Miracle-dz/UniFAR-FTUs huggingface dataset:
Detection of Shocked Molecular Gas by Full-Extent Mapping of the Supernova Remnant W44

Molecular gas toward the supernova remnant (SNR) W44 (G34.7-0.4) was extensively mapped in CO J = 1–0 emission with the 17″ beam of the Nobeyama 45 m radio telescope. We detected high-velocity (>25 km s-1) CO line wings. They are confined to compact (≈1.5 pc) spots, and they are located adjacent to bright radio filaments or knots. The low 13CO/12CO intensity ratio of 0.03 and high HCO+/12CO intensity ratio of 0.3 suggest that the wing-emitting gas has a moderate 12CO opacity of ≈1 and a high density of n(H2) > 105 cm-3. This gas might be shocked molecular gas that has been accelerated and compressed by the expanding blast waves of W44. In addition, the high spatial resolution CO maps reveal several other features that may reveal the interaction between the SNR and the surrounding interstellar gas. The giant molecular cloud CO G34.8-0.6 (vLSR = 48 km s-1) has a sharp edge coincident with the eastern radio continuum rim of W44, which may indicate that we observe the SNR/cloud interaction almost edge-on. The existence of the "edge" suggests that most of the molecular mass resides in smaller clumps that evaporate rapidly after the passage of the supernova blast wave. We also find spatially extended moderately broad emission (SEMBE) with a moderately large intensity of ≈30 K km s-1 in CO J = 1–0 and a typical line width of ≈10 km s-1 (FWHM). Its extent coincides with the brighter region of the radio synchrotron emission. We discuss the SEMBE in terms of molecular clumps shocked and disturbed by the compressed shell of the SNR.
Surface-layer fluxes, profiles, and turbulence measurements over uniform terrain under near-neutral conditions

Abstract An atmospheric surface-layer experiment over a nearly uniform plowed field was performed to determine the constants in the flux-profile similarity formulas, particularly the von Karman constant. New instruments were constructed to minimize flow distortion effects on the turbulence measurements and to provide high-resolution gradient measurements. In addition, a hot-wire anemometer directly measured the turbulent kinetic energy dissipation rate. An average value of the von Karman constant of 0.365 ± 0.015 was obtained from 91 runs (31 h) in near-neutral stability conditions. However, four near-neutral runs when snow covered the ground gave an average value of 0.42. This result suggests that the von Karman constant depends on the roughness Reynolds number, which may resolve some of the differences in previous determinations over different surfaces. The one-dimensional Kolmogorov inertial subrange constant was found to have a value of 0.54 ± 0.03, slightly larger than previous results. The flux-prof.
A note on estimation by least squares for harmonic component models

Abstract. Let observations (X1,…,Xn) be generated by a harmonic model such that Xt=A0 cos ω0t+B0 sin ω0t+εt, where A0,B0,ω0 are constants and (εt) is a stationary process with zero mean and finite variance. The estimation of A0,B0,ω0 by the method of least squares is considered. It is shown that, without any restriction on ω in the minimization procedure, the estimate is an n‐consistent estimate of ω0, and hence () has the usual asymptotic distribution.
Placing the Fornax and Sagittarius Dwarf Spheroidal Globular Clusters in the Horizontal-Branch Type versus Metallicity Diagram

We plot the globular clusters of the Fornax galaxy and those associated with the Sagittarius dwarf spheroidal galaxy in the horizontal-branch type versus metallicity diagram. The horizontal-branch types for the Fornax clusters include corrections for red horizontal-branch stars from the field and are based on our recent work and new results in the literature. Fornax globular clusters continue to stand out as having red horizontal branches for their low ([Fe/H] ∼ -2) metallicities, with no counterparts in either the outer Galactic halo or the Magellanic Clouds. The clusters associated with Sagittarius lie to the blue of the Fornax clusters, except for the metal-rich cluster Ter 7. Although the metallicities of the three metal-poor Sagittarius globular clusters are similar to those of the Fornax clusters, their horizontal branches are bluer and they lie in a region also populated by the old LMC and old halo clusters. Neither cluster system resembles the younger Galactic halo globular clusters, often suggested to have been accreted from disrupted dwarf spheroidal galaxies. Except for Ter 7, both the Fornax and Sagittarius globular clusters are metal-poor compared with their Galactic counterparts of the same horizontal-branch type. We find no correlation between HB type and other cluster properties such as central concentration, luminosity, central surface brightness, and estimated collision rate.
Application of the discrete null space method to domain decompositionand large deformation contact problems

We aim at the development of energy consistent ‘mechanical’ integrators for the differential‐algebraic equations (DAEs) associated with the contact problems under consideration. First steps towards the energy consistent time integration of frictionless dynamic contact problems can be found in the works by Laursen & Chawla [4], Armero & Petöcz [1] and Laursen & Love [5]. Energy consistent mechanical integrators have been recently developed for DAE‐formulations of constrained mechanical systems (e.g. Gonzalez [3]). These works are based on the direct discretization of the underlying DAEs leading to a saddle point system to be solved in each iteration of the iterative solution procedure. Due to the presence of Lagrange multipliers this approach leads to a large number of unknowns and potential conditioning problems. To remedy these drawbacks the discrete null space method (Betsch [2]) has been recently developed. We apply the discrete null space method to both domain decomposition in the framework of nonlinear elastodynamics and large deformation contact problems. (© 2006 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
RADIAL VELOCITIES OF M DWARF STARS.

Radial velocities for 72 M dwarfs have been obtained having internal errors of about 0.1 km/s and external errors of about 0.4 km/s. Multiple velocity measurements of ten dMe stars have yielded a set of six which have no stellar companions, providing confirmation that the dMe phenomenon can occur in single stars. These single dMe stars have low space motions indicative of relative youth. Four stars from the entire survey were found to have double-line spectra and two were found to be single-line spectroscopic binaries of low amplitude. The zero point of the velocity scale is found to agree well with that of O. C. Wilson (1967) and differences are noted among other radial-velocity studies. Most of the stars in this study have velocities sufficiently well determined to constitute potential radial-velocity standards.
On left derivations and related mappings

Let R be a ring and X be a left R-module. The purpose of this paper is to investigate additive mappings D1: R -* X and D2: R -X that satisfy D, (ab) = aD1 (b) + bD, (a), a, b E R (left derivation) and D2(a2) = 2aD2(a), a E R (Jordan left derivation). We show, by the rather weak assumptions, that the existence of a nonzero Jordan left derivation of R into X implies R is commutative. This result is used to prove two noncommutative extensions of the classical Singer-Wermer theorem.
Locating sets and numbers of graphs associated to commutative rings

For a graph G(V, E) with order n ≥ 2, the locating code of a vertex v is a finite vector representing distances of v with respect to vertices of some ordered subset W of V(G). The set W is a locating set of G(V, E) if distinct vertices have distinct codes. A locating set containing a minimum number of vertices is a minimum locating set for G(V, E). The locating number denoted by loc(G) is the number of vertices in the minimum locating set. Let R be a commutative ring with identity 1 ≠ 0, the zero-divisor graph denoted by Γ(R), is the (undirected) graph whose vertices are the nonzero zero-divisors of R with two distinct vertices joined by an edge when the product of vertices is zero. We introduce and investigate locating numbers in zero-divisor graphs of a commutative ring R. We then extend our definition to study and characterize the locating numbers of an ideal based zero-divisor graph of a commutative ring R.
On Properties of Product Acts over Monoids

Let S be a monoid. It is known that flatness may be defined in a number of ways for the class of right S − acts, and these notions themselves naturally give rise to some weaker associated conditions. To date no work has been done on these properties of product acts. This article is concerned with closure under products of the class of right S − acts possessing one of these “flatness” properties and conversely, when these properties transfer from products to components. We consider such questions for both a general monoid S, and for monoids coming from some special classes. Specifically, we answer the question of when properties such as torsion freeness, principal weak flatness, GP − flatness, (weak) flatness, Conditions (P), (P′), etc. transfer from products of acts to their components. Also we give equivalences of when properties such as torsion freeness, Conditions (PWP), (P′) (EP), etc. transfer from acts to their products. Finally, we extend some results from Bulman-Fleming, S. , Gilmour, A.
Accelerating non-local means algorithm with random projection

The non-local means (NLM) algorithm suppresses noise via replacing the noisy pixel by the weighted average of all the pixels with similar neighbourhood vectors. However, the weights calculation is computationally expensive, as a result of which the NLM algorithm is quite slow for practical applications. A random projection approach is introduced to reduce the dimension of neighbourhood vectors used in the NLM filtering process, which yields a faster and more accurate denoising effect. Experimental results illustrate the effectiveness of the proposed method.
Hypervelocity Fuel / Air Mixing in Mixed-Compression Inlets of Shcramjets

This paper investigates the mixing of hydrogen fuel with air in the mixing duct of a mixed-compression shock-induced combustion ramjet (shcramjet) inlet. Mixing augmentation through the use of cantilevered ramp injector arrays on opposite shcramjet inlet walls is studied and the influence of relative array locations is quantified. Studies were undertaken numerically using the WARP code that solves the Favre-averaged Navier-Stokes equations closed by the Wilcox k-w turbulence model. Air-based mixing efficiencies of up to 0.58-0.68 were achieved with thrust potential losses less than that gained from high-speed fuel injection. Shocks created from the fuel injector structures play a major role in the mixing behavior of the fuel jets on the opposing side of the mixing duct. Chemically reacting studies verified for the correct selection of spanwise displacement of the fuel injectors, an air buffer created between the fuel and walls suppresses premature ignition while still allowing for a mixing efficiency of up to 0.46-0.54.
Current Drive Calculations with an Advanced Adjoint Approach

Abstract The advanced adjoint approach for arbitrary collisionalities with momentum conservation in the like-particle collision is considered. The results are generally applicable for the parallel conductivity as well as for current drive calculations. In addition, the weakly relativistic extension of the variational principle for the Spitzer function with momentum conservation in the electron-electron collision is described. The models developed are well suited to ray-tracing calculations.
The Structure of Tornadoes near Attica, Kansas, on 12 May 2004: High-Resolution, Mobile, Doppler Radar Observations

Abstract The University of Massachusetts W- and X-band, mobile, Doppler radars scanned several tornadoes at close range in south-central Kansas on 12 May 2004. The detailed vertical structure of the Doppler wind and radar reflectivity fields of one of the tornadoes is described with the aid of boresighted video. The inside wall of a weak-echo hole inside the tornado was terminated at the bottom as a bowl-shaped boundary within several tens of meters of the ground. Doppler signatures of horizontal vortices were noted along one edge in the lowest 500 m of the tornado. The vertical structure of Doppler velocity displayed significant variations on the 100-m scale. Near the center of the tornado, a quasi-horizontal, radial bulge of the weak-echo hole at ∼500–600 m AGL dropped to about 400 m above the ground and was evident as a weak-echo band to the south of the tornado. It is suggested that this feature represents echo-weak material transported radially outward by a vertical circulation. Significant vertical .
Positive charging of fluorinated ethylene propylene copolymer (Teflon) by irradiation with low‐energy electrons

Starting with electron energies above a few keV, all materials show an increase in the number of secondary and backscattered primary electrons with decreasing primary energy. The number of secondary plus backscattered electrons becomes equal to the number of primaries at two energies called the first and second crossover points. Between these energies the number of backscattered primaries and of secondaries exceeds the number of incoming primaries. For Teflon FEP the higher‐energy crossover (second crossover) point occurs at about 1.6 keV. Between this energy and the first crossover (at a few hundred eV), holes are generated in the surface region of the material. This effect can be used to charge the surface of an insulating dielectric positively by negatively biasing the metallized rear during charging and subsequent discharging of the rear electrode after irradiation.
Surface fields on linear antennas

Surface fields are calculated for a source-excited flat-strip antenna in free space by modifying a variationalimpedance formulation. The exciting fields are related by an integral to the antenna current, and approximate current distributions correspond to nonvanishing tangential-electric-field components on the metallic antenna surface. Current distributions consisting of sine and shifted cosine waves violate the edge conditions and excite strong tangential electric fields near the ends of the conducting antenna surface. These field singularities are avoided by making the antenna current decay in proportion to the square root of the distance from the antenna edge. The more accurate current distributions produce smaller surface fields on the antenna, and it is possible to distinguish the more accurate current distribution even in cases where the variationally determined antenna impedances differ insignificantly. The calculated current distributions and impedances are compared with experimental data and with results of iterative calculations.
Beam wander experiments: terrestrial path

We report on a set of measurements made in December 2005 by researchers from the University of Central Florida, SPAWAR's Innovative Science and Technology Experiment Facility (ISTEF), Harris Corporation, NASA Kennedy Space Center, and Northrop Grumman. The experiments were conducted on the Shuttle Landing Facility (SLF) at Kennedy Space Center (KSC) over terrestrial paths of 1, 2, and 5 km. The purpose of the experiments was to determine the atmospheric-induced beam spreading and beam wander at various ranges. Two lasers were used in the experiments. Both were a pulsed 1.06 μm laser; however, one was single-mode and the other was multi-mode. Beam profiles were recorded near the target position. Simultaneous measurements of Cn2, wind speed and direction, humidity, visibility, temperature, and surface temperature profiles were all recorded.
The choice of conservation equations for plume models

Theories on the behavior of turbulent buoyant plumes generally form three classes: (1) strictly self-similar models valid only in a uniform environment; (2) quasi-similar models based on flux conservation of mass, momentum, and heat; and (3) quasi-similar models based on conservation of momentum, heat, and kinetic energy of mean motion. Few direct comparisons of the various numerical solutions for the different models have been reported; and little attempt has been made to compare the formulation of models (2) and (3) in spite of the fact that such a comparison must form the basis for an understanding of their differences. The following contribution has been stimulated by yet another solution published recently by Fox in this journal, but differs from earlier papers in that it concentrates wholly on a discussion of the equations used in the two quasi-similarity approaches. The relationship between the field and gross-flux forms of the equations of motion is considered. In particular, it is shown that the use of the flux equations for vertical momentum and kinetic energy is not equivalent to the use of flux equations for mass and vertical momentum, and that the latter pair is to be preferred.
Absorption and emission spectra of a Schwarzschild black hole

The absorption spectrum of a Schwarzschild black hole is studied in detail. Accurate and useful computational methods based on the analytical resolution of the wave equation are developed. In this way phase shifts and absorption cross sections are obtained for a wide range of energy and angular momentum. Comparison with the explicit results valid for low and high frequencies is made. The total absorption cross section of the black hole is obtained as a function of the energy. It presents behavior characteristic of a diffraction pattern. The constant geometric-optics limit [$(\frac{27}{4})\ensuremath{\pi}r_{s}^{}{}_{}{}^{2}$] is approached in an oscillatory fashion. The physical interpretation of these results is given and a simple model which describes qualitatively the absorption of waves by the black hole is presented. From these absorption parameters, the Hawking emission rates are calculated and their properties discussed.
Magnetohydrodynamic Simulations of Stellar Magnetosphere-Accretion Disk Interaction

The magnetohydrodynamic evolution of the interaction region between the inner edge of an accretion disk and the magnetosphere of the central object is studied by means of time-dependent numerical simulations. The simulations assume the disk is adiabatic, is axisymmetric, has nonzero resistivity, and is initially in Keplerian rotation. The magnetosphere is assumed to be initially in magnetostatic equilibrium, corotating with the central star, and threaded by one of three different initial magnetic field topologies: (1) a pure dipole field, which also threads the disk continuously everywhere; (2) a dipole field excluded from the disk by surface currents; and (3) a dipole field continuously threading a disk superposed with a uniform axial magnetic field. A number of exploratory simulations are performed by varying the field strength, the disk density and inner radius, the magnitude of the resistivity, and the stellar rotation rate. These simulations are designed as an initial study of the magnetohydrodynamics of the interaction region. Generally, we find that rapid evolution of the disk occurs because of angular momentum transport by either the Balbus-Hawley instability or magnetic braking effects. Equatorial accretion results on a dynamical timescale unless the magnetic pressure of the magnetosphere exceeds the ram pressure of the accreting disk plasma; the latter we find to be a highly time-dependent quantity. In the case of a pure dipole magnetospheric field, however, rapid stellar rotation can result in a field geometry that inhibits polar accretion even when ram and magnetic pressures balance. In contrast, we find that polar accretion can occur regardless of the stellar rotation rate when strong global disk magnetic fields combine with stellar magnetic fields to create a favorable net field topology. Highly time-dependent winds are evident in the evolution of all three field topologies. The winds are generally channeled along field lines that have been opened through reconnection. The speed and variability of the outflows is dependent on the magnetic field strength and accretion topology. Net torque on the star during accretion is measured to be positive, i.e., the star is being spun up.
Solid velocity correction schemes for a temperature transforming model for convection phase change

Purpose – To study the effects of velocity correction schemes for a temperature transforming model (TTM) for convection controlled solid‐liquid phase‐change problem.Design/methodology/approach – The effects of three different solid velocity correction schemes, the ramped switch‐off method (RSOM), the ramped source term method (RSTM) and the variable viscosity method (VVM), on a TTM for numerical simulation of convection controlled solid‐liquid phase‐change problems are investigated in this paper. The comparison is accomplished by analyzing numerical simulation and experimental results of a convection/diffusion phase‐change problem in a rectangular cavity. Model consistency of the discretized TTM is also examined in this paper. The simulation results using RSOM, RSTM and VVM in TTM are compared with experimental results.Findings – In order to efficiently use the discretized TTM model and obtain convergent and reasonable results, a grid size must be chosen with a suitable time step (which should not be too .
Split delivery routing

This article examines a relaxed version of the generic vehicle routing problem. In this version, a delivery to a demand point can be split between any number of vehicles. In spite of this relaxation the problem remains computationally hard. Since only small instances of the vehicle routing problem are known to be solved using exact methods, the vehicle route construction for this problem version is approached using heuristic rules. The main contribution of this article to the existing body of literature on vehicle routing issues in (a) is presenting a new vehicle routing problem amenable to practical applications, and (b) demonstrating the potential for cost savings over similar “traditional” vehicle routing when implementing the model and solutions presented here. The solution scheme allowing for split deliveries is compared with a solution in which no split deliveries are allowed. The comparison is conducted on six sets of 30 problems each for problems of size 75, 115, and 150 demand points (all together 540 problems). For very small demands (up to 10% of vehicle's capacity) no significant difference in solutions is evident for both solution schemes. For the other five problem sets for which point demand exceeds 10% of vehicle's capacity, very significant cost savings are realized when allowing split deliveries. The savings are significant both in the total distance and the number of vehicles required. The vehicles' routes constructed by our procedure tend to cover cohesive geographical zones and retain some properties of optimal solutions.
Tours Symposium on Nuclear Physics IV

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