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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.

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At least 343 records · Page 19
All sourcesNASA NTRSDOE OSTI
NASA NTRS1973

Product distributions and rate constants for ion-molecule reactions in water, hydrogen sulfide, ammonia, and methane

The thermal energy, bimolecular ion-molecule reactions occurring in gaseous water, hydrogen sulfide, ammonia, and methane have been identified and their rate constants determined using ion cyclotron resonance methods. Absolute rate constants were determined for the disappearance of the primary ions by using the trapped ion method, and product distributions were determined for these reactions by using the cyclotron ejection method. Previous measurements are reviewed and compared with the results using the present methods. The relative rate constants for hydrogen-atom abstraction, proton transfer, and charge transfer are also determined for reactions of the parent ions.

Huntress, W. T., Jr.↗
NASA NTRS1974

The abundance of ammonia on Jupiter, Saturn and Titan

From recent spectra of Jupiter, Saturn and Titan in the 6450-A band of NH3, new values of the abundance of ammonia are derived for Jupiter and Saturn. NH3 abundances of 13 plus or minus 3 m-Am on Jupiter and 2 plus or minus 1 m-Am on Saturn were found. High resolution profiles of NH3 lines on Jupiter are used to estimate a pressure of 2.1 atm at the line formation level in the Jovian atmosphere. In the case of Titan, an NH3 abundance of less than 2 m-Am was found. The implications of these results are discussed.

Encrenaz, T.↗
NASA NTRS1975

Optical constants of solid ammonia in the infrared

No direct measurements of the refractive index for solid ammonia could be obtained because of failures in attempts to map the reflection spectrum. Kramers-Kronig techniques were, therefore, used in the investigation. The subtractive Kramers-Kronig techniques employed are similar to those discussed by Ahrenkiel (1971). The subtractive method provides a more-rapid convergence than the conventional techniques when data are available over a limited spectral range.

Robertson, C. W.↗
NASA NTRS1975

Ultraviolet optical constants of water and ammonia ices

A method reported by Tempelmeyer and Mills (1968) for the determination of real refractive indices of transparent films was used in the investigation. It was found that the fringe period for a transparent film can be used to approximate the period for a semitransparent film near its extremum. The experimental apparatus is discussed along with details regarding the employed technique. Graphs are presented concerning the refractive index and the absorption coefficients for amorphous water ice and amorphous ammonia ice.

Browell, E. V.↗
NASA NTRS1976

Shuttle ECLSS ammonia delivery capability

The possible effects of excessive requirements on ammonia flow rates required for entry cooling, due to extreme temperatures, on mission plans for the space shuttles, were investigated. An analysis of worst case conditions was performed, and indicates that adequate flow rates are available. No mission impact is therefore anticipated.

Source record↗
NASA NTRS1976

Measurement of hydrogen- and self-broadened half-widths of ammonia at 200 and 300 K

The hydrogen- and self-broadened half-widths have been measured for the (nu1 + nu2) and (nu2 + nu3) bands of ammonia at 300 and 207 K. Measurement of hydrogen-broadened widths has been restricted to J and K values not exceeding 6, but that of self-broadened widths is done for a few lines outside that range. Assuming a power-law dependence of half-width on temperature, the average value of the index alpha for the lines measured is found to be 0.57 for hydrogen broadening.

Margolis, J. S.↗
NASA NTRS1976

Spectral properties of hydrogen, helium, methane, and ammonia at thermal infrared wavelengths

The paper presents some results of a theoretical and laboratory program to determine the thermal infrared spectral properties of the principal gaseous constituents of the atmosphere of Jupiter. Birnbaum (1975) has measured laboratory spectra in the 16- to 1000-micron wavelength range for hydrogen and hydrogen-helium mixtures at Jovian temperatures. These are compared with theoretically computed spectra in order to determine the temperature dependence of the line strengths in the pressure-induced rotational band and the overlap parameters from the translational band. Existing spectral data for methane do not agree well with measurements of the nu 4 band at room temperature. A revised allocation of line intensities is proposed. Existing data for the nu 2 (10-micron) band of ammonia agree reasonably well with measurements at room temperature and at -77 C, but there are some important discrepancies which remain to be explained.

Taylor, F. W.↗
NASA NTRS1977

Ammonia-compatible elastomers and alloys

Study examines and reports positive findings from suitability tests of metal alloys, Inconel 718 and Ti-6A1-4V and elastomers, Ethylene propylene terpolymer rubbers, for utilization in storage vessels, fluid lines, and other system components subjected to continuous immersion in liquid anhydrous ammonia.

Bantrell, M. T.↗
NASA NTRS1977

Infrared heterodyne spectrometer measurements of vertical profile of tropospheric ammonia and ozone

Remote sensing of the concentration and vertical distribution of atmospheric gases has been carried out using a dual CO2 laser multichannel infrared heterodyne spectrometer (IHS). The high specificity and nearly quantum-noise-limited sensitivity of the IHS provide the capability of scanning individual signature lines of selected atmospheric constituents in the 9 to 11 micron region. A comprehensive investigation of the spectral overlap between CO2 laser local oscillator transitions and selected atmospheric constituents was performed; measurements of the atmospheric absorption of solar radiation from the ground were carried out at selected laser transitions for ammonia and ozone.

Peyton, B. J.↗
NASA NTRS1977

Analysis of the nu3 + nu4 band of ammonia

The 2-micron band of ammonia has been studied in the laboratory with a spectral resolution of 0.05/cm. Most of the strong lines, belonging to the nu3 + nu4 (perpendicular) band have been identified and spectroscopic constants have been derived.

Sarangi, S.↗
NASA NTRS1977

Effect of ammonia on Swiss albino mice

Times to incapacitation and death and LC /50/ values were determined for Swiss albino male mice exposed to different concentrations of ammonia in a 4.2 liter hemispherical chamber. The LC/50/ for a 30 minute exposure was 21,430 ppm.

Hilado, C. J.↗
NASA NTRS1978

Measurement of solar radiation at ground level in the region 1950-2150 A using ammonia actinometry

The use of ammonia as an actinometer for measurement of the solar flux in the region 1950-2150 A is presented. The solar flux was found to be 270 million photons/sq cm per sec at ground level in this wavelength interval in an area with minimum overhead ozone concentration. The advantages of this method over previously used methods are discussed, and the results are related to the present estimates of the tropospheric photodissociation rates for the freons CFCl3 and CF2Cl2 by radiation in this wavelength region.

Knoot, P.↗
NASA NTRS1978

A determination of Jovian ammonia abundance based on a 2 micron spectrum

A spectrum of Jupiter in the two-micron region has been analyzed to determine the Jovian ammonia abundance. The result is approximately 4 cm-amagat, assuming an airmass factor of 2.5 and a single effective reflecting layer for this wavelength. This is compared with the abundances observed at other wavelengths.

Sarangi, S.↗
NASA NTRS1980

Design, fabrication and testing of a dual catalyst ammonia removal system for a urine VCD unit

A three-man capacity catalytic system for the recovery of water from urine was designed, constructed, and tested, it was designed to operate with feed streams containing high concentrations of urine vapor and only 5 to 7% of oxygen for the oxidation of ammonia and volatile organic vapor.It can operate either in a flow-through or a recycle mode and is capable of accepting the urine vapor produced by a vapor compression distillation evaporator. Testing consisted of short preliminary and optimization test, an endurance test of 74 hours continuous operation, and recycle tests using both air and oxygen. The system was designed for a urine processing rate of 0.86 liters/hr; however, it was tested at rates up to 1.2 liter/hr. Untreated urine evaporated by an electrically heated evaporator was used. The quality of the recovered water meets the U.S. Drinking Water Standards, with the exception of a low pH. Accumulation of solids in the urine sludge is reduced to approximately 65% of the anticipated value.

Budinikas, P.↗
NASA NTRS1980

Ammonia in the atmospheres of Saturn and Jupiter

A profile and equivalent width for the 6451.1-A feature of the 6450-A band of ammonia at the equator and south pole of Saturn have been measured. Estimates for the NH3 abundance at the center of the disk which vary from 0.4 to 5 m-am, depending upon the atmospheric model used, lead to uncertainties in the NH3/H2 ratio which are greater than a factor of 10. Half-widths for theoretical line profiles computed from models in which the NH3 absorption occurs at a pressure level of 1.0 atm agree with the observed profiles. NH3/H2 ratios have been obtained which range from 0.00001 to 0.00002 for Jupiter.

Smith, W. H.↗
NASA NTRS1980

Infrared observations of circumstellar ammonia in OH/IR supergiants

Ammonia has been detected in the circumstellar envelopes of VY Canis Majoris, VX Sagittarii, and IRC +10420 by means of several absorption lines in the nu-2 vibration-rotation band near 950 kaysers. The line profiles are well resolved (0.2 km/sec resolution) and show the gas being accelerated to terminal expansion velocities near 30 km/sec. The observations reveal a method for determining the position of the central star on VLBI maps of OH maser emission to an accuracy of approximately 0.2 arcsec. A firm lower limit of 2 x 10 to the 15th/sq cm is obtained for the NH3 column density in VY Canis Majoris.

Mclaren, R. A.↗
NASA NTRS1981

Study of the ammonia ice cloud layer in the Equatorial Region of Jupiter from the infrared interferometric experiment on Voyager

Spectra from the Voyager 1 infrared interferometer spectrometer (IRIS) obtained near the time of closest approach to Jupiter were analyzed for the purpose of inferring ammonia cloud properties associated with the Equatorial Region. Comparisons of observed spectra with synthetic spectra computed from a radiative transfer formulation, that includes multiple scattering, yielded the following conclusions: (1) very few NH3 ice particles with radii less than 3 microns contribute to the cloud opacity; (2) the major source of cloud opacity arises from particles with radii in excess of 30 microns; (3) column particle densities are between 1 and 2 orders of magnitude smaller than those derived from thermochemical considerations alone, implying the presence of important atmospheric motion; and (4) another cloud system is confirmed to exist deeper in the Jovian troposphere.

Marten, A.↗
NASA NTRS1982

Spectra of ammonia

Developments in the spectral analysis of ammonia are highlighted. Experimental techniques of diode laser spectroscopy were reviewed. It is shown that diode lasers give much better spectral resolution than even Fourier transform spectroscopy.

Rao, K. N.↗