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At least 865 records · Page 48
All sourcesNASA NTRSDOE OSTI
NASA NTRS1981

Influence of CO2 on melting of model granulite facies assemblages - A model for the genesis of charnockites

It is shown that partial melting studies at crustal pressures in SiO2-rich portions of the system KAlSiO4-Mg2SiO2-H2O-CO2 can be used in modeling the anatectic origin of charnockites. The univariant reaction phlogopite + sanidine + quartz + vapor = enstatite + liquid yields an SiO2-rich melt (granite analog) at 3 kbar; the vapor composition at the solidus is buffered to high H2O contents by virtue of the coexistence of phlogopite with its breakdown products. With higher pressures (8 and 15 kbar), the fluid phase is buffered to higher CO2 contents and the melt composition becomes enriched in K2O and MgO (charnockite analog). Melting relations are controlled through the expansion of the quartz liquidus field relative to the enstatite and sanidine fields with increasing pressure. It is noted that partial melts generated at the base of the crust in the presence of CO2-rich fluid will be of an alkaline nature and will crystallize enstatite at lower pressures. CO2-saturated melting of similar SiO2-rich bulk compositions (phlogopite-absent) through the reaction enstatite + sanidine + quartz + CO2 - liquid occurs at temperatures above 1000 C to about 15 kbar.

Wendlandt, R. F.↗
NASA NTRS1982

Theory of metal atom-water interactions and alkali halide dimers

Theoretical studies of the interactions of metal atoms with water and some of its isoelectronic analogs, and of the properties of alkali halides and their aggregates are discussed. Results are presented of ab initio calculations of the heats of reaction of the metal-water adducts and hydroxyhydrides of Li, Be, B, Na, Mg, and Al, and of the bond lengths and angles an; the heats of reaction for the insertion of Al into HF, H2O, NH3, H2S and CH3OH, and Be and Mg into H2O. Calculations of the electron affinities and dipole moments and polarizabilities of selected gas phase alkali halide monomers and dimers are discussed, with particular attention given to results of calculations of the polarizability of LiF taking into account electron correlation effects, and the polarizability of the dimer (LiF)2.

Jordan, K. D.↗
NASA NTRS1982

Far-infrared mapping of the double-lobed H II region S106

Photometry of S106 at 50 and 100 microns, as well as its mapping with 35 arcsec resolution and a search for a nearby H2O maser source at 2 and 10 microns, have yielded data that are consistent with a 900 pc distance and an O9 (ZAMS) spectral type for a single, central exciting star. The correlation of dust temperature with optical emission, and anticorrelation of dust optical depth with optical emission, support models of S106 which envision an exciting star surrounded by a dusty disk having very low optical extinction along its approximately north-south axis. A local maximum in the dust column density was found to the west of the optical nebula, near the position of an H2O maser, although no local near- or far-IR flux maximum was detected.

Harvey, P. M.↗
NASA NTRS1982

Mesospheric water vapor

Water vapor in the earth's mesosphere has been observed at the frequency of 22.235 GHz as an absorption against the sun by utilizing a ground-based radio telescope. The H2O mixing ratio of 4.3 + or - 1 ppm is obtained in the height 40-70 km for a constant distribution model. The data are equally well represented by a photochemical model of Crutzen (1974), which was scaled by a factor of 0.93 yielding a peak mixing ratio of 6 + or - 1 ppm at 55 km. These results are 3-day averages during November 1979, where the averaging periods cover the about + or - 4 hours of the sun's transit of our meridian. The measurements are insensitive to H2O above 70 km, where the absorption is very weak. It is not possible to estimate the mixing ratios below 50 km, since the pressure broadening in the line exceeds the bandwidth of our spectrometer at the lower altitudes.

Deguchi, S.↗
NASA NTRS1982

The photochemical heating of the cometary atmosphere

A self-consistent solution of the thermodynamic structure of an H2O-dominated multispecies cometary atmosphere at 1 AU is obtained by solving the simultaneous set of differential equations representing conservation of number density, momentum, energy, and the flux of solar UV radiation in the three streams responsible for the major photolytic processes. The relative efficiency of the expansion and infrared cooling by H2O over the photolytic heating by the UV radiation in the inner coma brings about a rapid decrease in the temperature there, reaching a minimum of only about 5.4 K at a nuclear distance of approximately 54 km. Thereafter, the temperature is found to increase to about 810 K at a nuclear distance of 25,000 km, owing to higher efficiency of the photolytic heating over the cooling process. The expansion in the inner coma is seen to be highly supersonic, attaining a maximum Mach number of about 15 at the distance of temperature minimum. After that, the Mach number steadily decreases, reaching a value of about 2.3 at a nuclear distance of 25,000 km.

Marconi, M. L.↗
NASA NTRS1983

Mechanism of lubrication by tricresylphosphate (TCP)

A pin-on-disk tribometer equipped with an induction heater was used to study the coefficient of friction as a function of temperature for tricresylphosphate (TCP) on continuous vacuum melted (CVM) M-50 tool steel when the TCP was present in a liquid reservoir (bulk lubrication), and when it was applied as a liquid layer directly to the disk (limited lubrication). Under limited lubrication conditions, experiments were performed in dry ( 100 ppm H2O) air, dry ( 20 ppm H2O) nitrogen, dry nitrogen with the disks heated to 700 C then cooled to room temperature before the TCP was applied and the measurements made (preheated disks), and moist nitrogen using preheated disks. When the coefficient of friction was plotted as a function of the disk temperature, the friction decreased at a characteristic temperature, T sub r whose observed values were 265 C for bulk lubrication conditions in dry air, 225 C for limited lubrication conditions in dry air, and 215 C for limited lubrication conditions in dry nitrogen. No decrease in friction was observed with preheated disks; instead a sharp failure temperature was observed at 218 C, which was taken as the temperature about which the behavior of TCP should be judged, X-ray photoelectron spectroscopy confirmed the presence of phosphate on the surface of the iron pins used in the tribometer under TCP lubrication. Depth profile studies support the idea that a chemical reaction occurs between the TCP and the metal surface at T sub r.

Faut, O. D.↗
NASA NTRS1983

Effect of pressure on infrared spectra of ice 7

The effect of pressure on the infrared spectra of H2O and D2O ice VII was studied at room temperature and pressures between 2 and 15 GPa with a Fourier transform infrared spectrometer and a diamond anvil high pressure cell. Two librational modes, one bending mode, and various overtone bands are well resolved. The stretching modes, nu sub 1 and nu sub 3 are poorly resolved due to overlap with diamond window absorption. Differences between the spectra of H2O and D2O are discussed.

Holzapfel, W. B.↗
NASA NTRS1982

The infrared spectral properties of frozen volatiles

Since Whipple's dirty snowball model of comet nuclei, it has been generally accepted that volatile ices help to explain cometary phenomena. The infrared spectral properties of many substances that are potential candidates for frozen volatiles in the solar system are being pursued; indeed some of these frozen materials have been found in the solar system: H2O, CO2, and SO2. A review of laboratory spectra in the range 1 to 20 microns of H2O, CO2, SO2, CH4, NH3, H2S, CO, NH4HS and NH3.H2O is presented. Both reflection spectra of thick frosts and transmission spectra of thin films are shown, and their main characteristics are described. Hydrates, clathrates, and composite spectra are discussed. When it is possible to observe the nuclei of comets at close range, it may be possible to identify frozen volatiles by their infrared spectra.

Fink, U.↗
NASA NTRS1982

The photochemistry and dynamics of a dusty cometary atmosphere

The solving of a simultaneous set of differential equations representing conservation of number density, momentum, and energy together with solar radiation transfer in the streams which result in photolytic processes and the heating of the nucleus yields a self-consistent solution of the dynamical and thermal structure of an H2O-dominated two-phase dusty gas cometary atmosphere. Two models are considered for the transfer of solar radiation through the circumnuclear dust halo. The first considers only the direct extinction by the dust, and in the second the diffuse radiation field due to multiple scattering by the dust halo, which compensates for radiation removed by direct absorption when the optical depth is near unity, is approximated by neglecting the attenuation of radiation given off by the dust. It is shown that while dust attenuation has a strong effect on the H2O production rate, it also increases the electron density in the inner coma over the unattenuated case.

Marconi, M. L.↗
NASA NTRS1982

Observations of the red auroral oxygen lines in nine comets

The digital sky-subtracted spectra of nine cometary nuclei are used to measure the 6300, 6363-A Auroral red doublet of the O I forbidden line, and in view of the confinement of the cometary oxygen lines to their nuclear source, a small but variable correction for NH2 blending in different comets is made. For seven of the comets measured, and under the assumption of H2O's exclusive role as the oxygen parent, the average Q(H2O)/Q(O I) ratio is about 20. This is in excellent accord with theory, and it is conjectured that the O I production rate can be used to scale the total cometary volatile loss in even faint, distant comets. The data obtained are consistent with heliocentric production rates that vary as power laws, with n values of 2.0 for 'gassy' comets and nearer to 5.0 for dusty ones. The comets with the greatest volatile mass-loss rates all were found to have dusty spectra.

Spinrad, H.↗
NASA NTRS1983

The stability of ground ice in the equatorial region of Mars

The lifetime of an unreplenished layer of ground ice lying within 30 deg of the Martian equator was examined within the context of the existing data base on Martian regolith and climate. Data on the partial pressure of H2O in the Martian atmosphere and the range of mean annual temperatures indicated the ground ice would be restricted to latitudes poleward of 40 deg. However, the ground ice near the poles may be a relic from early Martian geologic times held in place by a thin layer of regolith. Consideration of twelve model pore size distributions, similar to silt- and clay-type earth soils, was combined with a parallel pore model of gaseous diffusion to calculate the flux of H2O molecules escaping from the subsurface ground ice layer. Martian equatorial ground ice was found to be influenced by the soil structure, the magnitude of the geothermal gradient, the climatic desorption of CO2 from the regolith. It is concluded that equatorial ground ice is present on Mars only if a process of replenishment is active.

Clifford, S. M.↗
NASA NTRS1983

Coherent anti-Stokes Raman spectroscopic modeling for combustion diagnostics

The status of modelling the coherent anti-Stokes Raman spectroscopy (CARS) spectra of molecules important in combustion, such as N2, H2O, and CO2, is reviewed. It is shown that accurate modelling generally requires highly precise knowledge of line positions and reasonable estimates of Raman linewidths, and the sources of these data are discussed. CARS technique and theory is reviewed, and the status of modelling the phenomenon of collisional narrowing at pressures well above atmospheric for N2, H2O, and CO2 is described. It is shown that good agreement with experiment can be achieved using either the Gordon rotational diffusion model or phenomenological models for inelastic energy transfer rates.

Hall, R. J.↗
NASA NTRS1983

High-resolution submillimeter-wave radiometry of supersonic flow

The recent development of a high-resolution submillimeter-wave heterodyne radiometer has made possible the first measurements of H2O molecule rotational line excitation temperatures and detailed profiles in supersonic flow. Absorption signals were measured across the flow for the 2/11/ from 2//02/ (752 GHz) para-H2O rotational transition against a hot background. These signals decrease downstream owing to the volume expansion of the gas away from the sonic nozle exit in the high-vacuum chamber. Radiative transfer calculations based on the large-velocity-gradient approximation and multilevel statistical equilibrium agree with these results and with the measured spectral line shapes. The data reveal nearly isentropic gas expansion and cooling. These studies have shown that submillimeter-wave heterodyne radiometry can be useful for remote sensing of supersonic flow with low mass flux, provided the signal transmission is through a dry or thin atmosphere.

Dionne, G. F.↗
NASA NTRS1984

Mechanism of lubrication by tricresylphosphate (TCP)

The coefficient of friction was measured as a function of temperature on a pin-on-disk tribometer. Pins and disks of 440C and 52100 steels were lubricated with tricresylphosphate (TCP), 3.45 percent TCP in squalene, and pure squalene. The M-50 pins and disks were lubricated with 3.45 percent TCP in squalene and pure squalene. Experiments were conducted under limited lubrication conditions in dry ( 100 ppm H2O) air and dry ( pp H2O) nitrogen at 50 rpm (equivalent to a sliding velocity of 13 cm sec) and a constant load of 9.8 N (1 kg). Characteristic temperatures T sub r were identified for TCP on 52100 steel and for squalene on M-50 and 52100 steels, where the friction decreased because of a chemical reaction between the lubricant and the metal surface. The behavior of squalene obscured the influence of 3.45 percent TCP solute on the friction of the system. Wear volume measurements demonstrated that wear was lowest at temperatures just above T sub r. Comparing the behavior of TCP on M-50, 440C, and 52100 steels revealed that the TCP either reacted to give T sub r behavior or produced initial failure in the temperature range 223 + or - 5 C.

Faut, O. D.↗
NASA NTRS1984

A generalized behavioral model for rotating short period comets with spectral orbital elements and axial orientation

A generalized model for short period comets is developed which integrates in a fairly rigorous manner the isolation history of regions on rotating comets with specified axial orientation and the complex feedback processes involving heat, gas and dust transport, dust mantle development and coma opacity. Attention is focused on development, reconfiguration and partial or complete launching of dust mantles and the reciprocal effects of these three processes on ice surface temperature and gas and dust production. The dust mantle controls the H2O flux not only by its effect on the temperature at the ice interface but (dominantly) by its dynamic stability which strongly influences vapor diffusivity. The model includes the effects of latitude, rotation and spin axis orientation are included and applied to an initially homogeneous sphere of H2O ice and silicate using the orbital parameters of comet Encke. Numerous variations of the model, using combinations of grain size distribution, dust-to-ice ratio, latitude and spin axis orientation, are presented and discussed. Resulted for a similar nonrotating, constant Sun orientation models are also included.

Fanale, F. P.↗
NASA NTRS1983

Measured thermal ion environment of STS-3

The Plasma Diagnostic Package (PDP) on the third Space Shuttle Flight (STS- 3) included a Bennett RF ion mass spectrometer which surveyed the positive ion composition in the vicinity of the vehicle. The ion measurements both within and exterior to the Shuttle cargo bay show the pervasive influence of the Shuttle's own gaseous emissions on its immediate plasma environment. Within the bay the ion spectrometer detected copius quantities of ions when the Shuttle was in daylight and when the gas pressure at the surface of the PDP was enhanced. In general few cases of ion detection occurred when the bay was facing toward the Shuttle wake. The plasma near the Shuttle consisted predominately of O+ (16AMU) ions and ions with atomic masses of 18, 30, 32 and 44 AMU corresponding to H2O+, NO+, O2+, and CO2+. All of these ions with the exception of H2O+ and CO2+ are expected ambient ions at the Shuttle's altitude of 240 km. During some thruster firings the 18 and 30 AMU ion concentrations detected within the bay increase by up to an order of magnitude within the 2.4 second sweep of the instrument. During these latter events the O+ distributions did not show a similar change.

Grebowsky, J. M.↗
NASA NTRS1984

Micas in experimentally shocked gneiss

Powder-propellant guns are used to shock biotites and muscovites from a gneiss at pressures between 18 and 70 GPa. It is shown that shock in biotite and muscovite can produce homogeneous and devolatilized glasses within microseconds. Shock-deformed micas are found to exhibit fracturing, kinking, and complex extinction patterns over the entire pressure range investigated. Localized melting of micas commences at 33 GPa and reaches completion at 70 GPa. Even though melted biotite and muscovite are opaque optically, they exhibit extensive microvesiculation and flow when observed with the SEM. It is confirmed through electron diffraction that biotite and muscovite have transformed to a glass. The distribution of vesicles in shock-vitrified mica reveals escape of volatiles within the short duration of the shock experiment. It is noted that experimentally shocked biotite and muscovite undergo congruent melting. It is noted that the compositions of the glasses are similar to the unshocked micas except for volatiles (H2O loss and and K loss). These unusual glasses produced from mica can be quenched by rapid cooling conditions during the shock experiment. On the basis of the results, it is pointed out that the extremely low H2O content of tektites can be reconciled with a terrestrial origin by impact.

Lambert, P.↗