Operations of V/STOL aircraft in the terminal area
Terminal area operations of V/STOL aircraft, considering approaches, approach speeds, wind and velocity effects and noise
Garren, J. F. JR.↗
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Temporal evolution of velocity structures in the solar wind
Generally poor correlations were obtained of solar wind flow speed measurements at one point in the ecliptic plane with measurements at the same point 28 days (one solar rotation) earlier or with measurements at other points in the ecliptic plane separated by 50 deg or more in solar longitude. This is evidence that either the flow speed is a very sensitive function of solar latitude or that temporal processes typically alter the speed of the wind emanating from particular solar regions on a time scale of about 4 days. From a measure of the persistence of the flow speed at the orbit of the earth, it appears that the temporal explanation is more likely to be the correct one.
Gosling, J. T.↗
Comment on the large velocity discontinuities in the solar wind
Ivanov (1970) showed that rotational discontinuities can exist in an anisotropic medium, and claimed that 10 of the 11 discontinuities examined by Burlage (1969) are rotational in Hudson's sense. Using Hudson's (1970, 1971) data, it is argued that at least 5 of the 10 discontinuities are of the tangential and not rotational type. This supports Burlaga's interpretation, according to which there exist tangential discontinuities characterized by large shifts.
Burlaga, L. F.↗
On the relation between solar wind structure and solar wind rotational and tangential discontinuities.
Solar wind plasma and magnetic field data were used to identify rotational and tangential discontinuities during the first 40 days of the flight of Mariner 5. Of the 40 rotational discontinuities found, 36 were clustered in three distinct 3- to 6-day intervals. These three intervals were characterized by high solar wind bulk velocities, high magnetic field magnitudes, low densities, high correlation between velocity and magnetic field changes, and the presence of smooth Alfven waves. The rotational discontinuities had magnetic field changes that were generally close to the direction of magnetic field changes for smooth Alfven waves. Although the primary component of these changes was perpendicular to the equatorial plane for both, the radial component for the discontinuities was generally larger. The normals to the tangential discontinuity surfaces strongly preferred a direction near the ecliptic plane and perpendicular to the spiral field direction.
Turner, J. M.↗
Effects of electrostatic instabilities on planetary and interstellar ions in the solar wind.
It is shown that newly born ions in the solar wind result in unstable electrostatic waves propagating parallel and perpendicular to the interplanetary magnetic field. A description of the longitudinal instability is followed by a discussion of its implications for assimilating newly born ions of interstellar and planetary origin into comotion with the solar wind bulk velocity. The transverse electrostatic instability is then considered and it is shown that its growth rate is of the same order as that for transverse electromagnetic instabilities found by Wu and Davidson (1972).
Hartle, R. E.↗
Wind tunnel investigation of a large-scale model of a lift/cruise fan V/STOL aircraft
An investigation was conducted in the Ames 40- by 80-Foot wind tunnel to determine the aerodynamic characteristics of a large scale model of a lift/cruise fan V/STOL aircraft. The model was equipped with three fans, one mounted in the forward section of the fuselage in a lift mode, and two mounted on top of the wing adjacent to the fuselage in a lift/cruise mode. The data that were obtained include longitudinal and lateral-directional characteristics of the model, with the horizontal tail on and off, for both the Powered lift and cruise configurations. Powered lift data were obtained at several wind tunnel velocities and at several lift/cruise fan thrust vector angles by varying the position of the hooded deflectors from 0 deg. (the cruise condition) to 90 deg.
Gambucci, B. J.↗
Evidence for mass loss at moderate to high velocity in Be stars
Ultraviolet spectra of intermediate resolution have been obtained with Copernicus for 12 objects classified as Be or shell stars and for 19 additional early B dwarfs. Some of these spectra show marked asymmetries in certain resonance lines, especially the Si IV doublet at 1400 A, indicating the presence in some cases of outflowing material with maximum velocities of nearly 1000 km/s. Direct evidence for mass loss at these velocities is seen for the first time in dwarf stars as late as B1.5; the only objects later than B0.5 which show this effect are Be or shell stars. Among the stars considered, there is a correlation between the presence of mass-loss effects and projected rotational velocity, suggesting that the ultraviolet flux from B1-B2 dwarfs is sufficient to drive high-velocity stellar winds only if rotational effects reduce the effective gravity near the equator. The mass-loss rate for one of the most active Be stars, 59 Cyg, is crudely estimated to be one billionth or one ten-billionth of a solar mass per year. The data suggest that the extended atmospheres associated with Be-star phenomena may be formed by mass ejection.
Snow, T. P., Jr.↗
Wind-tunnel investigation of a large-scale model of a lift-cruise fan V/STOL aircraft with extended lift-cruise nacelles
The aerodynamic characteristics of a large-scale model of a lift/cruise fan V/STOL aircraft were determined. The model was equipped with three fans, one mounted in the forward section of the fuselage in a lift mode, and two mounted on top of the wing adjacent to the fuselage in a lift/cruise mode. The data that were obtained include longitudinal and lateral-directional characteristics of the model, with the horizontal tail on and off, for both the powered-lift and cruise configurations. Lateral-directional characteristics were obtained with the horizontal and vertical tail sections removed. Powered-lift data were obtained at several wind-tunnel velocities and at several lift-cruise fan thrust vector angles by varying the position of the hooded deflectors from 0 deg (the cruise condition) to 90 deg.
Gambucci, B. J.↗
A survey of mass loss from Be and shell stars using ultraviolet data from Copernicus
Ultraviolet spectra of intermediate resolution have been obtained with Copernicus of twelve objects classified as Be or shell stars, and an additional 19 dwarfs of spectral classes B0-B4. Some of these spectra show marked asymmetries in certain resonance lines, especially the Si IV doublet at 1400 A, indicating the presence of outflowing material with maximum velocities of nearly 1000 km/sec. Direct evidence for mass loss at these velocities is seen for the first time in dwarf stars as late as B1.5. Later than B0.5, the only survey objects showing this phenomenon are Be stars. Among the stars considered there is a correlation between the presence of mass-loss effects and projected rotational velocity, suggesting that the UV flux from B1-B3 dwarfs is sufficient to drive high-velocity stellar winds only if rotation reduces the effective gravity near the equator. The role of mass-loss in producing the Be star phenomenon and the effects of rotation on mass loss are discussed.
Marlborough, J. M.↗
A reexamination of two-fluid solar wind models
The two-fluid solar-wind equations have been solved by a method which is approximately 50 times faster than any previously developed, through the use of asymptotic expansions which are self-consistently iterated upon to find a solution that passes through the critical point. The energy assumptions in two-fluid solar-wind models are reexamined, and the conclusions are as follows: (1) proton thermal conduction may not be neglected, (2) the Coulomb logarithm must be calculated as a function of radius, and (3) the electron and proton temperatures at the base need not be equal, even when the time scale for energy exchange between the species is an order of magnitude smaller than the expansion time at the base. It is possible to reproduce reasonable quiet-time solar-wind parameters at 1 AU, but only if the proton temperature is approximately twice the electron temperature at 1 solar radius. This may indicate that extended proton heating is important in the outer solar corona. Winds with velocities at 1 AU of 450 km/s are generated without nonthermal energy deposition but require high proton temperatures as well as very low densities at the base. Higher-velocity solutions are not possible in a spherically symmetric geometry for reasonable particle fluxes at 1 AU, and it is suggested that these higher-velocity states probably require additional heating, acceleration mechanisms, or nonradial flow.
Nerney, S.↗
X-ray transfer in binary systems - A Monte Carlo study
Results are presented for Monte Carlo calculations of X-ray light curves for binary systems surrounded by clouds with simple density distributions, chemical compositions, and ionization structures. Occultation of the X radiation by the companion star is taken into account along with Compton scattering and photoionization within the clouds. The models are used to examine the effect of various cloud geometries and ionization structures on the emergent X-ray flux as a function of orbital phase and X-ray energy. The results demonstrate the sensitivity of observed light curves and phase-dependent spectra with respect to the optical depth, geometry, and ionization structure of a surrounding cloud for the cases of a uniform-density cloud with a radius four times the binary orbital separation, a steady-state constant-velocity stellar wind emanating from the companion star, and a spherically symmetric shell or 'cocoon' of the type proposed for Cyg X-3. It is concluded that X-ray binary systems are unlikely to be surrounded by obscuring clouds.
Hertz, P.↗
Solar-powered aircraft
Solar-powered aircraft, driven by electric motor, has vertical and horizontal wings. Design allows aircraft to fly straight path while banked, permitting optimal exposure of its wing-mounted solar cells to Sun. Such aircraft would fly at altitude high enough to be above clouds and to avoid winds with velocities much greater than its own airspeed. Its most likely application would be as pilotless aircraft to take advantage of its ability to remain aloft for long periods (for very long flights).
Phillips, W. H.↗
Pulsed Doppler lidar for the detection of turbulence in clear air
A pulsed C02 Doppler lidar system is described and demonstration tests in ground-based and airborne flight operations are discussed. As a ground-based system, it can detect wind shears in thunderstorm gust fronts to a range of 6 km. When in the airborne configuration, the lidar can detect clear air turbulence in advance of the aircraft encountering clear air turbulence. The data provided by the lidar included turbulence location and intensity with intensity being indicated by the measured spectral width which is proportional to the wind gust velocity.
Weaver, E. A.↗
Lower hybrid waves in the solar wind
It is demonstrated that the frequently observed broad band low frequency electrostatic noise in the solar wind generally has a dominant lower hybrid component. These modes are probably produced by the anisotropic halos of the solar wind electron velocity distributions exhibiting 'heat flux' profiles and thus, are accompanied by broad band, 'hybrid-like' whistler waves. When the electron temperature is much larger than the ion temperature, these modes can also co-exist with the ion acoustic waves. Since lower hybrid modes propagate nearly normal to the interplanetary magnetic field lines, the ions can be transversely accelerated by these waves and attain the observed anisotropic and/or loss-cone-like distributions.
Marsch, E.↗
Infrared photometry of O stars
The results of a survey of 50 O stars in the J, H, K, L, and M bands are described. The observations are described, and the fitting of reddening relations to them is discussed. The zero points in the reddening relations are related to the intrinsic colors of the samples of normal stars, and these are compared with theoretical colors. The comparison reveals anomalies at L and M, which are discussed. The residuals for an individual star from the reddening relations are a measure of its infrared excesses, if indeed it has any. How the excesses can be fitted to a stellar wind model to derive a parameter that involves the rate of mass loss in the wind, the stellar radius and temperature, and wind terminal velocity is considered. The results for a number of individual stars are discussed and compared with other mass loss measurements, and it is concluded that no single model is capable of reconciling the IR, UV, radio, and H-alpha observations for the stars.
Castor, J. I.↗
Radial evolution of ion distribution functions
A survey of solar wind ion velocity distributions and derived parameters (temperature, ion differential speed, heat flux, adiabatic invariants) is presented with emphasis on the heliocentric distance range between 0.3 and 1 AU traversed by the Helios solar probe. The radial evolution of nonthermal features are discussed which are observed to be most pronounced at perihelion. Within the framework of quasilinear plasma theory, wave particle interactions that may shape the ion distributions are considered. Some results of a self consistent model calculation are presented accounting for ion acceleration and heating by resonant momentum and energy exchange with ion cyclotron and magnetosonic waves propagating away from the Sun along the interplanetary magnetic field. Another tentative explanation for the occurrence of large perpendicular proton temperatures is offered in terms of heating by Landau damping of lower hybrid waves.
Marsch, E.↗
X-rays from Eta Carinae
X-ray observations of Eta Car obtained with the high-resolution imager and solid-state spectrometer of the Einstein observatory are reported and interpreted in terms of a two-shell model. A soft component with temperature 5 million K is located in the expanding outer shell, and the hard core component with temperature 80 million K is attributed to the interaction of a high-velocity stellar wind from the massive central object with the inner edge of a dust shell. Model calculations based on comparison with optical and IR data permit estimation of the mass of the outer shell (0.004 solar mass), the mass of the dust shell (3 solar mass), and the total shell expansion energy (less than 2 x 10 to the 49th ergs).
Chlebowski, T.↗
Gas exchange and CO2 flux in the tropical Atlantic Ocean determined from Rn-222 and pCO2 measurements
The piston velocity for the tropical Atlantic Ocean has been determined from 29 radon profiles measured during the TTO Tropical Atlantic Study. By combining these data with the pCO2 data measured in the surface water and air samples, the net flux of CO2 across the sea-air interface has been calculated for the tropical Atlantic. The dependence of the piston velocity on wind speed is discussed, and possible causes for the high sea-to-air CO2 flux observed in the equatorial zone are examined.
Smethie, W. M., Jr.↗