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Radioactive-nuclide system automatically monitors animals in the field, using radioactive tracers affixed to the animals, Geiger-Muller tube radiation detectors, and event-recorders. Four animals can be monitored simultaneously within a 32-m circle, with each animal as far as 1 m from its associated detector.
The thermal history and current state of the lunar interior are investigated using constraints imposed by recent geological and physical data. Theoretical temperature models are computed taking into account different initial conditions, heat sources, differentiation and simulated convection. To account for the early formation of the lunar highlands, the time duration of magmatism and present-day temperatures estimated from lunar electrical conductivity profiles, it is necessary to restrict initial temperatures and abundances of radioactive elements. Successful models require that the outer half of the moon initially heated to melting temperatures, probably due to rapid accretion. Differentiation of radioactive heat sources toward the lunar surface occurred during the first 1.6 billion years. Temperatures in the outer 500 km are currently low, while the deep interior (radius less than 700 to 1000 km) is warmer than 1000 C, and is of primordial material.
New information is used to demonstrate that better models for the thermal history of the moon are required. As a first step, account is taken of (1) a nonuniform initial composition in terms of fraction of low melting to high melting phase present, and for variation in the uranium, potassium, and thorium contents as a function of depth, (2) partitioning of the radioactive elements between the melt and the solid phases, and (3) a cutoff value of melt which must be exceeded before magma can move to the surface. The results of several attempts to determine whether reasonable conditions, composition, and thermal properties can be expected to give rise to two separate periods of volcanism are discussed. Two models with somewhat different distributions of radioactive heat sources and different conductivities are examined.
Technique involves introduction of radioactive sample into antecubital vein. Scintillation crystal mounted in collimating housing views portion of right and left hearts. As radioactive sample passes through heart, counting rate is measured by crystal and recorded on strip chart. Data is insensitive to geometric effects and other parameters.
A computer program was adapted from a previous generation program to analyze the temperature and internal pressure response of a radioactive nuclear waste material disposal container following impact on the earth. This program considers component melting, LiH dissociation, temperature dependent properties and pressure and container stress response. Analyses were performed for 21 cases with variations in radioactive power level, container geometry, degree of deformation of the container, degree of burial and soil properties. Results indicated that the integrity of SS-316 containers could be maintained with partial burials of either underformed or deformed containers. Results indicated that completely buried waste containers, with power levels above 5 kW, experienced creep stress rupture failures in 4 to 12 days.
Calculations were made to determine if a cladding failure could be detected in a 100-kW zirconium hydride reactor primary system by monitoring the highly radioactive NaK coolant for the presence of I-131. The system is to be completely sealed. A leak of 0.01 percent from a single fuel pin was postulated. The 0.364-MeV gamma of I-131 could be monitored on an almost continuous basis, while its presence could be varified by using a longer counting time for the 0.638-MeV gamma. A lithium-drifted germanium detector would eliminate radioactive corrosion product interference that could occur with a sodium iodide scintillation detector.
The gamma rays emitted from the moon or any similar body carry information on the chemical composition of the surface layer. The elements most easily measured are K, U, Th and major elements such as O, Si, Mg, and Fe. The expected fluxes of gamma ray lines were calculated for four lunar compositions and one chondritic chemistry from a consideration of the important emission mechanisms: natural radioactivity, inelastic scatter, neutron capture, and induced radioactivity. The models used for cosmic ray interactions were those of Reedy and Arnold and Lingenfelter. The areal resolution of the experiment was calculated to be around 70 to 140 km under the conditions of the Apollo 15 and 16 experiments. Finally, a method was described for recovering the chemical information from the observed scintillation spectra obtained in these experiments.
Preliminary review of data from the radioactivity relief map of the regions of the moon overflown by the Apollo 15 command module. The data represent count rates in the energy band from 0.55 to 2.75 MeV, appropriately corrected and averaged. Review results include the findings that: (1) the major concentrations of radioactivity in the area covered are in the region of Mare Imbrium and Oceanus Procellarum, (2) the highest regions are in the area of Aristarchus in Oceanus Procellarum and a region in eastern Mare Imbrium, and (3) the K/U ratio appears to be lower everywhere than that characteristic of the earth.-
The construction and use are described for a radioactive calibration source that produces an electronic gating pulse when a calibration gamma ray is emitted and makes it possible to employ this source in many calibration or stabilizing tasks without the disadvantage of having to introduce extra counts into the unknown spectrum. The described source is radioactively safe, easy to construct, and has the ability of producing gating efficiencies as high as 98%.
The amount of helium in the Venus atmosphere can be estimated from an examination of the measured ionization profiles and from the recent discovery of radioactive materials in the Venus crust. The amount necessary to give agreement between computed and experimental results is approximately 400,000,000 per cu cm at 140 km. When a nominal value of the eddy diffusion coefficient of 1,000,000 sq cm per sec is used, the atmospheric helium mixing ratio is found to be 0.00006, nearly ten times that for the earth. If agreement is required between the helium mixing ratio estimated from an earth-like distribution of crustal radioactive materials and from the measured ionization profile, the required eddy diffusion coefficient would be 5,000,000 sq cm per sec.
Examination of the data obtained by gamma-ray spectrometers on the Apollo 15 and Apollo 16 spacecraft has been carried out in part by summing up broad regions of the energy spectrum. The most instructive of these energy regions is 0.55 to 2.75 MeV, where the difference in count rates observed can be accounted for mainly by variations in the Th, U, and K content of the surface layers. The highest values are found in Mare Imbrium and Oceanus Procellarum, where a good deal of local variation is observed. By contrast, little increase is seen in the eastern maria surveyed compared with count rates in highland areas. The broad highland regions are low in radioactivity, but there is a measurable rise near the southernmost latitude on the far side. In addition to the radioactive lines, gamma-ray lines which can be ascribed to O, Si, Fe, Mg, and Al have been identified.
The gamma rays emitted from the moon or any similar body carry information on the chemical composition of the surface layer. The elements most easily measured are K, U, Th, and major elements such as O, Si, Mg, and Fe. The expected fluxes of gamma ray lines are calculated for four lunar compositions and one chondritic chemistry from a consideration of the important emission mechanisms: natural radioactivity, inelastic scatter, neutron capture, and induced radioactivity. The models used for cosmic ray interactions are those of Reedy and Arnold (1972) and Lingenfelter et al. (1972). The areal resolution of the experiment is calculated to be around 70-140 km under the conditions of the Apollo 15 and 16 experiments. Finally, a method is described for recovering the chemical information from the observed scintillation spectra obtained in these experiments.
The process of core formation in the earth is subject to the constraints that it be nearly simultaneous with accretion and yet occur in a manner that the mantle retains radiogenic Xe-129 produced from the extinct radioactivity of I-129 with a half life of 17.6 million y. From these constraints, it appears that the only feasible mechanism is the segregation of an Fe-FeS melt. Trace element abundances in major classes of meteorites and the silicate fractions of the earth show that not only there is a high depletion of sulphur in the crust and the mantle, but that it is even more highly depleted than the rare gases, water and the halogens. From the nature of this depletion pattern and the fact that any model of accretion of the earth will necessarily produce an Fe-FeS melt, it is concluded that the light element in the core is largely sulphur with minor amounts of carbon. A consequence of this mode of core formation is found to be the availability of K-40 radioactive heat production in the liquid core, estimated at about 10 to the 19th power erg/s at the present time.
Neutron and proton induced radioactivity at various locations within Skylab were measured. Samples of five metals were formed into activation packets and deployed at the following locations on the Skylab 4 mission: orbital workshop film vault, water storage tank, and two opposing orbital workshop internal locations. Radioactive nuclides were produced in the packets by nuclear interactions of high-energy protons and secondary neutrons within Skylab. Low-level gamma ray spectroscopy measurements were made on the returned packets to determine the incident neutron and proton fluxes and spectra and their variations with mass distribution.
Lunar thermal history modelling is used to demonstrate that a realistic computer simulation can be used to predict major and minor element concentrations, thickness of the lunar crust, and intensity of volcanic activity as a function of time. The models which are most consistent with the observations include: (1) a high surface temperature and low interior temperature during the very early lunar history; (2) high near-surface radioactivity and relatively low radioactivity in the interior; and (3) a molten zone formed at or near the surface which gradually migrates downward with time. Lunar magnetic anomaly calculations show that large anomalies measured at some of the landing sites and above some points on the surface cannot be caused by mere basalts but are consistent with valley fillings of Cayley-like material with a remanent magnetization of about 0.0002 emu/gm.
The intensities of proton fluxes of energy greater than 50 MeV in several recent solar flares are obtained from measurements of Ar-37 radioactivity as a function of depth in lunar material. These intensities agree within a factor of 2 with measurements made by detectors aboard satellites. The intensities of the solar proton fluxes of greater than 200-MeV and greater than 50-MeV energy averaged over the past 1000 years are estimated from measurements of Ar-39 radioactivity as a function of depth in lunar material. The intensity of greater than 200-MeV solar-flare protons obtained from Ar-39 in Fe, when averaged over the past 1000 years, was equal to that of galactic cosmic rays. This result indicates that the 19th solar cycle, which had a number of very energetic solar flares, was more typical of solar activity during the past 1000 years than was the 20th.
Contaminant generation studies were conducted at the component level using two different methods, radioactive tracer technique and gravimetric analysis test procedure. Both of these were reduced to practice during this program. In the first of these methods, radioactively tagged components typical of those used in spacecraft were studied to determine their contaminant generation characteristics under simulated operating conditions. Because the purpose of the work was: (1) to determine the types and quantities of contaminants generated; and (2) to evaluate improved monitoring and detection schemes, no attempt was made to evaluate or qualify specific components. The components used in this test program were therefore not flight hardware items. Some of them had been used in previous tests; some were obsolete; one was an experimental device. In addition to the component tests, various materials of interest to contaminant and filtration studies were irradiated and evaluated for use as autotracer materials. These included test dusts, plastics, valve seat materials, and bearing cage materials.
One mechanism previously proposed for the abiotic accumulation of molecules of one chirality in nature is asymmetric adsorption on the chiral surfaces of optically active quartz crystals. Earlier literature in this field is reviewed, with the conclusion that previous investigations of this phenomenon, using optical rotation criteria, have afforded ambiguous results. We now have studied the adsorption of radioactive D- and L-alanine on powdered d- and l-quartz, using change in radioactivity level as a criterion for both gross and differential adsorption, d-Quartz preferentially adsorbed D-alanine from anhydrous dimethyl-formamide solution, and l-quartz L-alanine. The differential adsorption varied between 1.0 and 1.8%. The implications of these observations are discussed from the viewpoint of early chemical evolution and the origin of optically active organic compounds in nature.