Miracle-dz/UniFAR-FTUs huggingface dataset:
Global phase diagram of the high- T c cuprates

The high-${T}_{c}$ cuprates have a complex phase diagram with many competing phases. We propose a bosonic effective quantum Hamiltonian based on the projected $\text{SO}(5)$ model with extended interactions, which can be derived from the microscopic models of the cuprates. The global phase diagram of this model is obtained using mean-field theory and the quantum Monte Carlo simulation, which is possible because of the absence of the minus sign problem. We show that this single quantum model can account for most salient features observed in the high-${T}_{c}$ cuprates, with different families of the cuprates attributed to different traces in the global phase diagram. Experimental consequences are discussed and theoretical predictions are presented.
A dynamic scaling assumption for phase separation

Abstract A review of the dynamics of phase separation is presented, which focuses on the scaling assumption of the problem. Conventional linear and nonlinear theories are briefly reviewed. The problems with these conventional theories, and how the scaling idea can be used to overcome them are discussed. The growth rates of the droplets, domains, or grains are discussed in terms of the scaling assumption, and experimental tests of the scaling assumption for growth laws and scattering intensities are reviewed. To explain singular properties of the structure function and growth rate, which are observed experimentally, a strong correlation among droplets or grains on phase separations is postulated. A nonconventional form of the scattering function and a nonconventional droplet growth rate are explained qualitatively.
Macroscopically distinct quantum-superposition states as a bosonic code for amplitude damping

We show how macroscopically distinct quantum superposition states (Schrodinger cat states) may be used as logical qubit encodings for the correction of spontaneous emission errors. Spontaneous emission causes a bit flip error, which is easily corrected by a standard error correction circuit. The method works arbitrarily well as the distance between the amplitudes of the superposed coherent states increases. [S1050-2947(99)06503-8].
Stepwise Confidence Intervals without Multiplicity Adjustment for Dose—Response and Toxicity Studies

Abstract Not all simultaneous inferences need multiplicity adjustment. If the sequence of individual inferences is predefined, and failure to achieve the desired inference at any step renders subsequent inferences unnecessary, then multiplicity adjustment is not needed. This can be justified using the closed testing principle to test appropriate hypotheses that are nested in sequence, starting with the most restrictive one. But what hypotheses are appropriate may not be obvious in some problems. We give a fundamentally different, confidence set–based justification by partitioning the parameter space naturally and using the principle that exactly one member of the partition contains the true parameter. In dose–response studies designed to show superiority of treatments over a placebo (negative control) or a drug known to be efficacious (active control), the confidence set approach generates methods with meaningful guarantee against incorrect decision, whereas previous applications of the closed testing app.
Modelling of compressibility effects in mixing layers

The ability of Reynolds-averaged Navier–Stokes (RANS) turbulence models to predict self-similar mixing layers is investigated. Low-speed flows are first considered. The influence of the velocity ratio is well captured. But standard models predict a wrong sensitivity of the mixing layer to density differences. A general correction previously derived from the balance in the logarithmic region of the boundary layer, stating that the variables to be dealt with must be combinations of the turbulent kinetic energy per unit mass and the length scale, hardly improves the prediction. A correction accounting for baroclinic effect is derived but its present form is not satisfactory. High-speed flows are then investigated. Analysis of the self-similar equations shows that no information about the speed of sound and hence about compressibility effects is available for the standard model. A revised form of the sonic eddy concept, which yields a smaller length scale than Kim's proposal, is shown to improve predictions.
Temperature and field dependence of microwave losses in manganite powders

We report systematic measurements of the temperature and field dependence of microwave losses in micron-size powders (∼3 μm) of the manganites Nd0.7Sr0. 3MnO3, La0.7Ca0. 3MnO3, La0.8Ba0. 2MnO3, and La1.4Ca1. 6Mn2O7. We fully confirm previous findings of a large increase in zero-field absorption, in La0.7Ba0. 3MnO3 and La0.7Sr0. 3MnO3, accompanying the onset of ferromagnetism and a concomitant colossal low-field magnetoimpedance (up to 80% at 600 Oe at room temperature). An oversimplified set of computations renders plausible support for interpreting these observations as arising from absorption in the spin system. Possible applications of these novel phenomena are also described.
The Las Campanas Distant Cluster Survey: The Catalog

We present an optically selected catalog of 1073 galaxy cluster and group candidates at 0.3 ≲ z ≲ 1. These candidates are drawn from the Las Campanas Distant Clusters Survey (LCDCS), a drift-scan imaging survey of a 130 square degree strip of the southern sky. To construct this catalog we utilize a novel detection process in which clusters are detected as positive surface brightness fluctuations in the background sky. This approach permits us to find clusters with significantly shallower data than other matched-filter methods that are based upon number counts of resolved galaxies. Selection criteria for the survey are fully automated so that this sample constitutes a well-defined, homogeneous sample that can be used to address issues of cluster evolution and cosmology. Estimated redshifts are derived for the entire sample, and an observed correlation between surface brightness and velocity dispersion, σ, is used to estimate the limiting velocity dispersion of the survey as a function of redshift. We find a net surface density of 15.5 candidates per square degree at zest ≥ 0.3, with a false-detection rate of ~30%. At z ~ 0.3 we probe down to the level of poor groups while by z ~ 0.8 we detect only the most massive systems (σ ≳ 1000 km s-1). We also present a supplemental catalog of 112 candidates that fail one or more of the automated selection criteria, but appear from visual inspection to be bona fide clusters.
Electromagnetic response of confined Dirac particles

The eigenstates of a single massless Dirac particle confined in a linear potential are calculated exactly by direct solution of the Dirac equation. The electromagnetic structure functions are calculated from the Dirac wave functions of the ground and excited states of the particle by coupling to its conserved vector current. We obtain the longitudinal and transverse structure functions as a function of y=nu-q, where nu and q are the energy and momentum transferred to the target in its rest frame. At values of q>~2.5 GeV, much larger than the characteristic energy scale ~440 MeV of the confining potential, the response exhibits y scaling, a generalization of Bjorken scaling. We compare the exact structure functions with those obtained from the ground state wave functions in the plane wave impulse approximation. The deviation from the Callan-Gross relation is compared with the parton model prediction.
The Lyman alpha emission of starburst galaxies

Nearby starburst galaxies have consistently shown anomalous Lyα/Hβ ratios. By reanalyzing the published IUE/optical observations, we show that most starbursts present a normal Lyα emission, consistent with case B recombination theory, provided extinction laws appropriate to their metallicities are used. This implies that extinction is more important than multiple resonant scattering effects. The anomalous emission and absorption lines present in a few remaining galaxies are simply explained if they are observed in the postburst phase, between about 10 7 and 10 8 yr after the start of the burst. We use updated stellar population synthesis models to show that anomalous ratios are produced by the aging of stellar populations, since the underlying stellar Lyα line is important in the cooler massive stars
Shock creation and Painleve property of colliding peakons in the Degasperis-Procesi Equation

The Degasperis-Procesi equation (DP) is one of several equations known to model important nonlinear effects such as wave breaking and shock creation. It is, however, a special property of the DP equation that these two effects can be studied in an explicit way with the help of the multipeakon ansatz. In essence this ansatz allows one to model wave breaking as a collision of hypothetical particles (peakons and antipeakons), called henceforth
Mixed Convection and Radiation Heat Transfer in a Horizontal Duct with Variable Wall Temperature

In this research, experiments are performed to study the laminar flow mixed-convection heat transfer with radiation effects for a hydrodynamically fully developed and thermally developing airflow in a horizontal duct. The duct cross section is made of two differentially heated isothermal vertical walls and two adiabatic horizontal walls with aspect ratios 1 and 0.5. The total heat transfer from the hot wall to the cold wall of the duct depends on the mixed convection and also on the surface radiation heat transfer that takes place within the duct. The analysis of experimental data for the Nusselt number from the hot wall of the duct shows that it is important to consider the effects of surface radiation, and to accounted for them, in the design and analysis of flow and heat transfer through ducts. The flow field within the duct is also made visible by a suitable smoke flow visualization method. The heated air moves upward, accumulates near the top wall adjacent to the hot wall of the duct, and gets circulated continuously to the cold wall on the opposite side. The accumulated flow is thermally stable; the stable conditions can reduce the heat transfer enhancement due to the buoyancy force. The results show that flow condition and surface radiation interaction significantly affect the total Nusselt number and the surface temperature variation along the walls.
MULTICOLOR PHOTOMETRY OF THE GALACTIC CLUSTER NGC 1039 (M34).

Multicolor uvby and H-beta photometries have been obtained for 42 stars in the field of the galactic cluster NGC 1039 (M34). Analyses give a mean cluster reddening of E(B-V) = 0.07 m and a distance modulus of 8.2 m corresponds to a distance of 440 pc. The metallicity of NGC 1039 is similar to the Pleiades cluster; its age is intermediate, older than the Pleiades but younger than the Hyades cluster. The properties of its three Ap stars, two additional peculiar stars, membership criteria, and gaps in the UBV color-color relation are discussed
Nonlinear α-Effect in Dynamo Theory

The standard two-scale theory of the dynamo coefficient α in incompressible isotropic helical MHD turbulence is extended to include nonlinear effects of B̄, the large-scale magnetic field. We express α in terms of statistical quantities that can be calculated from numerical simulations of the case B̄=0. For large magnetic Reynolds numbers, our formula agrees approximately with that of Kraichnan but disagrees with that of Cattaneo & Hughes.
Discrete product systems with twisted units

The spectral C*-algebra of the discrete product systems of H.T. Dinh is shown to be a twisted semigroup crossed product whenever the product system has a twisted unit. The covariant representations of the corresponding dynamical system are always faithful, implying the simplicity of these crossed products; an application of a recent theorem of G.J. Murphy gives their nuclearity. Furthermore, a semigroup of endomorphisms of B(H) having an intertwining projective semigroup of isometries can be extended to a group of automorphisms of a larger Type I factor.
Structure of turbulence at high shear rate

The structure of homogeneous turbulence subject to high shear rate has been investigated by using three-dimensional, time-dependent numerical simulations of the Navier–Stokes equations. The instantaneous velocity fields reveal that a high shear rate produces structures in homogeneous turbulence similar to the ‘streaks’ that are present in the sublayer of wall-bounded turbulent shear flows. Statistical quantities such as the Reynolds stresses are compared with those in the sublayer of a turbulent channel flow at a comparable shear rate made dimensionless by turbulent kinetic energy and its dissipation rate. This study indicates that high shear rate alone is sufficient for generation of the streaky structures, and that the presence of a solid boundary is not necessary. Evolution of the statistical correlations is examined to determine the effect of high shear rate on the development of anisotropy in turbulence. It is shown that the streamwise fluctuating motions are enhanced so profoundly that a highly anisotropic turbulence state with a ‘one-component’ velocity field and ‘two-component’ vorticity field develops asymptotically as total shear increases. Because of high shear rate, rapid distortion theory predicts remarkably well the anisotropic behaviour of the structural quantities.
The structure and dynamics of galaxies formed by cold dissipationless collapse

The observable characteristics and phase-space structure of systems formed by dissipationless collapse are investigated. An extensive set of N-body simulations is described; and three-dimensional and spherical collapses, their shapes, and dynamics are examined. It is demonstrated that collapses started from cold initial conditions are quantitatively different from warm collapses, in the sense that their final shapes are nearly uncorrelated with their initial shapes. It is suggested that this phenomenon is due to an instability similar to the radial-orbit instability in anisotropic equilibrium models. The results show that clumpy initial conditions are not required to produce a realistic final state via collapse, if the initial state is sufficiently cold; and that if elliptical galaxies collapsed from cold and smooth initial configurations (and did not evolve significantly thereafter), they should be triaxial or prolate, with intrinsic flattening of approximately 2:1. 24 refs.
Description of Stress-Strain Curves by Three Parameters

A simple formula is suggested for describing the stress-strain curve in terms of three parameters; namely, Young's modulus and two secant yield strengths. Dimensionless charts are derived from this formula for determining the stress-strain curve, the tangent modulus, and the reduced modulus of a material for which these three parameters are given. Comparison with the tensile and compressive data on aluminum-alloy, stainless-steel, and carbon-steel sheet in NACA Technical Note No. 840 indicates that the formula is adequate for most of these materials. The formula does not describe the behavior of alclad sheet, which shows a marked change in slope at low stress. It seems probable that more than three parameters will be necessary to represent such stress-strain curves adequately.
Terabit/s data transmission using optical frequency combs

Terabit/s interconnects rely on advanced wavelength-division multiplexing (WDM) schemes. However, while efficient photonic-electronic interfaces can be efficiently realized on silicon-on-insulator chips, dense integration of WDM laser sources still represents a major challenge. Chip-scale frequency comb sources are an attractive alternative for providing optical carriers for WDM transmission. In this paper we give an overview on our recent work towards terabit/s data transmission using optical frequency combs. We demonstrate transmission of a 32.5 Tbit/s data stream using a modelocked solid-state laser as an optical source. Our current experiments aim at transmission schemes that exploit Kerr nonlinearities in high-Q microresonators for frequency comb generation.
Angina with non-obstructed coronary arteries

The term ‘angina pectoris’, proposed over 200 years ago, is generally considered synonymous with obstructive coronary artery disease (CAD). In recent years, however, it has become apparent that abnormalities of the coronary microcirculation (coronary microvascular dysfunction, CMD) play an additional pathogenic role in the pathogenesis of myocardial ischaemia and angina. Functional and structural mechanisms can affect the physiological function of the coronary microvasculature and lead to myocardial ischaemia in people without CAD. Abnormal dilatory responses of the coronary microvessels, coronary microvascular spasm, and increased extravascular compressive forces have been identified as pathogenic mechanisms.1 The condition characterized by anginal symptoms and evidence of myocardial ischaemia triggered by CMD, in the absence of obstructive CAD, is known as ‘microvascular angina’ (MVA).
Suzaku Observations of Unidentified X-Ray Sources toward the Galactic Bulge

We present Suzaku observations of two unidentified sources towards the Galactic bulge, 1RXSJ165256.3� 264503 and 1RXS J174459.5� 172640, both of which were discovered with the ROSAT All-Sky Survey. We obtained wide-band spectra of these sources above 2keV for the first time. The X-ray spectrum of 1RXS J165256.3� 264503 consists of two absorbed thin thermal plasma components with temperatures of 0.7 and 2.4keV. An RSCVn star, HD152178, was found within a 90% error circle of the source position. Due to this position coincidence, and an X-ray spectrum analogous to those of other RSCVn binaries, we concluded that 1RXS J165256.3� 264503 is an RSCVn-type active binary. The X-ray spectrum of 1RXSJ174459.5� 172640 was dominated by continuum emission extending up to � 20keV, which can be explained by an absorbed cutoff power-law or a combination of absorbed multicolor disk-blackbody and Comptonized emission. We inferred that the source is a new Galactic-bulge low-mass X-ray binary (LMXB) with a luminosity of 2 � 10 35 ergs � 1 , based on its X-ray spectrum and lightcurve. Hence, 1RXSJ174459.5� 172640may be an intriguing example of an LMXB in
JVLA Observations of IC 342: Probing Star Formation in the Nucleus

IC 342 is a nearby, late-type spiral galaxy with a young nuclear star cluster surrounded by several giant molecular clouds. The IC 342 nuclear region is similar to the Milky Way and therefore provides an interesting comparison. We explore star formation in the nucleus using radio recombination line (RRL) and continuum emission at 5, 6.7, 33, and 35 GHz with the JVLA. These radio tracers are largely unaffected by dust and therefore sensitive to all of the thermal emission from the ionized gas produced by early-type stars. We resolve two components in the RRL and continuum emission within the nuclear region that lie east and west of the central star cluster. These components are associated both spatially and kinematically with two giant molecular clouds. We model these regions in two ways: a simple model consisting of uniform gas radiating in spontaneous emission, or as a collection of many compact H ii regions in non-local thermodynamic equilibrium. The multiple H ii region model provides a better fit to the data and predicts many dense ( ), compact ( pc) H ii regions. For the whole nuclear region as defined by RRL emission, we estimate a hydrogen-ionizing rate of , corresponding to the equivalent of ∼2000 O6 stars and a star formation rate of ∼0.15 M⊙ yr−1. We detect radio continuum emission west of the southern mini molecular spiral arm, consistent with trailing spiral arms.
A Scheme for Calculation of the Liquid Fraction in Mixed-Phase Stratiform Clouds in Large-Scale Models

A scheme for calculation of the liquid fraction f l in mixed-phase stratiform clouds has been developed for use in large-scale models. An advantage of the scheme, compared to the interpolation in temperature that is typically used, is that it makes it possible to simulate the life cycles of mixed-phase clouds, and the differences between deep and shallow clouds. The central part of the scheme is a physically based calculation of the growth of cloud ice crystals by vapor deposition at the expense of coexisting cloud liquid water, the so-called Bergeron‐ Findeisen mechanism. Versions of this calculation have been derived for three different ice-crystal habits (spheres, hexagonal plates, or columns) and for two different assumed spatial relationships of the coexisting cloud ice and liquid water (horizontally adjacent or uniformly mixed). The scheme also requires a parameterization of the ice crystal number concentration Ni. The variation with temperature of f l looks broadly realistic compared to aircraft observations taken in the vicinity of the British Isles when the scheme is used in the CSIRO GCM, if Ni is parameterized using a supersaturation-dependent expression due to Meyers et al. If Fletcher’s earlier temperature-dependent expression for Ni is used, the scheme generates liquid fractions that are too large. There is also considerable sensitivity to the ice-crystal habit, and some sensitivity to model horizontal resolution and to the assumed spatial relationship of the liquid water and ice. A further test shows that the liquid fractions are lower in cloud layers that are seeded from above by falling ice, than in layers that are not seeded in this way. The scheme has also been tested in limited-area model simulations of a frontal system over southeastern Australia. Supercooled liquid water forms initially in the updraft, but mature parts of the cloud are mostly glaciated down to the melting level. This behavior, which is considered to be realistic based on observations of similar cloud systems, is not captured by a conventional temperature-dependent parameterization of f l. The variation with temperature of f l shows a marked sensitivity to the assumed spatial relationship of the liquid water and ice. The results obtained using the uniformly mixed assumption are considered to be more realistic than those obtained using the horizontally adjacent assumption. There is also much less sensitivity to the time step when the former assumption is used.
Exact Critical Percolation Probabilities for Site and Bond Problems in Two Dimensions

An exact method for determining the critical percolation probability, pc, for a number of two‐dimensional site and bond problems is described. For the site problem on the plane triangular lattice pc = ½. For the bond problem on the triangular, simple quadratic, and honeycomb lattices, pc=2 sin (118π),12,1−2 sin (118π), respectively. A matching theorem for the mean number of finite clusters on certain two‐dimensional lattices, somewhat analogous to the duality transformation for the partition function of the Ising model, is described.