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Auroral electrons temporal and spatial structure from ground based optical observations and rocket- borne electron detector measurements

Rocket measurements of primary auroral particles energy spectra indicating spectral structure acceleration peaks associated with electrostatic fields

Visual aurora produced by energetic electrons

High latitude electron bursts observed by OGO 4, postulating electric field acceleration mechanism beyond 3 earth radii for ambient thermal plasma electrons

Energy spectrum fine structure of low energy auroral electrons

Rocket studies of energy spectra of primary auroral electrons, giving model for auroral display

Monoenergetic electron flux associated with prebreakup auroral display observed with rocket- borne instruments, discussing origin and acceleration mechanisms

Field aligned electron bursts at high latitudes observed by polar orbiting satellite OGO-4

Energy spectra of primary auroral electrons energized by electric field

Near monoenergetic beam of electrons associated with auroral display

Temporal periodicity of 10 cps observed in flux of auroral electrons by rocketborne radiation detectors

Program providing man-machine communication for electronic circuit analyses using time sharing computer

Rocket observations of energy spectra of auroral electrons

Program for on-line analysis of nonlinear electronic circuits written in AED language and operated on Compatible Time Sharing System

Rocket and satellite observations of low energy auroral electrons and other activity

Rocket measurements of energetic electron precipitation in auroral zone

Windowless continuous-channel electron multiplier detecting low energy charged particles in space

Low energy charged particle detection with continuous channel electron multiplier

The charged particle observations proposed for the new low altitude weather satellites, TIROS-N, are described that will provide the capability of routine monitoring of the instantaneous total energy deposition into the upper atmosphere by the precipitation of charged particles from higher altitudes. Estimates are given to assess the potential importance of this type of energy deposition. Discussion and examples are presented illustrating the importance in distinguishing between solar and geomagnetic activity as possible causative sources.

The low-energy electron experiment will provide differential measurements of the energy influx and angular distributions of electrons and protons on the Atmosphere Explorer-C and -D missions. The detectors consist of cylindrical electrostatic analyzers for species and energy selection and Spiraltron electron multipliers as particle sensors. The C version will contain three detectors, two measuring electrons and protons from 0.2 to 25 keV in 16 logarithmically spaced steps and one measuring 5 keV electrons continuously. Angular distributions will be acquired utilizing the spin of the spacecraft. The D version will contain 19 detectors, one proton-stepped energy analyzer, and two electron-stepped energy analyzers at two different angles, again over the energy range 0.2 to 25 keV.

Analysis of an occultation reappearance of the semiregular variable X Cancri observed with the 107-inch telescope of McDonald Observatory on 9 November 1971 by the laser group using slightly modified laser equipment. The problem of the effective temperature of this carbon star is discussed, and estimates near 2500 K are derived both from the occultation data and from an integration based on the multicolor photometry reported by Mendoza (1967). This figure is 300-400 K higher than Mendoza's calibration, and it is clear that unsolved problems remain in many areas connected with these stars.

The low energy electron experiment (LEE) will provide differential measurements of the energy influx and angular distributions of electrons and protons on the Atmosphere Explorer C and D missions. The detectors consist of cylindrical electrostatic analyzers for species and energy selection and Spiraltron electron multipliers as particle sensors. The C version will contain three detectors measuring the two species from 0.2 to 25 keV in 16 logarithmically spaced steps, and 5 keV electrons continuously. Angular distributions will be acquired utilizing the spin of the spacecraft. The D version will contain 19 detectors, one proton stepped energy analyzer and two electron stepped energy analyzers at two different angles, again over the energy range 0.2 to 2.5 keV. In addition it will contain 16 fixed energy detectors which will obtain high-time-resolution angular distributions in the spacecraft 1 RPO mode at 5 energies between 0.2 and 5 keV. Increase of these energies by a factor of 3.5 will be possible by ground command.