O /super 1 D/ quenching in the ionospheric F- region.
Oxygen collisional quenching rate in F region determined by comparing nightglow intensities with intensities calculated from electron density profiles
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Oxygen collisional quenching rate in F region determined by comparing nightglow intensities with intensities calculated from electron density profiles
Rocket measurement techniques for electron density profiles in D region, giving results from auroral zone disturbed and midlatitude quiet D region
S band occultation experiment for Mariner Mars 1971 orbiters, measuring atmospheric density and ionospheric electron density profiles
Nighttime E region structure variations observed by Wallops Island rocket flights, obtaining electron density profiles by Langmuir probe during ascent
D region electron density profiles during solar eclipse from X ray rocket and satellite observations
On-line closed loop processor for reducing topside ionograms to electron density profiles
A high-altitude electrostatic probe experiment is described and data are presented for three RAM C reentries at velocities of approximately 25 OOO feet per second. The electron density profiles inferred from the probe measurements are compared with theoretical calculations, and the probable cause of significant disagreement is briefly discussed. Probe measurements during material-addition sequences for radio-blackout alleviation are presented, and comparisons of probe measurements with other pertinent diagnostic measurements are made.
RAM C-3 S band diagnostic antenna systems and calculations of electron density profiles
Electron density profiles in plasma ahead of shock waves determined with electrostatic probes in shock tubes
Antenna radiation patterns and electron density profiles in turbulent plasma flow
Jicamarca radio observations of temperature and electron density profiles, films of Spread F structure, and nightglow emission intensities
Electron density profiles in supersonic plasma jet, using immersed microwave probe
Neutral wind effects on redistribution of E region ionization and recombination, comparing electron density profiles to vertical ion drift velocities
Martian lower ionospheric models during solar proton event, determining electron density profiles
Online data collection of the amplitudes of circularly polarized radio waves, partially reflected from the D region of the earth's ionosphere, has enabled the calculation of an electron-density profile in the height region 60-90 km. A PDP 15/30 digital computer with an analog to digital converter and magnetic tape as an intermediary storage device are used. The computer configuration, the software developed, and the preliminary results are described.
An attempt is made to establish an ionization source capable of maintaining the nighttime Venus ionosphere. The corpuscular ionization and heating caused by the penetration of solar wind plasma into the nightside ionosphere was suggested as a possible source. Theoretical tests, using an interacting solar wind model, were made of the electron density and the results compared with observed electron density profiles. Results indicate the solar wind could maintain the nighttime ionosphere of Venus.
20 MHz radio signals have been received during the day from satellite Beacon-B when it was below the optical horizon by using a bank of narrow filters to improve the signal to noise ratio. The Faraday fading rate becomes constant, under these conditions, at a level determined by the plasma frequency just below the F-layer peak. Variations in the Faraday fading rate reveal fluctuations in the electron density near the peak, while the rate of attaining the constant level depends on the shape of the electron density profile.
Simultaneous airglow and electron content measurements made at Hawaii are used to infer the number of 6300 and 6364 A quanta produced per electron lost in the nighttime F layer of the ionosphere. The equation of continuity of electrons is then solved numerically to obtain the electron density profile, and the amount of quenching is estimated. This leads to the number of excitations of O(super-1 D) per O2(+) recombination (epsilon). We find, for an exospheric temperature of 1100 K, epsilon is equal to 1.1 plus or minus 0.6, in good agreement with Zipf's laboratory measurement at 300 K.