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- Circular-Geometry
**Oscillators**... quadrature**oscillators**... LC**oscillators**...**frequency**synthesis... voltage-controlled**oscillators**Data Types:- Document

- No abstract.Data Types:
- Document

- The behavior of spheres in non-steady translational flow has been studied experimentally for values of Reynolds number from 0.2 to 3000. The aim of the work was to improve our qualitative understanding of particle transport in turbulent gaseous media, a process of extreme importance in power plants and energy transfer mechanisms. Particles, subjected to sinusoidal
**oscillations**parallel to the direction of steady translation, were found to have changes in average drag coefficient depending upon their translational Reynolds number, the density ratio, and the dimensionless**frequency**and amplitude of the**oscillations**. When the Reynolds number based on sphere diameter was less than 200, the**oscillation**had negligible effect on the average particle drag. For Reynolds numbers exceeding 300, the coefficient of the mean drag was increased significantly in a particular**frequency**range. For example, at a Reynolds number of 3000, a 25 per cent increase in drag coefficient can be produced with an amplitude of**oscillation**of only 2 per cent of the sphere diameter, providing the**frequency**is near the**frequency**at which vortices would be shed in a steady flow at the mean speed. Flow visualization shows that over a wide range of**frequencies**, the vortex shedding**frequency**locks in to the**oscillation****frequency**. Maximum effect at the natural**frequency**and lock-in show that a non-linear interaction between wake vortex shedding and the**oscillation**is responsible for the increase in drag.Data Types:- Document

**qubit**Data Types:- Document

- NOTE: Text or symbols not renderable in plain ASCII are indicated by [...]. Abstract is included in .pdf document. Measurements of some of the properties of high-degree solar p- and f- mode
**oscillations**are presented. Using high-resolution velocity images from Big Bear Solar Observatory, we have measured mode**frequencies**, which provide information about the composition and internal structure of the Sun, and mode velocity amplitudes (corrected for the effects of atmospheric seeing), which tell us about the**oscillation**excitation and damping mechanisms. We present a new and more accurate table of the Sun's acoustic vibration**frequencies**, [...], as a function of radial order n and spherical harmonic degree l. These**frequencies**are averages over azimuthal order m and approximate the normal mode**frequencies**of a nonrotating, spherically symmetric Sun near solar minimum. The**frequencies**presented here are for solar p- and f- modes with [...], [...], and [...]. The uncertainties, [...] , in the**frequencies**are as low as 3.1 pHz. The theoretically expected f-mode**frequencies**are given by [...], where g is the gravitational acceleration at the surface, [...] is the horizontal component of the wave vector, and [...] is the radius of the Sun. We find that the observed**frequencies**are significantly less than expected for l > 1000, for which we have no explanation. Observations of high-degree**oscillations**, which have very small spatial features, suffer from the effects of atmospheric image blurring and image motion (or "seeing"), thereby reducing the amplitudes of their spatial-**frequency**components. In an attempt to correct the velocity amplitudes for these effects, we have simultaneously measured the atmospheric modulation transfer function (MTF) by looking at the effects of seeing on the solar limb. We are able to correct the velocity amplitudes using the MTF out to [...]. We find that the**frequency**of the peak velocity power (as a function of l) increases with l. We also find that the mode energy is approximately constant out to [...], at which point it begins to decrease. Mode energy is expected to be constant as a function of f if the modes are excited by stochastic interactions with convective turbulence in the solar convection zone. Finally, we discuss the accuracy of the seeing correction and a test of the correction using the 1989 March 7 partial solar eclipse.Data Types:- Document

- A theory is presented for the calculation of the velocity potential of a harmonically
**oscillating**delta wing having subsonic leading edges in a supersonic flow. The velocity potential is expanded in a power series in powers of the reduced**frequency**. Two modes of**oscillation**, plunging and pitching, are considered. For both modes the analysis is carried through the term linear in reduced**frequency**, this being generally sufficient for dynamic stability analyses. The results thus obtained for the pitching mode verify those of Miles (Ref. 9) obtained by an integral transformation of the steady-state solution. In addition, the term that is quadratic in the reduced**frequency**is presented for the plunging mode to illustrate the general procedure. Lift and pitching moment coefficients are calculated from the velocity potential and numerical results valid for low**frequency****oscillations**are presented.Data Types:- Document

- This report covers an experimental investigation of the relationship between the vortex shedding
**frequency**and self excited torsional**oscillation****frequency**for a thin airfoil. The work consisted of measurements of velocity fluctuations in the airstream in the vicinity of a wing model mounted in a wind tunnel so that it could**oscillate**about the wing axis. The velocity fluctuation measurements were made with the Wing restrained and with the wing**oscillating**at various angles of attack and wind velocities. Two distinct types of**oscillations**were found. One type was self sustaining and increased in amplitude with increasing wind velocity while the other type stopped for velocities beyond some critical value.Data Types:- Document

**Oscillator**...**Frequency**DividerData Types:- Document

- I. Plasma
**Oscillations**and Radio Noise from the Disturbed Sun. Many investigators have suggested that plasma**oscillations**in the solar corona may be the source of large bursts of radio noise in the meter wavelength region. Two aspects of this problem are considered in this report: (a) the excitation of plasma**oscillations**by directed beams of charged particles, and (b) the conversion of energy in the longitudinal plasma**oscillations**to transverse electromagnetic waves by means of random inhomogeneities in electron density. It appears unlikely that charged particles whose velocity is much less than the r.m.s. thermal velocity of the coronal electrons will excite plasma**oscillations**. Charged particles whose velocity is much greater than the r.m.s. thermal velocity excite**oscillations**in a band of**frequencies**, including**frequencies**above the local plasma**frequency**. However, qualitative arguments indicate that the noise should be concentrated in a narrow band of**frequencies**slightly below the local plasma**frequency**. Thus it is impossible to explain the Type II (slow) bursts in the manner assumed and unlikely that the Type III (fast) bursts are explainable in this manner. The transfer of energy is studied in detail and it is shown that only waves whose phase velocity is less than the directed beam of charged particles receive energy from the beam. It is shown that plasma**oscillations**radiate a small fraction of their energy if the electron density is not uniform. In particular, random fluctuations in density, of the amount expected in thermal equilibrium, cause about 10[superscript -5] of the plasma-**oscillation**energy to be radiated; the remainder is dissipated by short-range collisions. Larger fluctuations than this are likely, and hence more energy should be radiated. II. A Field Analysis of the M Type Backward Wave**Oscillator**. A field theory of electron beams focused by crossed electric and magnetic fields is given. The theory is basic to the understanding of the small signal behavior of crossed field electron devices. It is applied to explain the slipping stream, or diocotron, effect as a coupling of two surface waves of the electron beam, and to derive the start**oscillation**conditions of the M-type backward wave**oscillator**. It is found that the slipping stream effect can reduce the starting current by an appreciable factor. The results are compared with the thin beam theory which neglects space charge effects. An analysis of a loaded strip transmission line is given, from which a method of representing space harmonic slow wave circuits by a surface admittance boundary condition is obtained. Forward and backward space harmonic interaction may be treated equally well.Data Types:- Document

- Damped free
**oscillations**of the magnetization have been clearly observed at the completion of 180° flux reversal along both the easy and the hard axis in Ni-Fe thin films. The flux component perpendicular to the applied pulse field was observed using a single turn pickup loop around the film. The**frequency**of the**oscillation**was studied as a function of applied pulse field and compared with the results obtained by ferromagnetic resonance. The**frequency**of the damped free**oscillation**agreed quite well with that obtained by resonance when the**frequency**was measured after the**oscillation**had damped to small amplitude. The damping constant obtained from the decay of the**oscillation**agreed quite well with that obtained from the half-power line-width of the resonance curve. The Landau-Lifshitz equation proposed for the coherent rotation, using the value of the damping constant obtained by resonance, could describe the initial part of the magnetization reversal and the damped free**oscillation**in the films with low angular dispersion. Agreement between the experimental and the calculated transverse flux change for the entire waveform could not be obtained by using the value of damping constant obtained by resonance. The agreement was better at both higher applied field or lower anisotropy dispersion. The effect of eddy currents was negligible on the flux reversal but appeared as a slight increase of the damping constant obtained by resonance experiment.Data Types:- Document