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Instrument consists of base, vernier height gauge, sliding block, and balance-beam assembly with tension weight. Pulley bracket is provided with three pulley mounting holes, 4 inches apart, to accommodate widely different belt lengths. Instrument is accurate to within 0.001 inch and is suitable for commercial production.
Photographs taken with the Catalina 61-inch reflector from June 21 through July 10, 1971 have enabled the author to study and measure the early developments of a major South Equatorial Belt (SEB) disturbance. High-resolution photographs of the disturbance were obtained on seven nights during the 19-day interval. Our first photograph at 04:38 UT on June 21 recorded the initial outbreak at 79.5 deg longitude (System II), and -14 deg zenographic latitude. From this point, dark spots moved along the SEBs towards increasing longitude, and white spots a short distance along the SEBn towards decreasing longitude.
Some aspects of the major South Equatorial Belt disturbance of 1971 are described from photographic observations obtained at the Catalina and Bosscha Observatories. The motions of several spots produced by the disturbance during the first two months of activity were measured. The projection comparator used for measurement is also described.
An outbreak of thirteen spots in Jupiter's North North Temperate Belt Current B was observed in 1972. These have been measured and compared with measures of the two most previous outbreaks. The drift in longitude of a hypothetical source supports both Reese's original hypothesis of a subsurface source, and Solberg's observation that its period is close to that of System III. There is some evidence that long-enduring atmospheric features exist at lower, unobservable depths.
The author has identified the following significant results. Geological correlation of terrain across the Gulf of California using ERTS-1 imagery revealed significant similarities between Isla Tiburon, Isla Angel de la Guarda, and the San Carlos Range in mainland Mexico. ERTS-1 imagery was used to check the validity of the existence of major trans-Baja fault zones. ERTS-1 imagery also shows that high albedo sediments similar to known late Tertiary marine sediments are widespread in southern and middle Baja and extend in places to the eastern side of the Peninsula. Major faults in northern Mexico and across the border in the United States were mapped, and ample evidence was found that the Parras and parts of the Texas lineament are belts of major transverse shear faults in areas outside the supposed limit of the Texas and Parras lineaments. A fundamental concept which may help explain many complexities in the tectonic development is beginning to emerge: The southwestern part of North America was torn by massive left-lateral shear of transverse trend (east-west) during the compressive stage of the late Mesozoic and early Cenozoic. This tectonic style has changed into tensional rifting (Basin and Range) and right-lateral shear later in the Cenozoic and Quaternary.
Photographs taken with the Catalina 61-inch reflector from June 21 through July 10, 1971 have permitted study and measurement of early developments of a major South Equatorial Belt (SEB) disturbance. High resolution photographs of the disturbance were obtained on seven nights during the 19-day interval. The first photograph at 04:38 UT on June 21 recorded the initial outbreak at 79.5 deg longitude (System 2), and -14 deg Zenographic latitude. From this point, dark spots moved along the SEBs towards increasing longitude. The preceding white spot had an initial period of 9h54m32.5 tor-3.5s, and retrograding dark spots on the SEBs a mean period of 9h58m30s.5 tor- 7s. The feature from which all the spots emerged had a rotation period of 9h55m29s tor- 2.5s, and is close to the System 3 radio period of 9h55m29.73s tor- 0.04s derived by Carr.
Some aspects of the major South Equatorial Belt disturbance of 1971 are described from photographic observations obtained at the Catalina and Bosscha Observatories. The motions of several spots produced by the disturbance during the first two months of activity were measured. The projection comparator used for measurement is also described.
An outbreak of thirteen spots in Jupiter's North North Temperature Belt Current B was observed in 1972. These have been measured and compared with measures of the two most previous outbreaks. The drift in longitude of a hypothetical source supports both Reese's original hypothesis of a subsurface source, and Solberg's observation that its period is close to that of System 3. There is some evidence that long-enduring atmospheric features exist at lower, unobservable depths.
Pioneer 10 counted relativistic electrons throughout the magnetosphere of Jupiter, with the greatest fluxes being inside 20 Jupiter radii. The peak flux of electrons with energy greater than 50 MeV was 13 million per square centimeter per second at the innermost penetration of the radiation belts.
The diffusion theory of inner belt protons is extended to lower energies for comparison with the data of Hovestadt et al. The effects of Coulomb energy loss, nuclear inelastic scattering, and the secular decrease of the earth's magnetic field are included. The Farley and Walt solar cycle averaged atmosphere and a neutron source based on the most recent measurements are used. It is found that diffusion theory can account for the observed flux of low-energy protons provided that the diffusion coefficient increases at smaller values of the first invariant. This result is interpreted as additional evidence for the importance of electrostatic field fluctuations in causing radial diffusion.
The University of California at San Diego trapped radiation detector measured proton and electron fluxes, angular distributions, and energy spectra throughout the Pioneer 10 fly by of Jupiter in December 1973. The instrumentation and calibrations are described, and good values for particle fluxes in the inner and outer regions are presented. The major features of the Jovian radiation belts are described, with preliminary discussions of their meanings.
The near-earth charged particle environment is discussed in terms of spacecraft design criteria. Models are presented of the trapped radiation belts and based on in-situ data obtained from spacecraft.
Models of Jupiter's radiation belts have been constructed to determine the distribution of particles and their energies which will produce the observed decimetric radio emission. Data on the spectrum and the variation of emission with Jovian longitude have been used to show that the relativistic particles have a nearly isotropic distribution with high energies (of order 100 MeV) within 2 Jovian radii and a very flat distribution in the equatorial plane of low energy particles further out in the magnetosphere. Subtraction of the emission predicted by this model from the total radio emission shows that the thermal contribution in the frequency range between 3000 and 10,000 MHz is somewhat less than had been previously expected. (The brightness temperature of the planetary disk is 180 K at 3,000 MHz, for example.) This suggests that the ammonia mixing ratio in Jupiter's upper atmosphere may be as high as 0.002.
Detailed Explorer 45 observations of quiet time pitch angle distributions and equatorial radial profiles of energetic radiation belt electrons are presented. The observed pitch angle distributions in the slot region and the outer regions of the plasmasphere are found to agree with the values expected from resonant interactions with the plasmaspheric whistler mode wave band, and Coulomb collisions are found to be the dominant electron loss mechanism in the inner zone. The overall structure of quiet time radial profiles is shown to agree with the equilibrium structure expected to result from a balance between pitch angle scattering losses and radial diffusion from an outer zone source, and this agreement suggests that the dominant quiet time source and loss mechanisms have been correctly identified. Electron fluxes in the inner plasmasphere are found to remain nearly constant during the quiet periods due to their decoupling from magnetic activity variations in the outer plasmasphere.
Predictions of theoretical models of Jupiter's radiation belts are compared with Pioneer 10 measurements. A brief quasi-historical review is given of the evolution of the basic theoretical ideas with emphasis on the three physical processes that were believed to be dominant in the Jovian electron fluxes: radial-diffusion transport, limitation of particle fluxes by plasma wave turbulence, and particle losses from collisional sweep-up by the Galilean satellites. Pioneer 10 data on the inner zone are discussed which yield the clearest evidence for radial diffusion being the dominant transport process, the synchrotron flux density is estimated using Pioneer 10 measurements, and the observed outer-zone electron fluxes are favorably compared with the qualitative and quantitative predictions of the whistler-mode stable-trapping model. The outer-zone electron-precipitation flux is estimated, and it is suggested that precipitation could affect the structure of the Jovian ionosphere. Satellite sweep-up is shown to be less severe than had been anticipated.
Detailed Explorer 45 equatorial observations of the storm and poststorm structure of radiation-belt electrons (35 to 560 keV) for L values between 1.7 and 5.2 are presented. Injection during major storms results in electron pitch-angle distributions and radial profiles that are greatly distorted from their quiet-time equilibrium structure. Following storms, the pitch-angle distributions return to their prestorm shape over a period of several days. This shape is maintained as electron fluxes decay back to the quiet-time levels. The equatorial radial profiles slowly return to their prestorm equilibrium structure over a period of a few weeks and then maintain that structure.
This paper describes the environmental models of the radiation belts and computational techniques which have been developed for predicting the radiation hazards for spacecraft. These data and techniques are then applied to the Atmosphere Explorer 51 spacecraft to explain its successful survival for more than 18 months in a severe environment. In particular, the results of the analysis are used to explain the performance of some 2400 CMOS devices, and consequently, they demonstrate the reliability of this device technology in spacecraft systems.
Far-ultraviolet imagery of the earth in the wavelength ranges from 1050 to 1600 A and from 1250 to 1600 A was obtained from the lunar surface during the Apollo 16 mission on Apr. 21, 1972. The images have an angular resolution of about 2 arcmin (230-km linear resolution) and have been quantitatively analyzed to obtain absolute intensities and spatial distributions of the polar auroras (both wavelength ranges), the day and night airglow, and tropical airglow belts (1250-A to 1600-A wavelength range). The observations are consistent with previous results obtained from the OGO-4 spacecraft, but they have also provided details on the spatial distributions of the various emissions over an entire hemisphere at a single time. A general night airglow, at least in the Northern Hemisphere, is indicated.