An improved horn feed with two modes for shallow paraboloid antennas
Improved horn feed for shallow paraboloid antennas
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Improved horn feed for shallow paraboloid antennas
Wake analysis and correlation of wind tunnel and shallow water tow channel data
Partial differential equation solution for wind-driven circulation in shallow seas or lakes
Nonlinear spinning shallow spherical shell equations solved for equilibrium stress and displacement distributions, discussing inertia loading
Partially loaded clamped plastic shallow spherical caps collapse loads and stress and velocity distributions
Linear compressive orthotropic stability theory for shallow-stiffened cylinders
Singular solutions to concentrated loads on shallow shell equations with quadratic middle surface
Solutions for normal and tangential displacements and concentrated forces on shallow cylindrical shells
Coupled integral equations for cutouts in shallow shells
Wind tunnel investigation of static pressure distributions along cylindrical surface behind shallow, three dimensional, rearward facing step of various heights
Curvature effects on shallow shell free vibration frequencies, solving linear eigenvalue problem
Symmetric and asymmetric dynamic buckling of shallow elastic arches under uniform loads, using nonlinear finite difference method
Main sequence A and early F stars with shallow convective envelopes, investigating particle diffusion effects on element abundance data
Spinning centrally clamped thin shallow spherical shell free vibration numerical analysis by considering perturbation about equilibrium configuration
Possible Earth reentry simulation of shallow-angle (3 to 30 deg) Jupiter entry was investigated in terms of four parameters of the bow shock layer ahead of a blunt vehicle: peak (equilibrium) temperature, peak pressure, peak inward radiative flux, and time-integrated radiative flux. It is shown that simulation ranging from fair to good can be achieved. Reentry is easiest (lowest Earth reentry speed) at steep Earth reentry, in the Earth entry speed range of 15 to 22 km/sec, for both the Jupiter nominal and cool atmospheres. Increased Earth speed is required, generally, for increasing Jupiter entry angle, and for increasing temperature, radiative flux, time-integrated flux and pressure, in that order.
A technique is given for obtaining exact analytical solutions for wind-driven currents in a shallow lake or sea with a large class of bottom topographies which may or may not contain an island. Welander's second-order partial differential equation for the lake's surface displacement is used for determining the lake circulation. The technique, together with some results based on conformal mapping, is used to reduce the problem of finding solutions to Welander's equation for a closed body of water to the problem of solving an ordinary differential equation. The method is applied to an elliptically shaped lake and a circular lake containing an eccentrically located circular island.
The capability of shallow-notched, round-bar, tensile specimens for screening critical environments as they affect the material fracture properties of the space shuttle main engine was tested and analyzed. Specimens containing a 0.050-inch-deep circumferential sharp notch were cyclically loaded in a 5000-psi hydrogen environment at temperatures of +70 and -15 F. Replication of test results and a marked change in cyclic life because of temperature variation demonstrated the validity of the specimen type to be utilized for screening tests.
Data relevant to the shallow structure of the moon obtained at the Apollo seismic stations are compared with previously published results of the active seismic experiments. It is concluded that the lunar surface is covered by a layer of low seismic velocity which appears to be equivalent to the lunar regolith defined previously by geological observations. This layer is underlain by a zone of distinctly higher seismic velocity at all of the Apollo landing sites. The regolith thicknesses at the Apollo 11, 12, and 15 sites are estimated from the shear-wave resonance to be 4.4, 3.7, and 4.4 m, respectively. These thicknesses and those determined at the other Apollo sites by the active seismic experiments appear to be correlated with the age determinations and the abundances of extralunar components at the sites.