No abstract

Results obtained from the electron detector on Telstar between July 10 and 31, 1962, are presented. The principal sensitivity of the detector is to electrons of energies between 0.25 and 1.0 Mev. Flux maps have been drawn for days 193–197, 203–207, and 208–212, 1962. Maximum omnidirectional electron fluxes of approximately 109/cm2 sec were encountered with energies in excess of 200 kev near the magnetic equator at L's of about 1.25 and 1.8Re. The intensity decreased exponentially with a time constant of about 4.5 days between L values of 2.2 and 3.0, and with a time constant of about 15 days at L = 2.0 and 3.5, creating a slot be tween the inner and outer electron belts that had become pronounced by the end of July. The energy spectrum encountered seems to contain a substantial number of electrons with energies of about a Mev or more and is not inconsistent with the fission β spectrum above 400 kev. At lower energies the spectrum is steeper. Within the sensitivity of the measurement no spectral changes with either position or time were observed. Because of Telstar's launch date it is not possible to conclude what fraction of the electrons measured were produced by the high‐altitude nuclear test of July 9. In spite of the high flux of electrons encountered, electrons are not the major source of radiation damage to the Telstar solar power plant.

This paper contains a statistical summary of the 14,000,000 measurements taken during 27 rainfalls in a six‐month period in 1967 from a 96‐station, rapid‐response rain guage network spread over a rectangular area 13 by 14 kilometers centered near Crawford Hill, New Jersey. The analysis emphasizes rain rates greater than 50 millimeters per hour, which interfere with radio transmission in the 10 to 30 GHz frequency range. Heavy rain rates are relatively rare events, come in irregular bursts, and do not appear amenable to description by simple analytic distributions. This paper presents statistics concerning the behavior of rain rates at a point in space, the relationship of rain rates separated in space or time, and the relationship of average rain rates on pairs of paths in various configurations.

The data from the particle experiments of the Telstar satellite have been analyzed to provide maps of the distribution of electrons and protons as measured in three of the Telstar detectors during the period from July through October, 1962. For the protons between 26 and 34 Mev and >50 Mev, the particle distributions are stable in time, but for the electron distribution there is a time decay of the electron flux over most of the region explored by the Telstar orbit. The connection of these observations to the high‐altitude nuclear explosion of July 9, 1962, is discussed. The introduction of additional electrons by Russian tests at the end of October was also observed. The particle maps have been used to derive the integral particle exposure of the satellite, which is found to account quantitatively quite well for the radiation damage observed in the main solar power plant and in the radiation damage experiments on solar cells and special damage transistors carried by the satellite. In the main power plant the proton and electron contributions to damage are found to be equal. The integral particle exposure has also been used to compute the level of ionization in different depths of material in order to evaluate the degradation of semiconductor devices in the Telstar canister.

Refractive-index dispersion data for 11 I-III-VI2 and II-IV-V2 chalcopyrite semiconductors are analyzed with a view towards obtaining a good representation of the data, values of physically meaningful parameters, and estimates of errors. Using a moment decomposition analysis, it is found that (i) only four parameters (three electronic and one lattice) are required to fit each dispersion curve, (ii) all differences between chalocopyrites and their zinc-blende binary analogs can be viewed as simple band-gap-shift effects, (iii) in contrast to cuprous halides, oscillator strength contributions from d-electron valence states in Cu and Ag chalcopyrites appear to be negligible, (iv) energy downshifts in chalcopyrites involve the entire ε2 spectrum, and (v) there is no clear quantitative correlation between structural distortions in chalcopyrites and anisotropies in optical parameters related to the birefringence. Finally, a brief discussion of the applicability of model ε2 spectra to descriptions of refractive-index dispersion and related optical effects is presented.