure of skewness (μ – M) / [sgrave] where μ, [sgrave], and M are, respectively, the expectation, standard deviation, and mode of the distribution was initially proposed by Karl Pearson. It unfortunately does not maintain the convex ordering. Here we introduce a measure based on the mode of a distribution that maintains the c-ordering. For many classes of right-skewed distributions, it is easily computed as a function of the shape parameter of the family and .
Self-diffusion of Brownian particles in concentrated suspensions under shear

The self-diffusivity of Brownian hard spheres in a simple shear flow is studied by numerical simulation. Particle trajectories are calculated by Stokesian dynamics, with an accurate representation of the suspension hydrodynamics that includes both many-body interactions and lubrication. The simulations are of a monolayer of identical spheres as a function of the Peclet number: Pe =gamma-dot a^2/D0, which measures the relative importance of shear and Brownian forces. Here gamma-dot is the shear rate, a the particle radius, and D0 the diffusion coefficient of a single sphere at infinite dilution. In the absence of shear, using only hydrodynamic interactions, the simulations reproduce the pair-distribution function of the equivalent hard-disk system. Both short- and long-time self-diffusivities are determined as a function of the Peclet number. The results show a clear transition from a Brownian motion dominated regime (Pe 10) with a dramatic change in the behavior of the long-time self-diffusivity.
Fundamental Properties of Elliptical Galaxies

The global properties of elliptical galaxies, such as luminosity, radius, projected velocity dispersion, projected luminosity, etc., form a two-dimensional family. This 'fundamental plane' of elliptical galaxies can be defined in observable terms by the velocity dispersion and mean surface brightness. Its thickness is given by the present measurement error bars, and there are no significant indications of nonlinearity or higher dimensionality. This is indicative of a strong regularity in the process of galaxy formation. The equations of the plane can be used as new, substantially improved distance indicators for elliptical galaxies. However, all morphological parameters which describe the shape of the light distribution (ellipticity, elippticity gradient, isophotal twist rate, slope of the surface brightness profile) and reflect dynamical anisotropies of stars are completely independent of this fundamental plane. Thus, the elliptical galaxies are actually a '2 + N' parameter family. The M/L ratios correlate only with the velocity dispersions and show a small intrinsic scatter, perhaps only about 30 percent, in a luminosity range spanning some four orders of magnitude; this suggests a constant fraction of the dark matter contribution in elliptical galaxies. 33 references.
New model atmospheres for very cool white dwarfs with mixed H/He and pure He compositions

New model atmosphere calculations for very cool white dwarfs with mixed H/He and pure He compositions are presented. The hydrogen-rich models incorporate improved cross section calculations of the collision-induced absorption by molecular hydrogen due to collisions with H2, H, and He. The effects associated with variations in the effective temperature (T(sub eff) greater than or equal to 4000 and less than or equal to 10,000 K), the surface gravity (log g greater than or equal to 7.5 and less than or equal to 9.5), and the chemical composition (N(He)/N(H) greater than or equal to O and less than or equal to 100) are investigated. Results from earlier calculations are confirmed qualitatively, but a more detailed comparison reveals large quantitative deviations. Cool white dwarfs with mixed H/He chemical compositions are shown to be easily recognizable from their predicted strong infrared flux deficiency. Pure helium model calculations are described as well. These include a modified version of the recently developed equation of state of D. Saumon and G. Chabrier. Nonideal effects brought about by various equations of state are explored in detail. For the purpose of this analysis, a model of pressure ionization based on an accurate description of the interactions in a mostly atomic helium fluid is developed. The effects of pressure ionization are shown to be the most important issue in the model calculations. A critical discussion of previous generations of pure helium model calculations is presented. Finally, broadband color indices are provided for the complete model grid.
An analytic expression for the luminosity function for galaxies

A new analytic approximation for the luminosity function for galaxies is proposed, which shows good agreement with both a luminosity distribution for bright nearby galaxies and a composite luminosity distribution for cluster galaxies. The analytic expression is proportional to L/sup -5///sup 4/e/sup -//sup L*/, where L* is a characteristic luminosity corresponding to a characteristic absolute magnitude M*/sub B0//sub -//sub 2//sub 0//sub . 6/For an individual cluster, the characteristic magnitude may be determined with an accuracy of approx.0. 25 mag, suggesting its use as a standard candle. The analytic expression is used to compute an expected richness-absolute magnitude correlation for first ranked cluster galaxies and an expected dispersion, which are compared with the data of Sandage and Hardy. (AIP)
Suzaku observations of two ultraluminous X-ray sources in the nearby spiral galaxy IC 342

We report a result of our Suzaku observations for two ultraluminous X-ray sources (ULX; X-1 and X-2) in IC 342 on 2010 August and 2011 March. We found a hint of hard X-ray photons (14-20 keV), and fitted the XIS and the PIN spectra simultaneously. As a result, the joint spectra can be explained by the power-law model for X-1 and the multi-color disk model for X-2. We briefly discuss the spectral states of the two ULXs comparing with those of Galactic black hole binaries.
PLUG‐IN ESTIMATION OF GENERAL LEVEL SETS

Given an unknown function (e.g. a probability density, a regression function, …) f and a constant c, the problem of estimating the level set L(c) ={f≥c} is considered. This problem is tackled in a very general framework, which allows f to be defined on a metric space different from . Such a degree of generality is motivated by practical considerations and, in fact, an example with astronomical data is analyzed where the domain of f is the unit sphere. A plug‐in approach is followed; that is, L(c) is estimated by Ln(c) ={fn≥c}, where fn is an estimator of f. Two results are obtained concerning consistency and convergence rates, with respect to the Hausdorff metric, of the boundaries ∂Ln(c) towards ∂L(c). Also, the consistency of Ln(c) to L(c) is shown, under mild conditions, with respect to the L1 distance. Special attention is paid to the particular case of spherical data.
Electronic structures of silicene/GaS heterosheets

Although Dirac-like electronic properties are predicted for silicene, recent experiments find substrate-induced complex bucklings would destruct such feature [C. -L. Lin et al., Phys. Rev. Lett. 110, 076801 (2013)]. Here, using first-principles calculations, we propose that the recently synthesized gallium sulfide (GaS) nanosheet could be an appropriate substrate for silicene, which can form commensurate Si/GaS heterosheets akin to graphene/BN systems. More importantly, in these heterosheets, the characteristic Dirac-like band feature of linear dispersions is retained, and due to the intrinsic electric field, a sizable band gap is opened at the Dirac point, which could be further tuned by bias voltage or strains.
Almost everywhere summability on nilmanifolds

Let G be a stratified, nilpotent Lie group and let L be a homogeneous sublaplacian on G. Let E(X) denote the spectral resolution of L on L2(G). Given a function K on R+ , define the operator TK on L2(G) by Tkf= j$> K(\) dE(\)f. Sufficient conditions on K to imply that TK is bounded on L\G) and the maximal operator K*(p(x) = supr>01 TKq>(x) | (where K,(X) = K(tXJ) is of weak type (1,1) are given. Picking a basis e0, e,,. of L2(G/T) (T being a discrete cocompact subgroup of G) consisting of eigenfunctions of L, we obtain almost everywhere and norm convergence of various summability methods of 2(qp, ef)e¡, <p E LP(G/T), 1 <p < oo.
Residual Potential and Approximate Methods for Three‐Dimensional Fluid‐Structure Interaction Problems

A method developed previously for an analysis of the two‐dimensional excitation of an elastic cylindrical shell by a transverse, transient acoustic wave is extended to three‐dimensional applicability. In addition, some fluid‐structure interaction approximations are presented that follow naturally from the rigorous development. Application to finite element analysis of the transient response of submerged structures is discussed.
On some characteristics of bivariate chi-square distribution

Product moments of bivariate chi-square distribution have been derived in closed forms. Finite expressions have been derived for product moments of integer orders. Marginal and conditional distributions, conditional moments, coefficient of skewness and kurtosis of conditional distribution have also been discussed. Shannon entropy of the distribution is also derived. We also discuss the Bayesian estimation of a parameter of the distribution. Results match with the independent case when the variables are uncorrelated.
Geometry of the tensor product of C*-algebras

When and ℬ are C*-algebras their algebraic tensor product ⊗ ℬ is a *-algebra in a natural way. Until recently, work on tensor products of C*-algebras has concentrated on norms α which make the completion ⊗α ℬ into a C*-algebra. The crucial role played by the Haagerup norm in the theory of operator spaces and completely bounded maps has produced some interest in more general norms (see [8; 12]). In this paper we investigate geometrical properties of algebra norms on ⊗ ℬ. By an ‘algebra norm’ we mean a norm which is sub-multiplicative: α(u.v) ≤ ≤ α(u). α(v).
Optical Measurements of Neutral Cesium Mass Flow Rate in Field Emission Thrusters

A = integral of the relative density profile, au A21 = Einstein coefficient for spontaneous emission, s 1 B21 = Einstein coefficient for stimulated absorption, s 1 C1 = calibration coefficient for the first moment I , m 3 s C2 = calibration coefficient for the second moment I , au c = speed of light, ms 1 dS = elementary surface element, m F = normalized velocity distribution function, m 3 s f = normalized projected velocity distribution function, m 1 s I = laser intensity, Wm 2 Ia = accelerator current, A Ie = emitter current, A ISat = saturation intensity, Wm 2 I = first moment of the fluorescence signal, s 2 I = second moment of the fluorescence signal, s 3 J = first moment of the transmission, s 1 K = cesium number density integrated along the absorption line of sight, m 2 kT = proportionality constant for thrust-dependent mass flow rate, mgh 1 N 1 LRef = length of the reference cell, m mCs = cesium atom mass, kg nCs = cesium number density, m 3 nRef = cesium number density in the reference cell, m 3 q = cesium mass flow rate, mgh 1 Q = quenching rate, s 1 S = fluorescence signal detected, count s 1 T = transmission coefficient u = microscopic velocity, ms 1 U = averaged velocity along a laser axis, ms 1 V = probed volume, m V = averaged velocity vector in the laboratory coordinate system, ms 1 Va = accelerator voltage, V Ve = emitter voltage, V V ij = averaged velocity along the Z axis, measured at node i; j , ms 1 Y = normalized line-shape function, s = deexcitation rate, s 1 0 = transition wavelength, m = frequency, MHz L = laser frequency, MHz = solid angle, sr
Dynamical Systems and Evolution Equations: Theory and Applications

I. Evolution Equations on ? n. - 1. The Space ? n. - 2. Evolution Equations on ? n. - 3. Finite Escape Times. - 4. Processes on ? sun X ? - 5. Linear Dynamical Systems. - 6. The Simplest Class of Processes. - 7. Stability of a Particular Motion: Processes. - 8. Stability of Equilibrium: Dynamical Systems. - 9. Stability of Equilibrium: Linear Dynamical Systems. - 10. Quadratic Liapunov Functions and Linearization. - 11. The Invariance Principle and Asymptotic Behavior. - 12. Comments and Extensions. - References. - II. Preliminaries for Abstract Evolution Equations. - 1. Abstract Spaces. - 2. Functions. - 3. Linear Functions. - 4. Differentiation of Functions. - 5. Abstract Evolution Equations. - References. - III. Abstract Dynamical Systems and Evolution Equations. - 1. Dynamical Systems and C0-Semigroups. - 2. Linear Dynamical Systems. - 3. Generation of Linear Dynamical Systems. - 4. Choosing the State Space in Applications. - 5. Generation of Nonlinear Dynamical Systems. - 6. Comments and Extensions. - References. - IV. Some Topological Dynamics. - 1. Liapunov Functions and Positive Invariance. - 2. Computation of V. - 3. Stability and Liapunov's Direct Method. - 4. Positive Limit Sets and the Invariance Principle. - 5. Orbital Precompactness and Use of the Invariance Principle. - 6. Comments and Extensions. - References. - V. Applications and Special Topics. - 1. A Feedback Control Problem. - 2. The Thermoelastic Stability Problem. - 3. The Viscoelastic Stability Problem. - 4. A Fission Reactor Stability Problem. - 5. A Supersonic Panel-Flutter Problem. - 6. Discrete Dynamical Systems. - 7. Finite-Dimensional Approximation. - References.
Electrical and optical properties of p-type InGaN

Mg-doped InxGa1−xN alloys were grown by metal organic chemical vapor deposition on semi-insulating c-GaN/sapphire templates. Hall effect measurements showed that Mg-doped InxGa1−xN epilayers are p-type for x up to 0.35. Mg-acceptor levels (EA) as a function of x, (x up to 0.35), were experimentally evaluated from the temperature dependent hole concentration. The observed EA in Mg-doped In0.35Ga0. 65N alloys was about 43 meV, which is roughly four times smaller than that in Mg doped GaN. A room temperature resistivity as low as 0.4 Ω cm (with a hole concentration ∼5×1018 cm−3 and hole mobility ∼3 cm2/V s) was obtained in Mg-doped In0.22Ga0. 78N. It was observed that the photoluminescence (PL) intensity associated with the Mg related emission line decreases exponentially with x. The Mg energy levels in InGaN alloys obtained from PL measurements are consistent with those obtained from Hall-effect measurements.
Demarcating prosodic groups with articulation

It is hypothesized that phrasal position affects articulation, and that what looks like overall declination of articulatory displacement could arise from local enhancements or reductions at particular phrasal positions. To test this hypothesis, linguopalatal contact was measured for both the consonant /n/ and the vowel /o/ in reiterant speech. Utterances were based on arithmetic statements like ‘‘(1+1)×(1+1)’’ [reiterant ‘‘(no no no) no (no no no)’’], where stress and phrasing were varied by choice of numerals and location of parentheses. For the one speaker analyzed, there was no overall downtrend in contact of /n/ through any sentence type when all syllables—stressed, word‐initial, or phrase‐initial—were compared. Instead, word‐, phrase‐, and sentence‐initial /n/’s have cumulatively more contact than medial and final ones. It is proposed that greater initial contact contributes to marking prosodic boundaries by enhancing the consonant–vowel contrast. Also enhancing the CV contrast is the more open posit.
High-energy component of GRB 941017 revisited and the reverse-shock synchrotron self-Compton emission

The different temporal behaviors of the high energy component and the hundreds of keV emission from GRB 941017 suggest that they come from different emission regions. The nearly constant flux of this high energy component is consistent with being produced in the region of the early external shock formed when the ejecta hit the surrounding medium. Here we show that the relatively hard spectrum of this component can be numerically modelled as the synchrotron self-Compton emission from external reverse shock when the ejecta is decelerated by a typical interstellar medium. Constraints on the parameters of the fireball, such as the initial Lorentz factor. , the burst energy, and the magnetic field equipartition fraction are obtained. Very high initial Lorentz factor (n greater than or similar to 10(3)) inferred for this burst may explain the rarity of this kind of high-energy component in gamma-ray bursts (GRBs). Large GeV - TeV flux from the reverse shock is predicted for GRBs with high initial Lorentz factors.
Stellar Population Synthesis Revisited

The isochrone synthesis method is introduced as a population synthesis method for galaxies. The method permits accurate distributions of stars in the theoretical color-magnitude diagram to be computed for any stellar population and thereby circumvent the problems faced by earlier techniques. A set of evolutionary tracks extending from the ZAMS up to the beginning of the white-dwarf cooling sequence is compiled to optimize the models. Comparison of model predictions with observational data leads to the conclusion that the isochrone synthesis can reproduce the observed colors of stellar populations of ages from a few tens of millions of yr to a Hubble time. 78 refs.
Macroscopic aspects of attosecond pulse generation

Attosecond pulses are generated by a macroscopic number of ionizing atoms interacting with a focused laser pulse, via the process of high harmonic generation. The physics of their generation consists of an interplay between the microscopic laser–atom interaction and macroscopic effects due to ionization and phase matching in the nonlinear medium. In this review, we focus on a complete understanding of the way in which attosecond pulses arrive at a target where they can be characterized and used in an experiment. We discuss a number of results from calculations of attosecond pulse generation obtained by simultaneous solution of the time-dependent Schrödinger equation and the Maxwell wave equation. These results, which allow for a clean separation of microscopic and macroscopic factors, illustrate how macroscopic effects are used to select attosecond pulses from the radiation that is emitted by atoms interacting with a strong laser field.
Periodic electric-field domains in optically excited multiple-quantum-well structures

We demonstrate using an ensemble Monte Carlo particle modeling that periodic electric-field domains can arise in optically excited multiple quantum well structures under applied voltage. In particular, the formation of the electric-field distributions with the period equal to twice the structure period is possible. This effect is attributed to the excitation of the recharging waves due to decreasing energy dependence of the capture rate of hot electron capture into quantum wells and nonlocal heating of electrons by electric field.
UNSTEADY SIMULATION OF TURBULENT FLOW AND HEAT TRANSFER IN A CHANNEL WITH PERIODIC ARRAY OF CUBIC PIN‐FINS

An unsteady three-dimensional numerical study is performed to explore flow and heat transfer in a periodic array of cubic pin‐fins housed inside a channel. The pin‐fins are arranged in an in-line pattern with both streamwise and transverse periodicity set to 2.5 times the pin-fin dimension. Calculations are done in the turbulent flow regime for Reynolds numbers in the range of 7,090–13,280. The unsteady Reynolds-averaged Navier–Stokes (URANS) and energy equations are solved using higher-order temporal and spatial discretization schemes. An unsteady k – ϵ turbulence model is employed to model the unresolved turbulence fluctuations. Large eddy simulations (LES) are also performed for a Reynolds number of 7,090 for validation purposes. The URANS results are able to resolve the discrete large-scale spatial and temporal fluctuations in the flow, and the time-averaged predictions with URANS match the LES results very well. The large-scale fluctuations in the flow appear primarily in the region between the cubic fins, but are linked to low-amplitude oscillations in the outer flow.Three thermal boundary conditions are studied: (1) only channel wall heated (2) only pin‐fins heated, and (3) both channel wall and pin‐fins heated. The overall heat transfer enhancement is about 1.8–2.0 times the heat transfer from a smooth duct flow. The heat transfer from pin‐fins is found to be 5–9% higher than that from the top wall at low Reynolds numbers (7,090 and 8,900), while it is of comparable magnitude at higher Reynolds number (13,280).