Engineering Papers⌕ Search

SEARCH · Engineering Papers

Results for “CH4”

Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

Quote a phrase for an exact phrase match. Source license links do not imply unrestricted reuse.

At least 1,081 records · Page 60
All sourcesNASA NTRSDOE OSTI
NASA NTRS1977

Whole-disk polarization measurements of Uranus at visible wavelengths

The whole-disk polarization of Uranus was measured over two apparitons in blue and red light. The blue polarization becomes negative near the 0.5-deg phase, indicating non-Rayleigh scattering. The red polarization phase curve shows positive polarization smaller than suggested by Rayleigh scattering models. An explanation of these data is that the blue and red radiation is scattered by the CH4 haze layer that has been suggested to reside high in the atmosphere of Uranus. As expected, there is no whole-disk circular polarization, an observation which confirms other observations and theoretical predictions.

Michalsky, J. J.↗
NASA NTRS1976

Light element geochemistry of the Apollo 15 site

Abundances of C, N, S, and He and contents of CH4 and metallic Fe at Hadley-Apennine are typical of a mixed mare and highland environment. Isotopic compositions of C, N, and S similarly conform in most cases to patterns observed elsewhere on the moon. Systematic relationships between S abundance and total Fe content are apparent for crystalline rocks from most landing sites but their full significance is not yet understood.

Kaplan, I. R.↗
NASA NTRS1976

The escape of solar-wind carbon from the moon

About 8 tons of solar-wind carbon is implanted in the lunar soil each year. This inflow is adequate to supply the present regolith carbon abundance (about 100 ppm) in 1-m thickness of soil per billion years. However, the present meteor flux is only capable of mixing to a depth of 10 cm over a billion-year period. As a result, soil mixing cannot act to assimilate the total influx of carbon in the soil. It is necessary that most of the carbon influx be balanced by escape. Model atmospheres for three candidate gases, CH4, CO, and CO2, have been computed. Each model is sized to provide the needed escape rate.

Hodges, R. R., Jr.↗
NASA NTRS1977

Ion cyclotron resonance studies of some reactions of N/+/ ions

Product distributions and rate constants for the reactions of ground-state N(+) ions with CO, NO, CO2, and CH4 were measured. Rate constants were obtained using ion-cyclotron-resonance trapped-ion methods, and product distributions were obtained using a tandem (Dempster-ICR) mass spectrometer. Rapid nitrogen isotope exchange was also observed in N(+)-N2 collisions.

Anicich, V. G.↗
NASA NTRS1977

The upper ionosphere of Titan

Photoionization of the upper atmosphere of Titan by sunlight is expected to produce a substantial ionospheric layer. One-dimensional forms of the mass, momentum, and energy conservation equations for ions and electrons have been solved along with electron number densities of about 1000/cu cm, using various model atmospheres. The significant ions in a CH4-H2 atmosphere are H(+), H3(+), CH5(+), CH3(+), and C2H5(+). Electron temperatures may be as high as 1000 K, depending on the abundance of hydrogen in the high atmosphere. Interaction of the solar wind with the ionosphere is also discussed.

Whitten, R. C.↗
NASA NTRS1977

Observations of exoelectron emission associated with heterogeneous catalysis

It is suggested that the exoelectron emission from the catalyst may be used to monitor the rate of oxidation of CO and CH4 over palladium catalysts. Indirect heating of the catalyst and atmospheric pressure have no effect upon this monitoring system. Although the mechanism relating catalysis to exoelectron emission is not clear, it is considered possible that electron emission is triggered by the adsorption-desorption cycle.

Hoenig, S. A.↗
NASA NTRS1977

On the 6825 A band of methane as observed in Uranus and Neptune

A high-resolution spectrum of the series of lines near 6825 A presumably due to CH4 has been obtained for Uranus. The line spacings are in agreement with the previous observations of Owen (1966), Bergstralh (1975), and Belton and Hayes (1975) but not with the laboratory observations reported by Lutz and Owen (1976). It is proposed that the transitions identified by Lutz and Owen are not correlated one-to-one with those features observed in the planets. Wavelength differences of up to 0.8 A are found between the laboratory and planetary features, where the resolving power allows one to specify the line positions to better than + or - 0.07 A. The spectrum obtained for Neptune is in essential agreement with that for Uranus.

Gelfand, J.↗
NASA NTRS1977

Indirect observation of unobservable interstellar molecules

It is suggested that the abundances of neutral nonpolar interstellar molecules unobservable by radio astronomy can be systematically determined by radio observation of the protonated ions. As an example, observed N2H(+) column densities are analyzed to infer molecular nitrogen abundances in dense interstellar clouds. The chemistries and expected densities of the protonated ions of O2, C2, CO2, C2H2, and CH4 are then discussed. Microwave transition frequencies for HCO2(+) and C2H3(+) are estimated, and a preliminary astronomical search for HCO2(+) is described.

Herbst, E.↗
NASA NTRS1977

Uranus - Limb and polar brightening at 7300 A

Pinhole photoelectric area-scanning photometry of the Uranus disk demonstrates directly the existence of both limb and polar brightening in the 7300 A CH4 band. Polar brightening, which appears to be present also at continuum wavelengths, is interpreted as being caused by scattering in a thin aerosol haze located over the polar region.

Franz, O. G.↗
NASA NTRS1977

A comment on methanogenic bacteria and the primitive ecology

As the phenotype of methanogenic bacteria is suggested to have been one of the major factors creating a dynamic balance between CO2 and CH4 in the primitive atmosphere, these organisms are thought to be very ancient. Their antiquity may be further postulated by comparative characterization of their ribosomal RNA. Accepting this antiquity, it is concluded that a carbon-dioxide-methane cycle, driven by photosynthesis, was the major carbon cycle in primitive ecology, and that photosynthesis and methanogens were thus contemporaneous.

Woese, C. R.↗
NASA NTRS1977

Reforming of glucose and wood at the critical conditions of water

Reforming of organics in aqueous solutions is being investigated as a potential waste treatment process. Earlier studies showed that glucose in water reacts to form a gaseous mixture of CO, H2, CH4, CO2, C2H6, and C2H4 in the vicinity of the critical conditions of water (374 C, 22 MPa). The earlier work has been extended to determine the effect of variations in temperature and feed concentration on the extent of gasification. The percent gasification decreases with increasing feed concentration, indicating an overall kinetic order less than unity. Surprisingly, the percent gasification decreases with increasing temperature. A number of preliminary experiments were conducted with maple sawdust feed, which was thought to be representative of complex organic wastes from paper and vegetable matter. Once again, no solid products were found under the critical conditions; the percent gasification ranged from 16 to 88 percent, depending on the feed composition and residence time.

Modell, M.↗
NASA NTRS1977

Gaseous sodium sulfate formation in flames and flowing gas environments

Formation of Na2SO4(g) in flames and hot flowing gas systems was studied by high pressure, free-jet expansion, modulated molecular beam mass spectrometric sampling. Fuel-lean CH4-O2 flames doped with SO2, H2O and NaCl yielded the gaseous Na2SO4 molecule in residence times of less than one millisecond. Intermediate species NaSO2(g) and NaSO3(g) were also observed and measured. Composition profiles were obtained for all reaction products. Non-flame flowing gas experiments showed that Na2SO4 and NaSO3 gaseous molecules were formed at 1140 C in mixtures of O2, H2O(g), SO2 and and NaCl(g). Experimental results are compared with calculated equilibrium thermodynamic predictions.

Stearns, C. A.↗
NASA NTRS1977

Tripropellant engine study

Work conducted was devoted to three main tasks. Thermochemical equilibrium performance data were assembled to establish the expected performance calculations of the mode 1 engine propellant combinations and thermodynamic and transport data for the products of combustion. Turbine drive gas characteristics were also established. Thrust chamber and nozzle cooling studies were devoted to the evaluation of H2, C3H8, CH4, and RP-1 as coolants in the existing SSME cooling circuit geometry. It was found that all these candidate coolants are feasible without limiting the desired operating conditions with the exception of RP-1, which would limit the maximum P(c) to 2000 psia. RP-1 could be used, however, to cool the nozzle only without imposing the chamber pressure limit. A total of 15 candidate engine system cycles were selected and a preliminary engine system balance was conducted for 12 of these systems to establish component operating flowrates, pressures and temperatures. It was found that the staged combustion cycles employing fuel rich LOX/hydrocarbon turbine drive gases are power limited.

Wheeler, D. B.↗
NASA NTRS1977

Atlas of Infrared Absorption Lines

This atlas of infrared absorption line contains absorption line parameters (line strength vs. wavenumber) from 500 to 7000 cm(exp-1) for 15 gases: H2O, CO2, O3, N2O, CO, CH4, O2, SO2, NO, NO2, NH3, HCl, HF, HNO3 and CH3Cl.

Park, J. H.↗
NASA NTRS1978

Stratospheric sounding by infrared heterodyne spectroscopy

Intensity profiles of infrared spectral lines of stratospheric constituents can be fully resolved with a heterodyne spectrometer of sufficiently high resolution. The constituents' vertical distributions can then be evaluated accurately by analytic inversion of the measured line profiles. Estimates of the detection sensitivity of a heterodyne receiver are given in terms of minimum detectable volume mixing ratios of stratospheric constituents, indicating a large number of minor constituents which can be studied. Stratospheric spectral line shapes, and the resolution required to measure them are discussed in light of calculated synthetic line profiles for some stratospheric molecules in a model atmosphere. The inversion technique for evaluation of gas concentration profiles is briefly described and applications to synthetic lines of O3, CO2, CH4 and N2O are given.

Abbas, M. M.↗
NASA NTRS1977

Inhomogeneous models of the atmosphere of Saturn

Ultraviolet spectra and absorption band measurements of H2, CH4 and NH3 at visible and near-infrared wavelengths are referred to in developing an inhomogeneous atmospheric model for Saturn. The atmospheric model includes a clear gas layer which lies above an absorbing particle layer surmounting an ammonia haze layer. The distribution of particles in the atmosphere, the radiative transfer calculations, and atmospheric mixing are considered. Comparisons are made with an atmospheric model of Saturn based on infrared observations.

Macy, W.↗
NASA NTRS1977

Production of simple molecules on the surface of Mercury

Lunar sample studies have shown that solar-wind irradiation of the lunar surface has produced a variety of low-molecular-weight compounds. Analysis of the lunar soils has revealed the presence of H2, CH4, H2O, N2, CO, CO2, He, Ne and other components which are extralunar. Irradiation experiments on lunar materials and analogs have shown that solar-wind and solar-flare irradiation of the lunar surface produces selected low-molecular-weight components. Solar-wind irradiation of Mercury's surface should also produce a wide variety of low-molecular-weight species because of the increased solar flux, which results from Mercury being nearer the sun than the moon. The thermal regime of Mercury's surface would result in thermal evaporation of low-temperature components followed by 'cold-trapping' on the night-time side of the planet. Such desorption-adsorption processes assist chemical weathering of Mercury's regolith.

Gibson, E. K., Jr.↗
NASA NTRS1978

Raman scattering in the atmospheres of the major planets

A technique is developed to calculate the detailed effects of Raman scattering in an inhomogeneous anisotropically scattering atmosphere. The technique is applied to evaluations of Raman scattering by H2 in the atmosphere of the major planets. It is noted that Raman scattering produces an insufficient decrease in the blue and ultraviolet regions to explain the albedos of all planets investigated. For all major planets, the filling-in of solar line cores and the generation of the Raman-shifted ghosts of the Fraunhofer spectrum are observed. With regard to Uranus and Neptune, Raman scattering is seen to exert a major influence on the formation and profile of strong red and near infrared CH4 bands, and Raman scattering by H2 explains the residual intensity in the cores of these bands. Raman scattering by H2 must also be taken into account in the scattering of photons into the cores of saturated absorption bands.

Cochran, W. D.↗