Lead isotopes and volatile transfer in the lunar soil
Lead isotopes volatile transfer in Apollo 11 and 12 lunar soil samples, discussing lunar age estimates
Black, L. P.↗
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Chemical fractionations in meteorites. V - Volatile and siderophile elements in achondrites and ocean ridge basalts.
Eighteen achondrites and 4 terrestrial basalts (3 ocean ridge, 1 continental) were analyzed by radiochemical neutron activation analysis for Ag, Au, Bi, Br, Cd, Co, Cs, Cu, Ga, In, Ir, Rb, Se, Tl and Zn. Samples included 7 eucrites, 5 howardites, 2 nakhlites, 2 shergottites, an angrite, and an aubrite. Light and dark portions of the gas-rich meteorites Kapoeta and Pesyanoe were analyzed separately. Nakhlites and shergottites have volatile element abundances similar to those in ocean ridge basalts; eucrites, howardites, and angrites show greater depletions by an order of magnitude and less similar abundance patterns. In terms of a two-component model of planetary accretion, the parent planets contained the following percentages of low-temperature material: eucrites 0.8, nakhlites 38, shergottites 28. Shergottites may be genetically related to L-chondrites. The siderophile element pattern of achondrites resembles that of the moon, but with less extreme depletions.
Laul, J. C.↗
Gas chromatography of volatile organic compounds
System has been used for problems such as analysis of volatile metabolities in human blood and urine, analysis of air pollutants, and in tobacco smoke chemistry. Since adsorbent is reusable after porper reconditioning, method is both convenient and economical. System could be used for large scale on-site sampling programs in which sample is shipped to central location for analysis.
Zlatkis, A.↗
Volatiles working group
The physical behavior of water and carbon dioxide on Mars was studied. Topics discussed include: physics of polar frosts, CO2 budget, atmospheric minor constituents, chemical and physical properties of surface materials, layered deposits, and the role of volatiles in the Martian landscape formation.
Cutts, J. A.↗
Volatilized lead from Apollo 12 and 14 soils.
Lead in some Apollo-12 and -14 soils and breccias was volatilized under vacuum at temperature intervals of 0 to 600 C, 600 to 800 C, 800 to 1000 C, and 1000 to 1350 C. It is found that the Pb(206)/Pb(204) ratio increases and the Pb(207)/Pb(206) ratio decreases in the temperature range between 600 and 1000 C. The Pb(208)/Pb(206) ratios decrease from a value of 2 at 600 C to a value of 0.7 at 1350 C. These and other data suggest a secondary isochron age of about 4200 million years.
Doe, B. R.↗
Volatile terpenoids from aeciospores of Cronartium fusiforme.
Identification of the terpenoids present in the volatile fraction from aeciospores of the gall rust fungus Cronartium fusiforme. The major monoterpenoid hydrocarbons found to be present with only traces of camphene include alpha-pinene, beta-pinene, delta(3)-carene, myrcene, linonene, beta-phellandrene, and delta-terpinene. A number of monoterpenoid alcohols, acyclic sesquiterpenes, and aromatic compounds were also present.
Laseter, J. L.↗
Polar volatiles on Mars - Theory versus observation
Synthesis of the results of the Mariner 9 mission, as they pertain to polar volatiles, and comparison of them with a description of the solid-vapor equilibrium relations believed to be presently active on Mars. The discovery by Mariner 9 of extensive volcanic deposits on portions of the Martian surface suggests that the total amount of CO2 liberated to the surface probably exceeds that now present in the atmosphere. Thus excess CO2 in the solid form is to be expected in the polar areas. Although the simplified model of Leighton and Murray (1966), which predicts a permanent CO2 cap, has significant deficiencies both theoretically and observationally, the seasonal caps are composed of CO2, as predicted, excess CO2 is quite likely, and a permanent deposit of solid CO2 evidently is in equilibrium with atmospheric CO2. It is suggested that there must be a large reservoir of solid CO2 in gaseous equilibrium with the atmosphere, but buried immediately below the exposed residual water-ice cap. This reservoir is believed to be located near the north pole. The principal effect of such a reservoir is to average out annual and longer-term fluctuations in the polar heat balance.
Murray, B. C.↗
Internal friction of rocks and volatiles on the moon
Internal friction quality factors Q up to 2200 have been observed in a strongly outgassed terrestrial analog of lunar basalt. This was accomplished by successively cycling a bar shaped sample vibrating in its fundamental longitudinal mode at 15 kHz to higher and higher temperatures in a vacuum between 100 and 10 nanotorr. After each cycle, Q measured at room temperature in the vacuum was observed to decrease with time suggesting that gas reabsorption was taking place even at these low pressures. A study of the effect of exposing a sample to a variety of gases and vapors showed that of the volatiles most likely to be present in the lunar environment H2O was by far the most effective in lowering Q.
Tittmann, B. R.↗
Microwave spectra of some volatile organic compounds
A computer-controlled microwave (MRR) spectrometer was used to catalog reference spectra for chemical analysis. Tables of absorption frequency, peak absorption intensity, and integrated intensity are included for 26 volatile organic compounds, all but one of which contain oxygen.
White, W. F.↗
Volatile and siderophilic trace elements in the soils and rocks of Taurus-Littrow
Data are reported on 22 elements determined on 11 soils, one soil breccia, and two crystalline rocks from the Apollo 17 Taurus-Littrow landing site. The elements determined include the siderophilic elements Ni, Ge, Ir, and Au. The volatile elements considered include Na, Zn, Cd, and In. Attention is given to the extralunar component in soils and breccias, the orange-glass component in soils and breccias, and the labile elements in lunar soils.
Baedecker, P. A.↗
Internal friction in rocks and its relationship to volatiles on the moon
The physical properties of lunar rocks were measured using the vibrating bar technique in order to provide data for interpretation of geophysical results such as those from seismic measurements. The effect of volatiles on the mechanical Q in lunar rocks was studied in addition to the effect of exposing a sample to controlled amounts of those gases most likely to be present in the lunar environment or likely to have been outgassed from the lunar interior. The moderate temperatures to which the sample was exposed during the thermal treatment and the small drop in resonant frequency during the course of the outgassing suggests that there was little change in microfracture density. The frequency, composition and texture dependence of the damping were investigated, to study the loss mechanism.
Tittmann, B. R.↗
Volatile organic components in the Skylab 4 spacecraft atmosphere
The volatile organic components in the spacecraft cabin atmosphere of Skylab 4 were trapped on a solid adsorbent at various times during the mission. In post-flight analyses, more than 300 compounds in concentrations from less than 1 ppb up to 8000 ppb could be detected by high-resolution gas chromatography. In the samples of the 11th, 47th, and 77th day of the mission, approximately 100 components in the molecular weight range from 58 to 592 were identified by mass spectrometry. Besides components known from other environments, such as alkanes, alkenes, and alkylated aromatic hydrocarbons, components typical of the human metabolism, such as ketones and alcohols, were found. Other typical components in the spacecraft atmosphere included fluorocarbons and various silicone compounds, mostly normal and cyclic methylsiloxanes.
Liebich, H. M.↗
Study of volatile contaminants in reclaimed water
Different methods were evaluated for reducing the volatile contaminants found in water recovered from urine by distillation. The use of activated carbon, addition of potassium permanganate, and the use of oxidation catalyst are described along with laboratory tests. It is concluded that catalytic decomposition appears to be feasible, and further investigation is recommended.
Mckee, H. C.↗
A new estimate of volatile outgassing on Mars
The presence of 28% argon on Mars, as calculated by Levine and Riegler (1974) and indirectly inferred from Soviet Mars-6 lander data, has important implications for the outgassing history of H2O, CO2, and N2 on Mars. Even if the terrestrial volatile outgassing ratio is only approximately valid for Mars, then large quantities of H2O (of the order of 100,000 g/sq cm), about 10,000 g/sq cm of CO2 (about 1000 times more CO2 than found at present in the Martian atmosphere), and some 450 g/sq cm of N2 may have outgassed over the history of Mars.
Levine, J. S.↗
Mars - Chemical weathering as a massive volatile sink
The amounts of volatiles incorporated in the Martian regolith by photostimulated oxidation weathering of Fe(2+)-bearing minerals are estimated. The process of photostimulated oxidation weathering is described, and it is noted that all the necessary constituents for this process are present on Mars. The rates at which oxygen and hydrogen are irreversibly removed from the Martian atmosphere by the present process are determined, irreversible and reversible water losses are considered, and the loss of CO2 by carbonate formation is shown to be irreversible. The results suggest that photostimulated oxidation weathering has irreversibly consumed 100 to 100,000 g/sq cm of H2O and 10 to 10,000 g/sq cm of CO2, assuming a uniform rate over geologic time. It is concluded that if the amounts of H2O and CO2 actually removed by photostimulated oxidation are close to the upper limits of the present estimates, then that process may have had a major effect in limiting the amount of H2O and CO2 trapped in the regolith and polar caps.
Huguenin, R. L.↗
Search for organic and volatile inorganic compounds in two surface samples from the Chryse Planitia region of Mars
Two surface samples collected from the Chryse Planitia region of Mars were heated to temperatures up to 500 C, and the volatiles that they evolved were analyzed with a gas chromatograph-mass spectrometer. Only water and carbon dioxide were detected. This implies that organic compounds have not accumulated to the extent that individual components could be detected at levels of a few parts per billion by weight in the samples. Proposed mechanisms for the accumulation and destruction of organic compounds are discussed in the light of this limit.
Biemann, K.↗
Oxygen isotopes in the Martian atmosphere - Implications for the evolution of volatiles
Nonthermal escape of oxygen by recombination of exospheric O2(+) combined with diffusive separation of gases at lower altitude provides a mechanism through which the Martian atmosphere may be enriched in O-18 relative to O-16. Measurement of the abundance of O-18 relative to O-16 together with a determination of the turbopause may be used to develop important constraints on the history of Martian volatiles. Models for the interpretation of these data are developed and discussed in light of present information.
Mcelroy, M. B.↗
Volatile compounds released during lunar lava fountaining
A modified radiochemical neutron activation analysis was used to determine 24 elements in three sieve separates and in HCl leach, HF etch, and residue fractions of the 500-62 micron separate of orange glass fines 74220. Six elements - In, Cd, Zn, Ga, Ge, and Au - were strongly concentrated in the leach, indicating that they were present as a surface deposit, probably a sublimate resulting from condensation of lava-fountain volatiles which expelled the orange glass onto the lunar surface.
Wasson, J. T.↗