Miracle-dz/UniFAR-FTUs huggingface dataset:
A HIGH ORDER KINETIC FLUX-SPLITTING METHOD FOR THE SPECIAL RELATIVISTIC HYDRODYNAMICS

In this article we present a flux splitting method based on gas-kinetic theory for the special relativistic hydrodynamics (SRHD) [Landau and Lifshitz, Fluid Mechanics, Pergamon New York, 1987] in one and two space dimensions. This kinetic method is based on the direct splitting of the macroscopic flux functions with the consideration of particle transport. At the same time, particle "collisions" are implemented in the free transport process to reduce numerical dissipation. Due to the nonlinear relations between conservative and primitive variables and the consequent complexity of the Jacobian matrix, the multi-dimensional shock-capturing numerical schemes for SRHD are computationally more expensive. All the previous methods presented for the solution of these equations were based on the macroscopic continuum description. These upwind high-resolution shock-capturing (HRSC) schemes, which were originally made for non-relativistic flows, were extended to SRHD. However our method, which is based on kinetic theory is more related to the physics of these equations and is very efficient, robust, and easy to implement. In order to get high order accuracy in space, we use a third order central weighted essentially non-oscillatory (CWENO) finite difference interpolation routine. To achieve high order accuracy in time we use a Runge-Kutta time stepping method. The one- and two-dimensional computations reported in this paper show the desired accuracy, high resolution, and robustness of the method.
Integrated marked Poisson processes with application to image correlation spectroscopy

Image correlation spectroscopy (ICS) is an experimental technique used in the study of cell tissue, specifically to obtain information about protein aggregates. This paper discusses a filtered Poisson process model of ICS, and uses this to obtain the sampling distribution of an estimator of interest, using spectral methods. Integrals of third‐ and fourth‐order spectra are involved, and methods proposed in the literature are studied numerically. They are found to be infeasible methods, requiring months of computing time. An alternative method is proposed and is illustrated on some actual ICS experiments. A novel feature in this study is the use of a SIMD‐class parallel computer, a MasPar MP‐2 machine, to obtain some statistical properties of the estimation method.
Accretion onto Hot White Dwarfs in Relation to Symbiotic Novae

Numerical calculations are used to study the hydrodynamic evolution of a hot white dwarf with 1 solar mass accreting hydrogen-rich matter at rates between 10 to the -8th and 10 to the -6th solar masses/yr. It is found that for accretion at a rate of about 10 to the -8th solar masses/yr, nova-type outbursts of long duration occur at intervals of about 1500 yr. About half of the accreted envelope is ejected during these outbursts. At a rate of about 10 to the -7th solar masses/yr, the star alternates between comparable periods at a high plateau luminosity and giant dimensions and periods at a low luminosity and white dwarf dimension. At 10 to the -6th solar masses/yr, equilibrium is achieved with a typical red giant luminosity supported by steady hydrogen burning. It is concluded that symbiotic novae are more likely to occur in detached systems involving wind accretors. Thus, the contribution of symbiotic stars to the frequency of type I supernovae is severely constrained. 39 refs.
Theory and Observations of Classical Novae

This review is mainly concerned with the physical nature and eruptive behavior of the classical nova outburst. Whether or not an eruptive variable can be considered a classical nova is most easily determined by both the optical light curve and spectral developments during the outburst. For the purposes of this review a star is defined as a classical nova if: 1. the optical brightness increases by > 9 mag in less than a few days; 2. significant brightness changes occur on a time scale of 10 00 days or less; 3. its spectral development can be classified in terms of the character­ istic nova stages [see the synthetic spectra by McLaughlin reproduced on pp. 135-36 in Hynek (1 951) or by Hack & Struve (1 970), pp. 16 8-69J; and 4. the spectra imply that matter is ejected with velocities greater than 100 km sec -1 and less than 5000 km sec -1. For more detailed discussion of empirical membership criteria, the reader is ref erred to Chapters 1 and
Isochrones for late-type stars

Abstract A brief summary of the history of stellar evolution theory and the use of isochrones is given. The present state of the subject is summarized. The major uncertainties in isochrone construction are considered: chemical abundances and color calibrations, and the treatment of turbulent convection in stellar interior and atmosphere models. The treatment of convection affects the modeling of stellar interiors principally in two ways: convective core overshoot which increases evolutionary lifetimes, and the depth of convection zones which determines theoretical radii. Turbulence also modifies atmospheric structure and dynamics, and the derivation of stellar abundances. The symbiosis of seismic techniques with increasingly more realistic three-dimensional radiation hydrodynamics simulations is transforming the study of late-type stars. The important case of very low mass stars, which are fully convective, is briefly visited.
Relationship between superfluid density at zero temperature and Tc of Bi2Sr2−xLaxCuO6+δ (0.4 ⩽ x ⩽ 0.76) and Bi2Sr1.6La0.4Cu1−yZnyO6+δ (0.0 ⩽ y ⩽ 0.015)

We have studied the relationship between superfluid density at zero temperature, ρs(0), and superconducting transition temperature, Tc, for the underdoped Bi2Sr2- xLaxCuO6+δ and nearly optimally doped Bi2Sr1.6La0. 4Cu1- yZnyO6+δ, using isothermal reversible magnetization. In our study, we found that ρs(0) in Bi2Sr2- xLaxCuO6+δ and Bi2Sr1.6La0. 4Cu1-yZnyO6+δ is proportional to Tc2, which is nearly in agreement with the relation suggested from the quantum criticality.
Sensitivity of Orographic Precipitation to Changing Ambient Conditions and Terrain Geometries: An Idealized Modeling Perspective

Abstract This paper utilizes the fifth-generation Pennsylvania State University–National Center for Atmospheric Research (PSU–NCAR) mesoscale model (MM5) in a two-dimensional (2D) configuration at 4-km horizontal grid spacing in order to better understand the relationship between orographic precipitation and the height and width of a barrier, as well as the ambient flow, uniform moist static stability, and freezing level. The focus is on how these parameters affect the orographic precipitation by changing the circulation and microphysical structures over the barrier. As the low-level flow becomes blocked for moist nondimensional mountain heights greater than 3.0, there is a rapid upstream shift in the precipitation maximum and a reduction in precipitation over the upper windward slope. For the terrain geometries used in this study (500 to 3500 m high and 25- to 50-km half-width), the maximum precipitation is a strong function of barrier slope for relatively weak upstream flow (U = 10 m s−1). For moderate .
The Classification and Orbital Period of WD 2154+408: A New Short‐Period Post–Common‐Envelope Binary

We present orbit‐sampled photometry of the binary system WD 2154+408. The photometric study reveals a period of P = 0.26772 day, which is taken to be the orbital period of the binary. No evidence is seen for either an accretion disk or mass transfer, leading to the conclusion that WD 2154+408 is not a contact or semidetached system but has detached components with a visible irradiation effect. The short orbital period also leads to the conclusion that the system passed through a common‐envelope phase at some time in the past. A single spectrum is shown exhibiting both narrow emission and broad absorption components of the Hβ line. This and the photometric variations are consistent with the system being a post–common‐envelope binary consisting of a hot white dwarf primary and a cool irradiated companion.
Numerical Renormalization Group Studies on Single Impurity Anderson Model in Superconductivity: A Unified Treatment of Magnetic, Nonmagnetic Impurities, and Resonance Scattering

We investigate a single impurity Anderson model in superconducting state focusing on the localized excited states induced around the impurity site with use of the numerical renormalization group method. Using this model, we present a unified treatment of electronic states around various kinds of impurities embedded in conventional s -wave superconductivity that have been investigated independently so far: (1) magnetic impurity, (2) nonmagnetic impurity with potential scattering, and (3) nonmagnetic impurity with resonance scattering. In the case of the symmetric Anderson model, we clarify how the localized excited state induced around (1) is transformed into the one induced around (3) with a decrease of the strength of the on-site Coulomb repulsion at the impurity site. On the other hand, in the case of the asymmetric Anderson model, we show how the bound state induced by the magnetic impurity disappears when the impurity is gradually transformed from (1) into (2) with an increase of the energy of the imp.
An Application of Adaptive Logic to Meteorological Prediction

Abstract Two adaptive logic models and a training algorithm for each are described. These models are tested on a meteorological prediction problem with the use of large developmental and test data samples. Discriminant analysis is used for comparison. It is found that ceiling heights at Washington National Airport could be forecast better with the discriminant analysis technique than with the adaptive logic models.
A new star pattern identification technique using an improved triangle algorithm

Triangle identification algorithm has been widely applied in star pattern identification of star sensor. However, its lower characteristic dimensions lead to matching redundancy and identification errors. To improve the identification accuracy, the identification process of the triangle identification algorithm is improved. First, the method of “quasi uniform distribution” of space solid angles is proposed. That is, based on the size of space solid angle a certain zone at the celestial equator corresponds to, the whole celestial sphere is partitioned into a number of sub-blocks. Then, guide stars are selected uniformly according to sub-blocks, obtaining a guide star catalogue with fewer stars, better distribution uniformity and higher completeness. Finally, an approach is proposed to further optimize primarily selected observation triangle groups for the second time for matching identification. The constraint relationship between the sides and included angles of the observation triangle is converted onto the image plane. The simulation experiment result shows that the star pattern identification technique based on the improved triangle algorithm has strong anti-interference performance against star point position noises, magnitude (brightness) noises and “missing stars” and it is superior to traditional algorithms in identification rate.
Observation of the charged defect migration that causes the degradation of double-Schottky barriers using a nondestructive quantitative profiling technique

The migration and neutralization of charged defect ions during the degradation of a double-Schottky barrier are observed by performing nondestructive pulsed electroacoustic measurements on ZnO bicrystals. This offers the possibility to experimentally access the predicted defect migration behavior and provides a solid foundation to validate the theoretical aging model for electroceramics. Theoretical modeling of the acoustic attenuation effects during measurements is also discussed to understand and validate the experimental results, gaining insight into the widely used acoustic technique.
The optical study of nanoporous C-Pd thin films

In this paper, the preliminary results for thin carbon-palladium (C-Pd) nanocomposites obtained by PVD/CVD method, carried out using optical methods are presented. Raman studies reveal the dominance of graphite-like structures. The optical transmittance measurement shows an exceptionally low value of the effective extinction coefficient when compared to amorphous graphite. The carbon structure porosity impact on the transmission properties of the studied layers is discussed.
SOLIS: an innovative suite of synoptic instruments

SOLIS (Synoptic Optical Long-term Investigations of the Sun) is a suite of three innovative instruments under construction that will greatly improve ground-based synoptic solar observations. The Vector Spectromagnetograph (VSM) is a compact, high-throughput vector-polarimeter with an active secondary mirror, an actively controlled grating spectrograph, and two high-speed cameras with silicon-on-CMOS-multiplexer hybrid focal plane arrays. It will measure the magnetic field strength and direction over the full solar disk within 15 minutes. The Full-Disk Patrol (FDP) takes full-disk solar intensity and Doppler images in various spectral lines and in the continuum at a high cadence through liquid-crystal tuned birefringent filters. The Integrated Sunlight Spectrometer (ISS) uses a fiber-fed spectrograph to measure minute changes of the Sun-as-a-star in many spectral lines. A high degree of automation and remote control provides fast user access to data and flexible interaction with the data-collection process. SOLIS is currently in the final assembly phase and will become operational early in 2003.
Straight interference fringes thinning algorithm

The straight interference fringes are very common in the optical measurement such as Michelson interferometer, interference of wedge, the diffraction of single slit, double slits, grating diffraction, the diffraction of thin straight line, speckle correlation technique, moiré topography. etc. With the rapid development of CCD and computer technology, the interference fringes are treated with efficient and fast image processing technique. Usually every interference fringe has certain width and is of low contrast, and even there are gaps or holes in the fringes, the central position is difficult to be located, therefore, the study of fringes thinning algorithm is an interesting subject. Many different algorithms have been presented, every algorithm has its own shortcomings, such as complication of the algorithm, there are spurs or discontinues on the final fringes, or unable to treat the low signal to noise ratio fringes. In this paper a robust and simple algorithm has presented, which mainly including morphological image processing and unusually implement of 1×N median filter to strengthen the horizontal fringes(supposing the fringes are in horizontal direction), to remove spurs and to fill the gaps in the fringes. The experiment result confirmed the validation and robust of the algorithm. Even though the image to be treated is of low signal to noise ratio and low contrast, smooth and continue straight fringes free of spurs could be obtained.
OFDM spectral characterization: estimation of the bandwidth and the number of sub-carriers

This paper deals with the analysis of modulated signals in a NDA (non data aided) context. Assuming the detection of an OFDM signal, our goal is to estimate the bandwidth and the number of sub-carriers of this signal. First, we propose an algorithm based on wavelet decomposition in order to estimate the bandwidth: bandwidth is correctly estimated in 100% of the cases with an error lower than 8% until the SNR = 3 dB. Second, we apply the MUSIC algorithm with decision criterion to obtain the number of sub-carriers: the number of carriers can be estimated with an error lower or equal to 9% in 100% of the cases until the SNR = 10 dB.
Palladium nanoparticle decorated silicon nanowire field-effect transistor with side-gates for hydrogen gas detection

A silicon nanowire field-effect transistor (SiNW FET) with local side-gates and Pd surface decoration is demonstrated for hydrogen (H2) detection. The SiNW FETs are fabricated by top-down method and functionalized with palladium nanoparticles (PdNPs) through electron beam evaporation for H2 detection. The drain current of the PdNP-decorated device reversibly responds to H2 at different concentrations. The local side-gates allow individual addressing of each sensor and enhance the sensitivity by adjusting the working region to the subthreshold regime. A control experiment using a non-functionalized device verifies that the hydrogen-sensitivity is originated from the PdNPs functionalized on the SiNW surface.
Combining Correlation Matrices: Simulation Analysis of Improved Fixed-Effects Methods

The originally proposed multivariate meta-analysis approach for correlation matrices—analyze Pearson correlations, with each study’s observed correlations replacing their population counterparts in its conditional-covariance matrix—performs poorly. Two refinements are considered: Analyze Fisher Z-transformed correlations, and substitute better estimates of correlations in the conditional covariances. Fixed-effects methods with and without each refinement were examined in a Monte Carlo study; number of studies and the distribution of within-study sample sizes were varied. Both refinements improved element-wise point and interval estimates, as well as Type I error control for homogeneity tests, especially with many small studies. Practical recommendations and suggestions for future methodological work are offered. An appendix describes how to transform Fisher-Z (co)variances to the Pearson-r metric.
Chaotic streamlines in the ABC flows

The particle paths of the Arnold-Beltrami-Childress (ABC) flows \[ u = (A \sin z+ C \cos y, B \sin x + A \cos z, C \sin y + B \cos x). \] are investigated both analytically and numerically. This three-parameter family of spatially periodic flows provides a simple steady-state solution of Euler's equations. Nevertheless, the streamlines have a complicated Lagrangian structure which is studied here with dynamical systems tools. In general, there is a set of closed (on the torus, T3) helical streamlines, each of which is surrounded by a finite region of KAM invariant surfaces. For certain values of the parameters strong resonances occur which disrupt the surfaces. The remaining space is occupied by chaotic particle paths: here stagnation points may occur and, when they do, they are connected by a web of heteroclinic streamlines. When one of the parameters A, B or C vanishes the flow is integrable. In the neighbourhood, perturbation techniques can be used to predict strong resonances. A systematic search for integrable cases is done using Painlevé tests, i.e. studying complex-time singularities of fluid-particle trajectories. When ABC ≠ 0 recursive clustering of complex time singularities occurs that seems characteristic of non-integrable behaviour.
The probability distribution of the partition function of the random energy model

The authors give the expression for both integer and non-integer moments of the partition function Z of the random energy model. In the thermodynamic limit, they find that the probability distribution P(Z) can be decomposed into two parts. For log Z-(log Z) finite, the distribution is independent of N, the size of the system, whereas for log Z-(log Z) positive and of order N, the distribution is Gaussian. These two parts match in the region 1<<log Z-(log Z)<<N where the distribution is exponential.
Steep Slopes and Preferred Breaks in Gamma-Ray Burst Spectra: The Role of Photospheres and Comptonization

The role of a photospheric component and of pair breakdown is examined in the internal shock model of gamma-ray bursts. We discuss some of the mechanisms by which they would produce anomalously steep low-energy slopes, X-ray excesses and preferred energy breaks. Subrelativistic Comptonization should dominate in high comoving luminosity bursts with high baryon load, while synchrotron radiation dominates the power-law component in bursts which have lower comoving luminosity or have moderate to low baryon loads. A photosphere leading to steep low-energy spectral slopes should be prominent in the lowest baryon load cases.
Problems of set-theoretic non-standard analysis

The main results in the area of set-theoretic non-standard analysis (non-standard set and class theories) obtained over the last few years are presented. It is demonstrated how a? universe of a? comparably simple theory (beginning with the usual Zermelo-Fraenkel set theory ZFC) can be extended to a universe of a more complicated non-standard set or class theory. The last section develops the foundations of Boolean-valued analysis as a part of set-theoretic non-standard analysis.
A partition‐of‐unity‐based finite element method for level sets

Level set methods have recently gained much popularity to capture discontinuities, including their possible propagation. Typically, the partial differential equations that arise in level set methods, in particular the Hamilton–Jacobi equation, are solved by finite difference methods. However, finite difference methods are less suited for irregular domains. Moreover, it seems slightly awkward to use finite differences for the capturing of a discontinuity, while in a subsequent stress analysis finite elements are normally used. For this reason, we here present a finite element approach to solving the governing equations of level set methods. After a review of the governing equations, the initialization of the level sets, the discretization on a finite domain, and the stabilization of the resulting finite element method will be discussed. Special attention will be given to the proper treatment of the internal boundary condition, which is achieved by exploiting the partition‐of‐unity property of finite element shape functions. Finally, a quantitative analysis including accuracy analysis is given for a one‐dimensional example and a qualitative example is given for a two‐dimensional case with a curved discontinuity. Copyright © 2008 John Wiley & Sons, Ltd.
Inner source distributions: Theoretical interpretation, implications, and evidence for inner source protons

A new and important source of pickup ions has been recently observed for the first time, the so-called inner source. We examine properties of inner source ions at high heliographic latitudes through analysis of data from the Solar Wind Ion Composition Spectrometer on the Ulysses satellite for a period extending through the year of 1994 while Ulysses achieved its southernmost latitudes. As demonstrated by Gloeckler et al. [this issue], the relative abundances of inner source ions resemble those of the solar wind, which implies that the dominant production mechanism for the inner source ions involves the absorption and reemission of solar wind ions from interplanetary dust grains. A simple transport model is devised that compares favorably to observed distribution functions and provides an important consistency check for the previously mentioned production mechanism. The model comparison also allows for constraints to be placed on the total dust geometric cross section. The observed distribution function of protons reveals a significant contribution from the inner source, but the abundance of inner source protons relative to oxygen falls significantly below the universal abundance. We postulate causes of this low relative abundance. We also find that inner source protons have a sizable pressure and may constitute an important energetic population in the solar wind, particularly near the their source.