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Fanale, F. P.

Publications and source records attributed to Fanale, F. P..

At least 73 records · Page 4
All sourcesNASA NTRSDOE OSTI
NASA NTRS1977

Io's surface composition based on reflectance spectra of sulfur/salt mixtures and proton-irradiation experiments

Available full-disk reflectance spectra of Io in the range 0.3 to 2.5 microns have been used to determine a surface compositional model for Io that is consistent with Io's other known chemical and physical properties. Results indicate that the surface of Io contains abundant dehydrated salts of high Na, Mg, and Fe(3+) content such as bloedite and ferrous iron sulfate. Experiments were performed studying the irradiation damage effects from low-energy proton bombardment, since Io is immersed in Jupiter's magnetosphere.

Nash, D. B.↗
NASA NTRS1977

Io's surface and the histories of the Galilean satellites

Similarities and differences among the Galilean satellites are discussed. A hypothesis is offered that the surface of Io is largely covered by 'evaporite' salts produced by defluidization of Io's interior, migration of salt-saturated solutions to Io's surface, and subsequent H2O loss to space. Laboratory reflectance studies show that evaporites constitute a good match to Io's spectrum in the infrared, in contrast to ices or frosts, the presence of which is not considered likely in view of the absence of near IR ice bands in Io's surface spectrum. Likely coloring agents in the blue include elemental sulfur, which may be produced from sulfates by proton irradiation or other processes, and F-centers produced by irradiation with magnetospheric protons. Preferential irradiation of material in the polar regions may account for Io's peculiar dark polar caps.

Fanale, F. P.↗
NASA NTRS1976

Space exploration and the history of solar-system volatiles

The thermochemical history of volatile substances in all solar-system planets, satellites, and planetoids is discussed extensively. The volatiles are viewed as an interface between the abiotic and biotic worlds and as a key to the history of bodies of the solar system. A flowsheet of processes and states is exhibited. Differences in bulk volatiles distribution between the planetary bodies and between the interior, surface, and atmosphere of each body are considered, as well as sinks for volatiles in degassing. The volatiles-rich Jovian and Saturnian satellites, the effect of large-planet magnetosphere sweeps on nearby satellites, volatiles of asteroids and comets, and the crucial importance of seismic, gravity, and libration data are treated. A research program encompassing analysis of the elemental and isotopic composition of rare gas in atmospheres, assay of volatiles-containing phases in regoliths, and examination of present or past atmospheric escape/accretion processes is recommended.

Fanale, F. P.↗
NASA NTRS1976

Martian volatiles - Their degassing history and geochemical fate

Implications of the Ar-40 content of the Martian atmosphere for Martian volatile history are considered. It is assumed that the potassium content of both Mars and earth is similar to that of normal chondrites, that Mars possesses a water content similar to that of normal chondrites, and that earth's water content is equal to or somewhat less than Mars'. A simple earth-analogous Mars degassing model is outlined in which the Martian surface volatile inventory is presumed to be identical to earth's, but scaled to the smaller mass and surface area of Mars. Physical storage of volatiles in the Martian regolith is examined along with the occurrence of volatile-containing mineral phases in the regolith, exospheric escape as a massive volatile sink, and the effect of the time history of degassing on the surface volatile inventory. Implications of earth's degassing history for Mars are assessed, and models describing the overall intensity of Mars degassing are presented. It is concluded that the maximum amounts of water and other volatiles that could be stored in the Martian regolith are marginally compatible with those required by the earth-analogous model, although a lower atmospheric Ar-40 concentration and regolith volatile inventory would be easier to reconcile with observational constraints.

Fanale, F. P.↗
NASA NTRS1976

Scientific possibilities of a solar electric powered rendezvous with comet Encke

The minimum scientific spacecraft instrumentation is considered that is likely to result in as complete an understanding of the composition, structure, and activity of a cometary nucleus as is possible without landing on it. The payload will also give useful results on secondary goals of a better understanding of physical processes in the inner and outer coma. Studies of composition, by means of an actual landing on the surface, details of the internal structure of the nucleus, and sample return were considered beyond the scope of this mission.

Newburn, R. L., Jr.↗
NASA NTRS1976

Asteroids and comparative planetology

The state of knowledge concerning the asteroids is reviewed and discussed in terms of the relationship of the asteroids with other solar system bodies. The data on spectral reflectances of asteroids are examined, and their implications for comparative planetology are discussed.

Matson, D. L.↗
NASA NTRS1975

Na-D line emission from rock specimens by proton bombardment - Implications for emissions from Jupiter's satellite Io

The effectiveness of low-keV range protons in producing Na line emission from selected sodium-bearing rock and mineral samples is examined. Laboratory experiments show that substantial Na-D line emission is produced by 3- to 5-keV proton bombardment of silicate and halite rock powders. It is found that emission intensity and energy efficiency are directly proportional to sodium content and are dependent on total dose, dose rate, and proton energy. Na-D photon emission is considered to emanate predominantly from sputtered sodium slightly above the target surfaces. It is concluded that the Na-D line emission directly excited during surface sputtering by Jovian magnetospheric protons appears to be an observable component in the Jovian satellite Io emission.

Nash, D. B.↗
NASA NTRS1974

Io - A surface evaporite deposit

A model is suggested for Io's surface composition involving evaporite salt deposits, rich in sodium and sulfur. According to this model, these deposits were produced as a result of the migration of salt-saturated aqueous solutions to Io's surface from a warm or hot interior followed by loss of the water to space. This model satisfies cosmochemical constraints based on Io's initial composition, current density, and thermal history. Salt-rich assemblages are easily derivable from the leaching of carbonaceous chondritic material. The chemical and optical properties of such deposits, after modification by irradiation, can be used to explain Io's overall albedo and spectral reflectance, its dark reddish poles, and the observed sodium emission as well as or better than other currently suggested materials.

Fanale, F. P.↗
NASA NTRS1974

Exchange of adsorbed H2O and CO2 between the regolith and atmosphere of Mars caused by changes in surface insolation

Estimates have been made of the capacity of the Martian regolith to exchange adsorbed H2O and CO2 with the atmosphere-plus-cap system (APCS). These estimates are based upon measured isotherms for H2O and CO2 adsorption on pulverized basalt at low temperatures and on theoretical considerations. A unit column (1 sq cm) of regolith with a deep subsurface temperature of -77 C, considered average for the disk, will contain about 0.4 g of adsorbed CO2 and about 1 g of adsorbed H2O per meter of depth. Under favorable circumstances the top 3 cm can exchange much more H2O with the lower atmosphere each day than is necessary to produce the diurnal brightening. The process appears to be seasonally reversible. The total regolith may contain, in the adsorbed phase alone, as much as 1% of the H2O and 5% of the CO2 surface inventories expected for a hypothetical Mars that has experienced degassing as intensive as that of earth.

Fanale, F. P.↗
NASA NTRS1974

Sodium D-line emission from Io - Sputtering and resonant scattering hypothesis

A model is presented in explanation of the observation of sodium D-line emission from Io. The model involves: (1) charged-particle sputtering of sodium from Io's surface, (2) ejection of sodium into a cloud surrounding Io, and (3) resonant scattering of incident sunlight. Observational consequences and tests of the proposed model are also discussed.

Matson, D. L.↗
NASA NTRS1974

Surface properties of the Orgueil meteorite - Implications for the early history of solar system volatiles

The Kr and H2O adsorption properties of Orgueil were studied. Dehydration by stepwise calcination produced a tenfold change in its B.E.T. surface area, which increased to 120 and then fell to 40 square meters per gram. Water exchangeability was measured by water regain from lab air between calcination cycles. Dehydration at room temperature showed that Orgueil contained 6 per cent by weight of water adsorbed on free surfaces. These results are consistent with an identification of Orgueil as montmorillonite, although chemical data conflict with this. High D/H ratios in CI carbonaceous chondrites may result from D enrichment in OH- groups during equilibration of dispersed phyllosilicate dust with preplanetary nebula gas at temperatures much less than 0 C.

Fanale, F. P.↗
NASA NTRS1973

Optical properties of carbonaceous chondrites and their relationship to asteroids

Results of diffuse reflectance measurements of nine samples of carbonaceous chondrites (one C1, three C2, four C3, and one C4) and one iron meteorite, Odessa. Measurements were also made of mineral mixtures in an attempt to understand the cause of some features of the meteorite reflectances. The C1 and C2 carbonaceous chondrites have reflectances low enough to match the anomalously low albedos of some asteroids. Some asteroids have spectral reflectances similar to carbonaceous chondrites, whereas others with flat or F-type curves appear to match simulated mineral mixtures with slightly greater amounts of the carbonaceous component than those found in the meteorites. This observation suggests either that surface physical processes such as melting may be enhancing the optical effect of opaque carbonaceous material on some asteroid surfaces and/or that these asteroids contain even more carbonaceous material than the C1 meteorites.

Johnson, T. V.↗
NASA NTRS1973

Volatile evolution

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Fanale, F. P.↗
NASA NTRS1972

Origin of planetary primordial rare gas - The possible role of adsorption.

The degree of physical adsorption of Ne, Ar, Kr, and Xe on pulverized samples of the Allende meteorite at 113 K has been measured. The observed pattern of equilibrium enrichment of heavy rare gases over light on the pulverized meteorite surfaces relative to the gas phase is similar to the enrichment pattern exhibited by planetary primordial rare gas when compared with the composition of solar rare gas. Results indicate that, at 113 K, a total nebular pressure of from .01 to .001 atm would be required to explain the Ar, Kr, and Xe abundances in carbonaceous chondrites with an adsorption mechanism. This pressure estimate is compatible with the range of possible nebular pressures suggested by astrophysical arguments. However, the subsequent mechanism by which initially adsorbed gas might have been transferred into the interiors of grains cannot be identified at present.

Fanale, F. P.↗
NASA NTRS1971

History of Martian volatiles - Implications for organic synthesis.

A theoretical reconstruction of the history of Martian volatiles indicates that Mars probably possessed a substantial reducing atmosphere at the outset of its history, and that its present tenuous and more oxidized atmosphere is the result of extensive chemical evolution. As a consequence, it is probable that Martian atmospheric chemical conditions, now hostile with respect to abiotic organic synthesis in the gas phase, were initially favorable. Evidence indicating the chronology and degradational history of Martian surface features, surface mineralogy, bulk volatile content, internal mass distribution, and thermal history suggests that Mars catastrophically developed a substantial reducing atmosphere as the result of rapid accretion.

Fanale, F. P.↗
NASA NTRS1971

A case for catastrophic early degassing of the earth.

Evidence is given for the occurrence in early earth history of massive escape of volatiles from the interior of the earth to its surface, which must have had catastrophic proportions. The mechanism and time of this event are inferred from the abundances and distribution of volatiles in the atmosphere, hydrosphere and crust, and from meteorite studies, and geophysical and astronomical observations. This event is linked to the melting of the earth during accretion which resulted in the concentration of U, Th, K and Pb in the outermost portion of the earth and in virtually complete expulsion of nonradiogenic Ar, Ne and Kr from its interior.

Fanale, F. P.↗