Stage sizing data for an unmanned planetary sample return mission, task E-94 Project technical report
Outbound and inbound stage weight requirements for planetary sample return mission payload and energy requirements - graphs
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Outbound and inbound stage weight requirements for planetary sample return mission payload and energy requirements - graphs
Application of VHF Doppler tracking data from Goddard Range and Range Rate system to determine lunar orbits for Explorer 35 satellite
Clear air turbulence pulse Doppler laser radar design including analysis of mechanical vibration effects on laser transmitter and reciever
Predictions and recommendations for development and deployment of manned space stations
Application of spacecraft technology to aircraft for improvement in systems, materials, and performance
Sketch map of proposed Descartes Apollo 16 lunar landing site
Equatorial D region positive ion composition studies by rocket payloads
Bibliography of publications and compilation of abstracts on Explorer 33 and 35 satellites
Directional differential energy spectra for proton intensities in outer radiation zone near magnetic equator from satellite observations
Energetic electrons distribution in magnetotail plasma sheet from Explorer 35 satellite observation data
Energetic electrons in magnetospheric tail plasma sheet, investigating flux time profiles and correlation with local magnetic fields from Imp 3 satellite observation data
Accelerated procedures for Markov chain model optimal control problems solution with computation time advantage over usual dynamic programming
Critique of paper on Apollo 11 ilmenite basalts petrology and lunar bodies origin and form
Positive-ion and electron densities were measured in the 75 to 110 km altitude range with the aid of two rockets launched from White Sands near sunrise. The solar zenith angles were 91 and 79 deg respectively. The densities were derived from measurements made by an ion collector and from data obtained with a Faraday rotation technique capable of detecting electrons in the D-region. It has been found that in the 80-95 km altitude range, electron detachment from negative ions takes place mainly at zenith angles of less than 91 deg. The source of the high positive-ion density (N(+) approximately 700/cu cm) at an altitude of 75 km just before sunrise is presumed to be scattered Lyman alpha radiation which is ionizing nitric oxide.
Evidence for negative ions in the lower ionosphere is based on the difference between simultaneously measured profiles of electron and positive ion density. The electron density profiles reported were obtained from ground-to-rocket radio wave absorption measurements while Gerdien ion traps were used to measure the positive ion profiles. Results from a series of three rockets launched from Thumba, India near sunset on 27 March, 1970 indicate that a significant number of negative ions are formed at altitudes as high as 95 km at twilight.
An analysis of the combustion products resulting from the solid propellant rocket engines of the space shuttle booster is presented. Calculation of the degree of pollution indicates that the only potentially harmful pollutants, carbon monoxide and hydrochloric acid, will be too diluted to constitute a hazard. The mass of products ejected during a launch within the troposphere is insignificant in terms of similar materials that enter the atmosphere from other sources. Noise pollution will not exceed that obtained from the Saturn 5 launch vehicle.
High resolution panoramic photographs taken from 110 km orbits of the command service module show the lunar module structure on the moon as evidenced by reflected light and by the shadow. Before and after photographs of the landing site are presented; the increased brightness or halo is attributed to mare surface materials.
From the data on solar protons with energy 0.3 MeV obtained by Explorer 35 since July 1967, ten events were selected for the study of intensity vs time and of angular distributions of intensity in interplanetary space near the earth. The bases of selection were that the events be of adequate intensity for statistically satisfactory study and that they be attributable to a single solar flare so that their time histories were not complicated by overlapping emissions of particles. The principal findings for these events are presented.