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NASA NTRS1975

Practical aspects of plasma processes in thermionic energy converters

Over a decade of cesium vapor thermionic converter research has yielded sufficient understanding of the basic plasma processes to permit application of this understanding to improvement of converter performance. A performance index is defined which relates such converter improvements directly to increases in system performance. A prime practical objective of current research is to reduce or eliminate the arc potential drop presently required to sustain the plasma in the ignited cesium diode. This will substantially increase the energy conversion efficiency, and will permit operation at substantially lower emitter temperatures without requiring lower collector (heat rejection) temperature. Present work is concentrating on evaluating and reducing to practice the several methods employing auxiliary ion sources to eliminate the arc drop which were demonstrated over a decade ago: i.e., various ignited and unignited triode concepts, and the pulse-enhanced diode and triode. These methods are reviewed in light of present understanding and recent experimental data.

Rasor, N. S.↗

NASA NTRS1975

Airship construction

Forty-four years ago the first successful metal airship was completed and delivered to the United States Navy, the ZMC-2. Between those years and the present, very little effort or serious consideration has been given to the manufacture, design, construction, or economic impact of airships. It is important to retain and exploit the small but continually diminishing pool of airship talent that will expedite the success of the United States in what is now a pioneering venture. The relative simplicity of airship construction, utilizing the tremendous technical advances of the last 44 years, leads to the conclusion that this form of transportation holds great promise for reducing costs of military missions and improving the international competitive position of the United States in commercial applications.

Roda, J.↗

NASA NTRS1973

Ocean tides

Progress in the understanding of ocean tides since the field was reviewed two years ago by Hendershott and Munk [1970] has confirmed their characterization of the field as rapidly developing. The First Geodesy/ Solid‐Earth and Ocean Physics (GEOP) Research Conference on Solid‐ Earth and Ocean Tides provided an opportunity to gather subsequent results and to view them in the context of long‐term trends in the development of the field. This review, therefore, largely picks up where that of Hendershott and Munk [1970] left off; the two reviews together are intended to provide a modern view of our state of understanding of ocean tides. Vital progress in instrumentation, in data analysis, and in the closely related field of solid‐earth tides is outlined in the accompanying summary of conference discussions beginning on page 96 of this issue.

M. C. Hendershott↗

NASA NTRS1973

The Earth's Rotation

The most ancient and fundamental concern of astronomy is the orientation and motion of a terrestrial observer relative to the stars. Its geophysical aspects date from the time of Newton and Halley, and its mathematical foundations were laid by Euler 200 years ago. Despite this honorable antiquity, the subject is far from moribund and today presents a rich and fascinating array of challenges to observation, experiment, data analysis, and theory. The many‐faceted problems of the three‐dimensional rotation of the earth about its center of mass now attract astronomers and paleontologists, solid earth geophysicists and electrical engineers, general relativists and oceanographers, and applied mathematicians and scholars of classical texts.

M G Rochester↗

NASA NTRS1975

Foundations of space biology and medicine. Volume 1: Space as a habitat

The last decade has witnessed the beginning of man's exploration of the Universe with an entirely new potentiality-manned and instrumented space vehicle capable of bringing observations closer to celestial bodies than had been deemed possible a few years ago. How far into the Universe this exploration will ultimately lead is in the hands of future generations. However, the solar system is already highly instrumented, with data being recorded hourly both directly and indirectly. A vast amount of information is accumulating, the resolution of which will take painstaking effort for many years. In short, mankind has achieved familiarity with the Sun and its planets in a comparatively short time.

Malvin Calvin↗

NASA NTRS1976

An equivalent energy for the outgassing of space materials

Materials for space applications must have low outgassing rates at normal operating temperatures, and the outgassing products should include a minimum of condensables at the temperatures of nearby surfaces. A screening method, developed several years ago and used at many space laboratories, consists of holding a material sample at 398 K (125 C) for 24 hours and measuring its percentage total mass loss (TML) and the percentage volatile condensable mass (VCM) accreted on a 298-K (25-C) collector. In general, the material is acceptable if the TML is less than 1 percent and the VCM is less than 0.1 percent. An analysis of the test and its results is presented.

Scialdone, J. J.↗

NASA NTRS1976

Petrographic and petrological study of lunar rock materials

Samples returned from Apollo 14 (14171, 14305, 14319), Apollo 15 (15255), Apollo 16 (61175, 67455), and Apollo 17 (77215) were studied optically and selected polished sections by SEM/Microprobe. Splits and separates from 77215, 67455, 61175 and 15255 were prepared; 77215 and 67455 were analyzed for major, minor and LIL trace elements. The data indicate that 77215, a noritic breccia clast found in the Station7 boulder, is a norite cumulate similar to and probably derived from the same body as 78235. The Apollo 17 boulders are found to be part of the same melt sheet, which was formed by a major impact event, possibly Serenitatis, about 4 B. Y. ago. The Apollo 14 and 16 breccias are polymict, their clast populations indicating quite different provenance. The Apollo 14 breccias are possibly the result of multiple impacts, while the other breccias studied appear to have been formed by single impacts. ANT suite clasts included in 61175 are, for the most part, granulites resulting from subsolidus recrystallization of norites, anorthosites or gabbros. This metamorphism appears to have occurred prior to the impact event forming 61175.

Winzer, S. R.↗

NASA NTRS1976

Rb, Sr and strontium isotopic composition, K/Ar age and large ion lithophile trace element abundances in rocks and glasses from the Wanapitei Lake impact structure

Shock metamorphosed rocks and shock-produced melt glasses from the Wanapitei Lake impact structure have been examined petrographically and by electron microprobe. Eleven clasts exhibiting varying degrees of shock metamorphism and eight impact-produced glasses have been analyzed for Rb, Sr and Sr isotopic composition. Five clasts and one glass have also been analyzed for large ion lithophile (LIL) trace element abundances including Li, Rb, Sr, and Ba and the REE's. The impact event forming the Wanapitei Lake structure occurred 37 m.y. ago based on K/Ar dating of glass and glassy whole-rock samples. Rb/Sr isotopic dating failed to provide a meaningful whole-rock or internal isochron. The isotopic composition of the glasses can be explained by impact-produced mixing and melting of metasediments.

Winzer, S. R.↗

NASA NTRS1976

Impedance of silver oxide-zinc cells

Over 100 sealed AgO-Zn cells were subjected to prolonged periods of storage over a range of temperatures and storage modes including open circuit, trickle charge, and float charge. Impedances of these cells were monitored throughout, and at the end of the storage period their transient voltage characteristics were observed at the onset of discharge. Results revealed that the impedances of these cells tended to increase with storage time; the magnitude of the impedance rise was dependent primarily on temperature and to a lesser degree on storage mode. Typical values for 50 A-hr cells were usually less than 100 mohm immediately after activation and from 1 to 30 ohm after 6-10 months of storage. Transient voltages of these cells droped sharply during the first msec of discharge and then rose to a stablized value during the following few seconds. The magnitude of the initial drop and the stabilized voltage values were found to be related to impedance but not in a linear manner. The magnitude and duration of the low transient voltages may be unacceptable in some applications of these cells. The impedance variations are attributed to changes occurring at the positive electrode.

Frank, H. A.↗

NASA NTRS1975

Evolution of the moon - The 1974 model

Based on the geological discoveries of the Apollo and Luna missions, the evolution of the moon is divided into seven major stages, beginning at some time near the end of the formation of the solar system. These stages are: (1) the beginning, 4.6 billion years ago (b.y.a.); (2) melting of the outer shell, 4.6 to 4.4 b.y.a.; (3) cratering of the highlands, 4.4 to 4.1 b.y.a.; (4) formation of the large basins, 4.1 to 3.9 b.y.a.; (5) formation of the light-colored plains, 3.9 to 3.8 b.y.a.; (6) formation of the basaltic maria, 3.8 to about 3.0 b.y.a.; and (7) the quiet-crust stage, about 3.0 b.y.a. to the present. Each Apollo and Luna mission is reviewed, emphasizing the most important discoveries and experiments performed. The limits on this interpretative understanding of the moon and the outlined sequence of events are pointed out.

Schmitt, H. H.↗

NASA NTRS1976

Early lunar magnetism

A new method (Shaw, 1974) for investigating paleointensity (the ancient magnetic field) was applied to three subsamples of a single, 1-m homogeneous clast from a recrystallized boulder of lunar breccia. Several dating methods established 4 billion years as the age of boulder assembly. Results indicate that the strength of the ambient magnetic field at the Taurus-Littrow region of the moon was about 0.4 oersted at 4 billion years ago. Values as high as 1.2 oersted have been reported (Collison et al., 1973). The required fields are approximately 10,000 times greater than present interplanetary or solar flare fields. It is suggested that this large field could have arisen from a pre-main sequence T-Tauri sun.

Banerjee, S. K.↗

NASA NTRS1976

Nd isotopic variations and petrogenetic models

The isotopic composition of Nd in selected terrestrial rocks is investigated to gain information about its implications for petrogenesis and the history of the earth's crust and mantle. Chemical and mass-spectrometric measurements of the Nd-143/Nd-144 ratio in terrestrial rocks of different ages show that the Sm/Nd ratio and the rare-earth-element (REE) abundance pattern are equal within a few per cent to those of chondritic meteorites. Variations in the Nd isotopic ratio in young basalts are found to permit the identification of distinctive mantle sources and to indicate the preservation of significant heterogeneities in the mantle for times of 1 to 4 billion years ago. The isotopic data also show that mantle source regions with a Sm/Nd ratio which differs from the chondritic value by a factor of two are not preserved for more than a few hundred million years. The average continental crust material is found to have a much lower isotopic ratio than the mantle, reflecting the crust's low Sm/Nd ratio resulting from REE fractionation during crust formation from the mantle.

Depaolo, D. J.↗

NASA NTRS1976

Lunar volcanism in space and time

The role of lunar volcanism in the history of the moon is documented using lunar-orbit and earth-based data along with characterizations derived from Apollo and Luna sample-return missions. Characteristics of mare and highland volcanic features are described, Apollo and Luna results are discussed, and the characteristics of other mare deposits and of other highland features of possible volcanic origin are summarized. Major conclusions are that: (1) there is little unequivocal morphologic evidence for highland volcanism, (2) lunar mare lavas appear to have originated from depths of 100 to 500 km, (3) impact melting does not appear to have been a factor in the generation of mare lavas, (4) mare volcanism was characterized by massive outpourings of very fluid volatile-poor lava analogous to terrestrial flood basalts, (5) mare volcanism took place from 3.83 to about 2.5 billion years ago, (6) the preferential occurrence of mare deposits in large impact basins appears to be generically unrelated to basin formation, and (7) a thicker farside crust may be responsible for the distinctive nearside-farside asymmetry of mare deposits.

Head, J. W., III↗

NASA NTRS1976

On the equation of state for an electron gas in an intense magnetic field

In this paper we derive the equation of state for a relativistic electron gas imbedded in a static homogeneous magnetic field of arbitrary strength. The derivation is based on the evaluation of the energy-momentum tensor and the use of Dirac's equation for such a problem. Contrary to a derivation presented several years ago, the present derivation is completely gauge-invariant. We also show how to recover, in an exact manner, the perfect gas law for the case of weak magnetic fields.

Canuto, V.↗

NASA NTRS1976

Preliminary results from the Viking orbiter imaging experiment

During its first 30 orbits around Mars, the Viking orbiter took approximately 1000 photographic frames of the surface of Mars with resolutions that ranged from 100 meters to a little more than 1 kilometer. Most were of potential landing sites in Chryse Planitia and Cydonia and near Capri Chasma. Contiguous high-resolution coverage in these areas has led to an increased understanding of surface processes, particularly cratering, fluvial, and mass-wasting phenomena. Most of the surfaces examined appear relatively old, channel features abound, and a variety of features suggestive of permafrost have been identified. The ejecta patterns around large craters imply that fluid flow of ejecta occurred after ballistic deposition. Variable features in the photographed area appear to have changed little since observed 5 years ago from Mariner 9. A variety of atmospheric phenomena were observed, including diffuse morning hazes, both stationary and moving discrete white clouds, and wave clouds covering extensive areas.

Carr, M. H.↗

NASA NTRS1977

DSN automation

An overall hierarchical automation philosophy along with the results of the radio frequencies automation effort undertaken 2 years ago are summarized. A brief description of each subassembly controller's salient features, the software development process, and the common software used by these controllers will be presented. Comments will be made with respect to the relative advantages of high-level language and assembly language, the operational effectiveness of operator Macro commands, and the program development, and a list of suggested future effort will be given.

Crow, R. B.↗

NASA NTRS1977

Origin of the earth's ocean basins

The earth's original ocean basins were mare-type basins produced 4 billion years ago by the flux of asteroid-sized objects responsible for the lunar mare basins. Scaling upwards from the observed number of lunar basins for the greater capture cross-section and impact velocity of the Earth indicates that at least 50 percent of an original global crust would have been converted to basin topography. These basins were flooded by basaltic liquids in times short compared to the isostatic adjustment time for the basin. The modern crustal dichotomy (60 percent oceanic, 40 percent continental crust) was established early in the history of the earth, making possible the later onset of plate tectonic processes. These later processes have subsequently reworked, in several cycles, principally the oceanic parts of the earth's crust, changing the configuration of the continents in the process. Ocean basins (and oceans themselves) may be rare occurrences on planets in other star systems.

Frex, H.↗

NASA NTRS1976

Emission object in Orion

The note draws attention to a structural feature in the Orion nebula, consisting of a parachute-shaped object converging on 64 Orionis, noted on H alpha photographs of the Orion nebula taken with the 76-cm Allegheny refractor. The same feature shows up clearly on a photograph taken in 1909 with the Mount Wilson 152-cm reflector, and on a photograph taken with the Palomar 5-m reflector. Measurements made on these three plates indicate a possible expansion of the object of about 3.6 seconds of arc per century, corresponding to a tangential velocity of about 90 to 100 km/sec. If the expansion continued at a linear rate, an explosive event may have occurred approximately 900 years ago.

Feibelman, W. A.↗