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At least 163 records · Page 9
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NASA NTRS1972

Toxic Hazards Research Unit annual technical report, 1972

The activities of the Toxic Hazards Research Unit (THRU) for the period of June 1971 through May 1972 are reviewed in this report. Acute inhalation toxicity experiments were conducted on hydrogen chloride (HCl) gas and aerosol, ethyl bromide (C2H5Br), hydrogen bromide (HBr), hydrogen sulfide (H2S), ammonia (NH3), chlorine (CL2), and silane (SiH4). Subacute toxicity studies were conducted on chlorine pentafluoride (ClF5), dichloromethane (CH2Cl2) and coal tar volatiles. Further toxicity studies of subacute and chronic responses to inhaled monomethylhydrazine (MMH) are also described.

Macewen, J. D.↗
NASA NTRS1973

Carbon chemistry of Luna 16 and Luna 20 samples.

Luna 16 and Luna 20 samples were analyzed for volatilizable species using vacuum pyrolysis to 1400 C. The major gaseous products evolved (ranging from 10-650 micrograms/g) were H2O, CO, CO2, N2 and CH4. Minor components (all less than 10 micrograms/g) included NH3, HCN, NO, SO2, H2S, C2H2, C2H4, C2H6, C3H6 and higher hydrocarbons, benzene, toluene, and the polymeric contaminants Teflon and silicone oil. The total carbon and nitrogen contents (micrograms/g) for these sieved samples were: Luna 16 - C 418, N 134 and Luna 20 - C 380, N 80.

Simoneit, B. R.↗
NASA NTRS1974

Pre-resonance Raman spectra of some simple gases

The pre-resonance Raman spectra of SO2, N2O, and H2S were investigated using the 4880 A, 4727 A, and 4579 A lines of the argon ion laser. Although these molecules have electronic absorption bands in the near ultraviolet, none exhibit any pre-resonance enhancement within our experimental error of + or - 10%. Possible explanations taking into account the current theories for resonance Raman are discussed.

Low, P. W.↗
NASA NTRS1976

New upper limits for atmospheric constituents on Io

A spectrum of Io from 0.86 to 2.7 microns with a resolution of 3.36 per cm and a signal to rms noise ratio of 120 is presented. No absorptions due to any atmospheric constituents on Io could be found in the spectrum. Upper limits of 0.12 cm-atm for NH3, 0.12 cm-atm for CH4, 0.4 cm-atm for N2O, and 24 cm-atm for H2S were determined. Laboratory spectra of ammonia frosts as a function of temperature were compared with the spectrum of Io and showed this frost not to be present at the surface of Io. A search for possible resonance lines of carbon, silicon, and sulfur, as well as the 1.08-micron line of helium, proved negative. Upper emission limits of 60, 18, 27, and 60 kilorayleighs, respectively, were established for these lines.

Fink, U.↗
NASA NTRS1976

Laboratory reflection spectra for the determination of chemical composition of ice bodies

The visible (0.3 to 1.03 microns) spectral reflectances of N2O, NH3, H2S, and NH4HS frosts and mixtures of these frosts as well as their UV-irradiated products have been measured. These spectra are compared with the spectra of the Galilean satellites of Jupiter, Saturn's rings, and Saturn's satellites to place limits on their surface compositions.

Lebofsky, L. A.↗
NASA NTRS1976

Absolute rate of the reaction of O/3-P/ with hydrogen sulfide over the temperature range 263 to 495 K

The technique of flash photolysis coupled with time resolved detection of O via resonance fluorescence has been used to obtain rate constants for the reaction of O(3-P) with H2S at temperatures from 263 to 495 K and at pressures in the range 10-400 torr. Under conditions where secondary reactions are avoided, the measured rate constants for the primary step obey the Arrhenius equation k = (7.24 plus or minus 1.07) x 10 to the -12th exp(-3300 plus or minus 100/1.987 T) cu cm/molecules/s. Experiments with D2S show that the reaction exhibits a primary isotope effect, in support of a hydrogen abstraction mechanism.

Whytock, D. A.↗
NASA NTRS1976

Hydrogen-induced slow crack growth of a plain carbon pipeline steel under conditions of cyclic loading

The investigation described was aimed at establishing the degree of compatibility between a plain carbon pipeline-type steel and hydrogen and also hydrogen-rich environments containing small additions of H2S, O2, H2O, CO, CO2, CH4, and natural gas at pressures near 1 atm. Test were carried out under conditions of static and cyclic loading; the subcritical crack growth was monitored. The rates of crack growth observed in the hydrogen and hydrogen-rich environments are compared with the crack rate observed in a natural gas environment to determine the compatibility of the present natural gas transmission system with gaseous hydrogen transport.

Nelson, H. G.↗
NASA NTRS1976

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

Product distributions and rate constants for the reaction of ground state C(+) ions with O2, NO, HCl, CO2, H2S, H2O, HCN, NH3, CH4, H2CO, CH3OH, and CH3NH2 have been measured. Rate constants were obtained using ion cyclotron resonance trapped ion methods, and product distributions were obtained using a tandem mass spectrometer. Rapid carbon isotope exchange has also been observed in C(+)-CO collisions.

Anicich, V. G.↗
NASA NTRS1977

Atomic and molecular fluorescence as a stratospheric species monitor

The results of an investigation are presented evaluating the potential of atomic and molecular fluorescence as a stratospheric monitor of the concentrations of any one of 18 minor species: Cl, Cl2, ClO, ClO2, CO, H2, HCHO, HCl, HNO2, HNO3, H2S, NH3, NO, NO2, N2O, O, OH, and SO2. All spectral regions from the vacuum ultraviolet through the infrared were included. It was found that suitable systems can be constructed for the stratospheric monitoring of CO (5 ppb), NO2 (less than 1 ppb), OH (0.2 ppt), and O (50-200 ppt). The fluorescence sensitivities for Cl (0.5-1.0 ppt), H2 (0.2 ppm at 10 torr) and SO2 (1-10 ppb) are marginally insufficient with current technology.

Schofield, K.↗
NASA NTRS1977

On the sources of ultraviolet absorption in spectra of Titan and the outer planets

In response to observations of the ultraviolet deficiencies shown by all of the outer planets and Titan, models have been proposed to explain the low albedos in terms of absorption by particles in the upper atmospheres of these objects. These particles are generally believed to be photochemically formed from gases in the upper atmospheres, primarily methane and hydrogen. Such processes may also be operative on Titan. Results of some laboratory experiments on proton irradiation of mixtures of gases including CH4, H2, and NH3 have shown that liquid and solid materials are produced that are strong ultraviolet absorbers. However, the material produced from the CH4 + H2 mixture was colorless, indicating that species containing elements other than carbon and hydrogen are necessary for the production of color. Two such elements are nitrogen (as NH3 or N2) and sulfur (as H2S); colored materials have been produced from such mixtures. None of these materials has spectral properties identical to those shown by the planets. Therefore it is necessary that mixtures (and/or cloud layers) of the photochemical materials be present.

Scattergood, T.↗
NASA NTRS1977

The sodium and hydrogen gas clouds of Io

Models are developed to describe the spatial distribution of gases emitted by Io and are applied to recent observations which indicate extensive gas clouds of hydrogen and sodium in orbit around Jupiter. Hydrogen and sodium atoms are emitted from Io with velocities in the range from 2 to 3 km/sec, with fluxes of about 10 billion and 100 million per sq cm/sec for hydrogen and sodium, respectively. Hydrogen atoms may be formed by photodecomposition of gases such as NH3 or H2S released from the satellite surface and may escape thermally from an exosphere whose temperature is about 500 K. Sodium may be ejected from the surface by energetic particles or by ultraviolet radiation, and it appears that a nonthermal mechanism drawing energy from Jupiter's magnetic field is required in order to account for its release to space.

Smyth, W. H.↗
NASA NTRS1977

Ultraviolet observations of Mars and Saturn by the TD1A and OAO-2 satellites

Ultraviolet photometric and spectrophotometric observations of Mars and Saturn, obtained from two earth-orbiting satellites, are discussed. High-resolution data reveal no definite absorption features in the spectra of either planet. In order to reconcile the absence of a prominent absorption in the Mars data near 2150 A with preliminary Viking measurements of NO, this gas must be preferentially concentrated at high Martian altitudes. Broadband photometry from OAO-2 shows that atmospheric dust from the great dust storm of 1971-1972 on Mars reduced the ultraviolet geometric albedo by a factor of 3 at the height of the storm. Atmospheric energy deposition appears to be an important mechanism of the storm dynamics. The combined Saturn data indicate that NH3 is not the absorber that influences the UV spectrum of Saturn. The possibility that H2S is the absorber is investigated.

Caldwell, J.↗
NASA NTRS1978

Upper limits to trace constituents in Jupiter's atmosphere from an analysis of its 5 micrometer spectrum

A high-resolution spectrum of Jupiter at 5 micrometers recorded at the Kuiper Airborne Observatory is used to determine upper limits to the column density of 19 molecules. The upper limits to the mixing ratios of SiH4, H2S, HCN, and simple hydrocarbons are discussed with respect to current models of Jupiter's atmosphere. These upper limits are compared to expectations based upon the solar abundance of the elements. This analysis permits upper limit measurements (SiH4), or actual detections (GeH4) of molecules with mixing ratios with hydrogen as low as 10 to the minus 9th power. In future observations at 5 micrometers the sensitivity of remote spectroscopic analyses should permit the study of constituents with mixing ratios as low as 10 to the minus 10th power, which would include the hydrides of such elements as Sn and As as well as numerous organic molecules.

Treffers, R. R.↗
NASA NTRS1979

Tholins - Organic chemistry of interstellar grains and gas

The paper discusses tholins, defined as complex organic solids formed by the interaction of energy - for example, UV light or spark discharge - with various mixtures of cosmically abundant gases - CH4, C2H6, NH3, H2O, HCHO, and H2S. It is suggested that tholins occur in the interstellar medium and are responsible for some of the properties of the interstellar grains and gas. Additional occurrences of tholins are considered. Tholins have been produced experimentally; 50 or so pyrolytic fragments of the brown, sometimes sticky substances have been identified by gas chromatography-mass spectrometry, and the incidence of these fragments in tholins produced by different procedures is reported.

Sagan, C.↗
NASA NTRS1978

Selective photodestruction of alpha-amino acids

A problem encountered in the analysis of amino acids in chemical evolution experiments and in extracts of meteorites is the large number present. A method for selectively destroying the alpha-amino acids, with only the beta- and gamma-amino acids remaining in the solution, is described. The amino acids used were racemic, with one milliliter of solution containing 0.0000025 mol of each acid irradiated in a 1-cm quartz cell having 254-nm monochromatic light in the presence of CuCl2. Excess H2S was added to precipitate the Cu (2+) as CuS. A gas chromatographic analysis was used to observe that irradiation with 254-nm light in the presence of Cu (2+) destroyed all the amino acids except the beta and the gamma types. It is concluded that with such a procedure, complex mixtures of amino acids can be simplified to make identification by GC mass spectrometry easier.

Levi, N.↗
NASA NTRS1978

Reactions of OH/+/ and H2O/+/ ions with some diatomic and simple polyatomic molecules

The rate constants and product distributions of the reactions of OH(+) and H2O(+) with some diatomic and simple polyatomic molecules were studied by ion cyclotron resonance (ICR) mass spectrometric techniques. Reaction rates with CO, NO, O2, N2, CO2, H2S, N2O, H2CO, CH4 and CD4 were measured. Charge transfer and proton transfer were generally observed in cases for which the reaction channel is exothermic, but processes involving rearrangement were not found.

Karpas, Z.↗
NASA NTRS1978

An ion cyclotron resonance study of reactions of some atomic and simple polyatomic ions with water

Reactions of various positive ions with water vapor were studied by ion cyclotron resonance mass spectrometric techniques. Rate constants and product distributions were determined for reactions of the ions: Ar(+), Co(+), N2(+), and CO2(+), CH2(+), and CH4(+), CH2Cl(+), HCO(+), H2CO(+), H2COH(+), H2S(+) and HS(+). The results obtained in this work are compared with earlier reported data where available.

Karpas, Z.↗
NASA NTRS1978

Reactively evaporated films of copper molybdenum sulfide

Films of superconducting Chevrel-phase copper molybdenum sulfide CuxMo6S8 were deposited on sapphire substrates by reactive evaporation using H2S as the reacting gas. Two superconducting temperatures (10.0 K and 5.0 K) of the films were found, corresponding to two different phases with different copper concentrations. All films were superconducting above 4.2 K and contained Chevrel-phase compound as well as free molybdenum. The critical current was measured as a function of applied field. One sample was found to deviate from the scaling law found for co-evaporated or sputtered samples, which possibly indicates a different pinning mechanism or inhomogeneity of the sample.

Chi, K. C.↗