Miracle-dz/UniFAR-FTUs huggingface dataset:
The structure of extended extragalactic radio sources

The observational properties of extragalactic radio sources of sizes comparable with or greater than a typical galactic diameter and intrinsic luminosities at 408 MHz greater than 10 to the 23rd W/Hz are discussed. Following a survey of the major instrumental and observational techniques developed over the last three decades for the measurement of source structure, classes of radio structure that are commonly observed, including narrow edge-brightened and -darkened double sources, narrow- and wide-tailed sources and cluster halos, are described, and various taxonomic sequences of these morphologies are discussed. Means by which such physical properties as the energetics, confinement parameters, magnetic fields, sites of electron acceleration and rotation are derived from intensity and polarization distribution measurements are examined, and the observed characteristics of the various components of extended radio sources are considered in detail, including diffuse emission regions, hot spots, cores and jets. Finally, relationships of radio source morphologies to the properties of the parent galaxies and clusters are reviewed, and a model of the radio-source phenomenon is proposed.
Size and shape analysis of landmark data

SUMMARY The paper deals with statistical analysis of landmark data using the exact joint distribution theory for the size and shape of planar Gaussian configurations. This is an extension of earlier work which considered marginal shape analysis. Special cases of the size and shape distribution are examined and the isotropic Gaussian model is investigated in particular detail. Various properties are studied, including conditional distributions and a curve of regression. Finally we consider some possible approaches to inference, including exact maximum likelihood estimation of size and shape. A practical biological application is given which investigates the size and shape of mouse vertebrae.
A Numerical model based on the mixed interface‐tracking/interface‐capturing technique (MITICT) for flows with fluid–solid and fluid–fluid interfaces

We propose a numerical model for computation of flow problems that involve both fluid–solid and fluid–fluid interfaces. The model is based on the mixed interface‐tracking/interface‐capturing technique (MITICT), which was introduced earlier for problems that involve both fluid–solid interfaces that are accurately tracked with a moving mesh method and fluid–fluid interfaces that are too complex to track and therefore treated with an interface‐capturing technique. In our numerical model, fluid–solid interfaces are handled with the moving Lagrangian interface technique (MLIT) and fluid–fluid interfaces with the edge‐tracked interface locator technique (ETILT). The mixed technique is tested in computation of a fluid–particle interaction problem in the presence of a fluid–fluid interface impacted by the particle. Copyright © 2007 John Wiley & Sons, Ltd.
The evolution of the lithium abundances of solar-type stars. III - The Pleiades

New measurements of lithium in more than 100 Pleiades F, G, and K dwarfs are reported. Abundances are determined from spectrum synthesis fits to the data as well as from use of new covers of growth from the Li 6708-A feature. It is argued that most Late-F and early-G dwarfs in the Pleiades are consistent with the tight N(Li) vs mass relation seen in the Hyades in the same mass range. Most Li-rich stars have abundances at or near the primordial level for Population I, and none exceed that level by a significant amount. At any given color the stars that rotate fast have the most Li and have the strongest chromospheric activity. Ways in which an apparent spread in N(Li) could arise from an intrinsically tight n(Li)-mass relation are considered, and it is concluded that the spread is probably real and is not an artifact of line formation conditions or inhomogeneous atmospheres on the stars.
On $L_p$-Norms of Multivariate Density Estimators

where K is a bivariate function satisfying certain regularity conditions and h(n) is a sequence of positive numbers. Density estimators of the form (1.1) were introduced by Rosenblatt (1956) and Parzen (1962) and have been extensively studied since then. For a recent survey on density estimators, we refer to the monograph of Prakasa Rao (1983). In this article we consider the asymptotic properties of
Superconductivity-Induced Transparency in Terahertz Metamaterials

A plasmonic analogue of electromagnetically induced transparency is activated and tuned in the terahertz (THz) range in asymmetric metamaterials fabricated from high critical temperature (Tc) superconductor thin films. The asymmetric design provides a near-field coupling between a superradiant and a subradiant plasmonic mode, which has been widely tuned through superconductivity and monitored by Fourier transform infrared spectroscopy. The sharp transparency window that appears in the extinction spectrum exhibits a relative modulation up to 50% activated by temperature change. The interplay between ohmic and radiative damping, which can be independently tuned and controlled, allows for engineering the electromagnetically induced transparency of the metamaterial far beyond the current state-of-the-art, which relies on standard metals or low-Tc superconductors.
The birth of high-energy neutrino astronomy: A personal history of the DUMAND project

DUMAND is a project to build a Deep Underwater Muon And Neutrino Detector offshore near the island of Hawaii. At present under construction, it hopes to inaugurate the field of high-energy neutrino astronomy. Potential sources of high-energy neutrinos are listed, and estimates of neutrino intensity given. The paper is concerned with the physics, technology, and history of the project, which started informally in 1973. It survived through a series of summer conferences until it was funded as a feasibility study in 1979 and established in the Hawaii DUMAND Center, at the University of Hawaii. Over a dozen collaborating groups have contributed to the successful construction and operation of DUMAND I, the SPS or Short Prototype String, which established the benign character of the ocean environment and demonstrated its suitability for DUMAND II, a 216-phototube array now under construction. DUMAND II, recently funded, will have more than 20 times the area of any existing detector and a mass of almost 2 million tons; this size is minimal for the intensities and cross sections anticipated. The project became feasible---both technically and financially---through important technical advances in data transmission via fiber optics, high-speed computer technology, special photomultiplier tubes made by Hamamatsu and Philips,more » remotely controlled undersea vehicles with manipulative abilities, and many deep-sea electronic and oceanographic components. It is supported by an international collaboration with 15 collaborating institutions in the U.S., Europe, and Japan. It is scheduled to install a three-string test array (TRIAD) by late 1992, and the complete nine-string array is scheduled for operation in late 1993. « less
Comparing the fundamental frequencies of resolved and unresolved harmonics: Evidence for two pitch mechanisms?

Four experiments measured sensitivity (d′) to differences in fundamental frequency (F0) between two simultaneously presented groups of frequency‐modulated harmonics. Each group was passed through a bandpass filter in either a LOW (125–625 Hz), MID (1375–1875 Hz), or HIGH (3900–5400 Hz) frequency region. In the first two experiments, a dynamic F0 difference (ΔF0) was created by introducing a 180° disparity between the frequency modulations imposed on the two groups. Experiment 1 measured sensitivity to such ΔF0’s between a MID group with a baseline F0 of 125 Hz and all components summed in sine phase, and a HIGH group, in four conditions. When the baseline F0 of the HIGH group was also 125 Hz, performance was good when its components were summed in sine phase and bad when they were in alternating phase. Conversely, when the HIGH F0 was 62.5 Hz, performance was better for alternating phase than for sine phase, consistent with alternating phase doubling the internal representation of HIGH group’s F0. Similar.
Optimal 3-D traveltime tomography

We propose a practical new method for 3-D traveltime tomography. The method combines an efficient approximation to the extended Kalman filter for rapid, accurate, nonlinear tomography, with the concept of data‐driven zonation, in which the dimensionality and geometry of the parameterization are dynamically determined using cluster analysis and region merging by random field union. The Bayesian filter uses geostatistics as it recursively incorporates measurements in an optimal (minimum‐variance) manner. Geologic knowledge is introduced through a priori estimates of the parameter field and its spatial covariance. Conditional estimates of the parameter number, geometry, value, and covariance are evolved. An initial decomposition of the 3-D domain into 2-D slices, the simplified filter design, and the data‐driven reduction in parameter dimensionality, all contribute to make the method computationally feasible for large 3-D domains. The method is verified by the inversion of crosswell seismic traveltimes to 3-.
A new 3D-registration method based on arbitrary geometric shape and unscented particle filter

A tracking algorithm based on arbitrary geometric shape and Unscented Particle Filter is proposed in this paper. Traditional tracking algorithm based on arbitrary geometric shape has following advantages, matching convenient, high precision, but when the geometric shape is not fully visible it results tracking failure so that restricts its use. Another tracking algorithm based on natural feature utilizes natural feature points to finish registration, there are disadvantages such as error accumulation as time goes by. This approach firstly uses arbitrary geometric shape to finish camera calibration, then use unscented particle filter to predict the possible location of the camera, and get 3-D registration matrix, it can reduce non-linear, non-Gaussian interfere brought by other issues. Experiment results show that this method can efficiently work under the circumstances of occlusion, large changes in illumination, and have a high accuracy.
Bayesian multivariate GARCH models with dynamic correlations and asymmetric error distributions

The main goal in this paper is to develop and apply stochastic simulation techniques for GARCH models with multivariate skewed distributions using the Bayesian approach. Both parameter estimation and model comparison are not trivial tasks and several approximate and computationally intensive methods (Markov chain Monte Carlo) will be used to this end. We consider a flexible class of multivariate distributions which can model both skewness and heavy tails. Also, we do not fix tail behaviour when dealing with fat tail distributions but leave it subject to inference.
Theorie des festen Zustandes einatomiger Elemente

1. Die Voraussetzungen der Theorie. 2. Die potentielle Energie des Mol. 3. Direktionskraft und Frequenz des einzelnen Atoms. 4. Uber den Wert der Funktion ϕ. 5. Die Anderung der Frequenz mit Temperatur und Druck. 6. Die Zustandsgleichung des festen Korpers. 7. Isochorische Zustandsanderung. 8. Atomwarme, Schwingungsenergie und Entropie als Funktionen von Temperatur und Druck. 9. Adiabatische Zustandsanderung. 10. Isotherme Zustandsanderung. 11. Isopiestische Zustandsanderung (Thermische Ausdehnung). 12. Die Sublimationswarme beim absoluten Nullpunkt. 13. Berechnung der Frequenz aus der Kompressibilitat oder aus dem Grenzverhaltnis von Atomwarme und Ausdehnungskoeffizient. 14. Die Ausdehnung der Theorie auf hohere Temperaturen. 15. Volumanderung zwischen Nullpunkt und Schmelzpunkt. 16. Das Verhaltnis der mittleren Schwingungsamplitude zur Volumausdehnung. Raumerfullung der Atome. 17. Beziehung zwischen Frequenz und Schmelzpunkt. 18. Beziehung zwischen Kompressibilitat und Schmelztemperatur. 19. Uber den Schmelzvorgang und die Schmelzwarme.
Direct numerical simulation of isotropic turbulence interacting with a weak shock wave

Interaction of isotropic quasi-incompressible turbulence with a weak shock wave was studied by direct numerical simulations. The effects of the fluctuation Mach number Mt of the upstream turbulence and the shock strength M21 — 1 on the turbulence statistics were investigated. The ranges investigated were 0.0567 ≤ Mt ≤ 0.110 and 1.05 ≤ M1 ≤ 1.20. A linear analysis of the interaction of isotropic turbulence with a normal shock wave was adopted for comparisons with the simulations. Both numerical simulations and the linear analysis of the interaction show that turbulence is enhanced during the interaction with a shock wave. Turbulent kinetic energy and transverse vorticity components are amplified, and turbulent lengthscales are decreased. The predictions of the linear analysis compare favourably with simulation results for flows with M2t < a(M21 — 1) with a ≈ 0.1, which suggests that the amplification mechanism is primarily linear. Simulations also showed a rapid evolution of turbulent kinetic energy just downstream of the shock, a behaviour not reproduced by the linear analysis. Investigation of the budget of the turbulent kinetic energy transport equation shows that this behaviour can be attributed to the pressure transport term. Shock waves were found to be distorted by the upstream turbulence, but still had a well-defined shock front for M2t < a(M21— 1) with a ≈ 0.1). In this regime, the statistics of shock front distortions compare favourably with the linear analysis predictions. For flows with M2t > a(M21— 1 with a ≈ 0.1, shock waves no longer had well-defined fronts: shock wave thickness and strength varied widely along the transverse directions. Multiple compression peaks were found along the mean streamlines at locations where the local shock thickness had increased significantly.
Confidence Intervals for Correlation Ratios

It is suggested that for fixed effects experiments, the traditional statistical question is inappropriate. It is suggested that variance ratios—the signal to noise ratio (σ2 a /σ2 e ) and the correlation ratio (σ2 a /σ 2 t )—are more desirable. Criticisms of these values are explored. Finally confidence intervals and percentiles for the random and fixed effects model's signal to noise and correlation ratio are given. The latter being dependent on the evaluation of a family of non-central F distributions. The latter will also give the confidence interval and percentiles of the multiple correlation coefficient in the regression model. The lower limit of the confidence interval can test the traditional null hypothesis. The upper limit of this interval is suggested to be a test which would allow the investigator to accept the null hypothesis.
Infrared to x-ray spectral energy distributions of high redshift quasars

We have observed 14 quasars with z greater than 2.8 with the ROSAT-PSPC, and detected 12 of them, including the z=4.11 quasar 0000-263. We present the first x-ray spectrum of a radio quiet quasar with z greater than 3, 1946+768. Its x-ray spectrum is consistent with a power law with spectral index alpha(sub E)=1.8(sup +2.1, sub -1.4) and no evidence for absorption in excess of the galactic column (alpha(sub E)=1.00(sup +0.28, sub -0.32) assuming N(sub H)=N(sub H)(Gal)). A Position Sensitive Proportional Counter (PSPC) hardness ratio is used to constrain the x-ray spectral properties of the quasars for which there were less than 100 photons detected. For the radio quiet quasars, (alpha(sub E)) approximately equals 1.2, if one assumes that there is no absorption in excess of the galactic column. We combine the x-ray data with new ground based optical and near-IR spectrophotometry obtained at the Steward 2.3 m and Multiple Mirror Telescope, and data from the literature. The spectral energy distributions are compared to those of low redshift objects. For the radio quiet quasars with z greater than 2.5, the mean (alpha(sub ox)) is approximately 1.8. This is larger than the mean for quasars with z less than 2.5, but consistent with the expected value for quasars with the high optical luminosities of the objects in this sample. For the radio-loud quasars, (alpha(sub ox)) is approximately 1.4, independent of redshift. This is smaller than the expected value for the optically luminous, high redshift objects in this sample, if they are mostly GHz peaked radio sources and hence comparable to steep-spectrum, compact radio sources at lower redshift. Finally, we compare the spectral energy distributions of two representative objects to the predicted spectrum of a thin accretion disk in the Kerr geometry, and discuss the uncertainties in deriving black hole masses and mass accretion rates.
On the expansion of the rotational eigenfrequencies in Legendre polynomials

N Av(n, l, m) = v(n, l, m) v(n, l) = Lj] a¡ P¡( m/L) i = 0 (Duvall, Harvey, and Pomerantz) where v is the frequency of the nth p-mode averaged over m, the Pf are Legendre polynomials and L = [(/ + 1)/]. It is shown here that, instead, it is advantageous to use the following expansion for v(n, /, m) — v(n, /): N v(n, /, m) — v(n, /) = m £ . i = 0 In this case the h/s are simply related to the coefficients which determine the angular velocity, leading to the expectation that we can more accurately determine the internal rotation of the Sun from the extant helioseismological data. Subject headings: analytical methods — Sun: oscillations — Sun: rotation
Growth of Narrow and Straight Germanium Nanowires by Vapor–Liquid–Solid Chemical Vapor Deposition

This paper describes the growth of germanium nanowires (Ge NWs) via vapor–liquid–solid (VLS) mechanism by the low-pressure chemical vapor deposition (CVD) technique. A systematic study of the growth conditions of the Ge NWs has been conducted by varying the size of the Au nanoparticles and the substrate temperature. The tapering of the nanowires has been minimised when the growth temperature is lowered from 300 to 280 °C which also contributes to the decrease in the diameter of the Ge NWs. The growth temperature of 280 °C yields Ge NWs with diameters of less than 5 nm, offering an opportunity for the fabrication of high-performance germanium nanowire field-effect transistors.
High-throughput screening of thermoelectric oxides and power generation modules consisting of oxide unicouples

A high-throughput screening technique has been developed and utilized in the discovery of a new n-type oxide possessing good thermoelectric properties. With this technique, 1000 samples can be prepared via a sol–gel method and their Seebeck coefficient (S) evaluated all within a day. For evaluation of S, a ‘Seebeck tester’ consisting of two pairs of thermocouples, a heater and a voltage meter, was developed. S values measured using the Seebeck tester more or less coincide with those using a conventional method. The validity of this technique was proven by Ca–Co–O and Na–Co–O systems. Screening ternary systems consisting of 3d transition metals using this technique showed LaNiO3 to possess the desired n-type properties. Electrical resistivity (ρ) of this oxide is favourably quite low; however, S is as low as –25 µV K−1 at high temperature. To enhance the thermoelectric properties of LaNiO3, high-throughput screening was employed to examine candidates from the metal ternary systems La1–xM1xNiO3 and LaNi1–xM2xO3. Bi substitution in the La1–xM1xNiO3 systems and Cu substitution in the LaNi1–xM2xO3 systems were found to be effective for improvement of S and ρ, respectively. A thermoelectric unicouple composed of p-type Ca3Co4O9 (Co-349) and n-type LaNiO3 (Ni-113) bulks was constructed. Open-circuit voltage (Vo) of the unicouple reaches 100 mV at 1073 K on the hot side (TH) with a temperature difference (ΔT) of 500 K in air. Resistance of the unicouple (RI) is 26 mΩ at 1073 K in air and increases with increase in temperature. The Vo values are consistent with those calculated using S values for each oxide leg. Maximum power (Pmax), which was evaluated using the formula Pmax = V2o/4RI, is 94 mW at 1073 K (ΔT = 500 K) and increases with temperature. This value corresponds to a volume power density of 660 mW cm−3.
Indication of Te segregation in laser-irradiated ZnTe observed by in situ coherent-phonon spectroscopy

We irradiate a ZnTe single crystal with 10-fs laser pulses at a repetition rate of 80 MHz and investigate its resulting gradual modification by means of coherent-phonon spectroscopy. We observe the emergence of a phonon mode at about 3.6 THz whose amplitude and lifetime grow monotonously with irradiation time. The speed of this process depends sensitively on the pump-pulse duration. Our observations strongly indicate that the emerging phonon mode arises from a Te phase induced by multiphoton absorption of incident laser pulses. A potential application of our findings is laser-machining of microstructures in the bulk of a ZnTe crystal, a highly relevant electrooptic material.
“Space weather forecast”: Prediction of relativistic electron intensity at synchronous orbit

Long-term variations in high-energy (greater than 2 MeV) electron flux at synchronous orbit are examined to reveal their close relationship to geomagnetic activity. The electron flux diminishes rapidly in association with an enhancement of geomagnetic activity (storm) and then increases. The flux becomes higher than the pre-storm level and its peak occurs approximately 4–5 days after the enhancement of geomagnetic activity. A linear prediction filter is designed for daily sums of Kp as input data and corresponding daily averages of the electron flux (Log value) as output data. The data are those taken in 1984–1985. This filter can successfully reproduce the electron flux behavior observed not only in 1984–1985 but also in 1978–1981.
New Variational Formulation of Maxwell-Vlasov and Guiding Center Theories Local Charge and Energy Conservation Laws

A new variational formulation of Maxwell-Vlasov and related theories is given in terms of a common Lagrangian density for both the "Vlasov particles" and the Maxwell fields. This formulation is used to derive in a consistent way, on the one hand, correct charge and current densities and, on the other, corresponding energy and energy flux densities. All of these densities generally show in addition to particle like contributions electric polarization and magnetization terms. By some limiting procedure collisionless guiding center theories with polarization drifts included are also treated. In this way local energy conservation laws are formulated for such theories, which has not been possible up to now
Spectrum of atmospheric gamma rays to 10 Mev at λ = 40°

We report measurements of the differential counting rate spectra due to atmospheric γ rays as a function of altitude to 3.6 g/cm² over Texas. Two gain settings and a 128-channel pulse height analyzer were used to cover the range 0.2–10 Mev. The detector was a 7.6 cm × 7.6 cm NaI crystal, which was surrounded on five sides by a 2-cm-thick plastic anticoincidence shield for charged particle rejection. The system had a nearly isotropic response to photons above 0.2 Mev. The spectrum at ceiling appeared as a steep continuum with a power law index of about 1.4. The only obvious feature was the 0.51-Mev positron annihilation line. The spectral shape was independent for depths less than 20 g/cm², the absolute intensity varying in proportion to the intensity of the cosmic ray secondary charged particles. Also, at depths less than 30 g/cm² the observed flux variation with altitude can be described in terms of an empirical depth-dependent source function. At 3.6 g/cm² the continuum flux had a value of 0.4 count/cm² sec Mev near 1 Mev, and the deduced strength of the 0.51-Mev line was 0.10 ± 0.005 photon/cm² sec.