Edna O'Connell

Bio: Edna O'Connell is an academic researcher from RAND Corporation. The author has contributed to research in topics: Planetary science & Atmospheric physics. The author has an hindex of 1, co-authored 1 publications receiving 6 citations.

Pitch Angle Distributions and Mirror Point Densities in the Outer Radiation Zone

Abstract: A method is presented for the calculation of the equatorial pitch angle distribution (unidirectional intensity distribution) of trapped radiation from the count rate of an omnidirectional detector along a line of force. An expression is derived for the calculation of the mirror point density from the equatorial pitch angle distribution. The method is applied to data obtained from the Space Technology Laboratories scintillation counter and the University of Chicago proportional counter on the Explorer VI satellite. The results from the scintillation counter show a relative absence of electrons with pitch angles of 90° during quiet periods, a sharp increase in such particles shortly after a sudden commencement magnetic storm, and restoration of the prestorm distribution at a higher intensity level after the storm. The results from the proportional counter are qualitatively similar with the exception of the apparent deficiency of 90° pitch angles during quiet periods, which does not appear.

Evidence from the Moon's Surface Features for the Production of Lunar Granites

Abstract: Abstract If tektites come from the moon, they indicate a granitic constitution for a considerable portion of the outer crust, especially if allowance is made for the chemical effects of volatilization (loss of alkalies). The evidence for granitic rocks from the morphology of the moon's surface is considered in this paper. The displacement of the center of the moon's visible face with respect to the center of mass is considered evidence of the existence of isostasy on the moon. It is shown that this displacement is not merely a limb phenomenon, amd that it is probably not explicable in terms of the kind of lumpy interior proposed by Urey to explain the differences of the moments of inertia. Evidence for characteristic granite landforms, including tholoids and laccoliths, is summarized. The possibility that the maria are produced by the fluidization of volcanic ash is considered. The transporting fluid is considered to be the contained gases as in a terrestrial ash flow. Ash flows on the earth are responsible for the emplacement of a large fraction of all volcanic ash. From a study of the physics of ash flows, it is concluded that the fluidization should be more effective on the moon. It should require only about 1 30 as much gas to transmit a given amount of rock, an amount which is well within reasonable expectations for the gas yield from the rocks. It is concluded that the morphology of the moon's surface does not contradict the notion that large amounts of acid rock are present on its surface.