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At least 397 records · Page 22
All sourcesNASA NTRSDOE OSTI
NASA NTRS1972

Climatic modification by CO2, H2O, and aerosol

Research is reported on the effects of increasing the CO2, aerosols, and water content of the atmosphere on the surface temperature and climatology. An atmospheric model is described with the incoming solar radiation for a planetary albedo of 33 percent, surface temperature of 288 K, relative humidity of 75 percent, cloud cover of 48 percent, CO2 of 0.3 parts per thousand, and aerosol density of two million per square centimeter. The results show that if the CO2 increases by a factor of 1000 or more, the total pressure of the atmosphere increases, and the earth may become as hot as Venus. It is also shown that as the amount of dust particles in the atmosphere increases, the solar radiation decreases, and the surface temperature lowers.

Rasool, I.↗
NASA NTRS1971

The strengths of H2O lines in the 8200 A region and their application to high dispersion spectra of Mars.

The improvement in the quality of spectroscopic plates taken in recent years in the search for water vapor in the atmosphere of Mars has dictated the need for improved laboratory data with which to interpret the spectra. This paper presents the results of measurements of the strengths of 41 lines of the 8200 A (211) water vapor band. The measured values show evidence of vibration-rotation interactions on the line intensities, beyond the principal stretching effect.

Farmer, C. B.↗
NASA NTRS1972

Ion dipole capture cross sections at low ion and rotational energies - Comparison of integrated capture cross sections with reaction cross sections for NH3 and H2O parent-ion collisions.

The numerical capture cross section is calculated from the capture ratio, defined as the fraction of trajectories reaching a prescribed minimum separation of 3 A. The calculated capture cross sections for a rotational temperature of 77 K suggest large reaction cross sections in 80 K experiments for the large dipole-moment target, methyl cyanide.

Dugan, J. V., Jr.↗
NASA NTRS1972

Theoretical interpretation of the Venus 1.05-micron CO2 band and the Venus 0.8189-micron H2O line.

The synthetic-spectrum technique was used in the analysis. The synthetic spectra were constructed with a model which takes into account both isotropic scattering and the inhomogeneity in the Venus atmosphere. The Potter-Hansen correction factor was used to correct for anisotropic scattering. The synthetic spectra obtained are, therefore, the first which contain all the essential physics of line formation. The results confirm Potter's conclusion that the Venus cloud tops resemble terrestrial cirrus or stratus clouds in their scattering properties.

Regas, J. L.↗
NASA NTRS1972

Mars - Are observed white clouds composed of H2O.

A total of 252 occurrences of white clouds are studied. Water abundances are compared with those of white clouds as a function of latitude on Mars. It appears not necessarily to be the case that observed cloud frequencies will always follow water abundances. Martian white cloud frequencies tend to follow the distribution of water both seasonally and latitudinally on the planet, which strongly suggests that most white clouds are formed from water vapor.

Wells, R. A.↗
NASA NTRS1973

Mars: Mariner 9 spectroscopic evidence for H2O ice clouds

Spectral features observed with the Mariner 9 Interferometer Spectrometer are identified as those of water ice. Measured spectra are compared with theoretical calulations for the transfer of radiation through clouds of ice particles with variations in size distribution and integrated cloud mass. Comparisons with an observed spectrum from the Tharsis Ridge region indicate water ice clouds composed of particles with mean radius 2.0 microns and integrated cloud mass 0.00005 g/sq cm.

Curran, R. J.↗
NASA NTRS1973

Electron impact excitation of H2O.

The authors (1971) detected a new triplet state of water at 9.81 eV energy, and assigned the low energy-loss feature to the excitation of low-lying triplet state(s) of water on the basis of the angular distribution of the scattered electrons. The results are discussed here in more detail, as well as relative differential cross sections for elastic scattering, and for the excitation of these and several other electronic and pure vibrational states of water at impact energies of 15, 20, and 53 eV and at scattering angles ranging from 0 to 90 deg.

Trajmar, S.↗
NASA NTRS1974

The chemisorption of H2O, HCOOH and CH3COOH on thin amorphous films of Al2O3

Investigation of the irreversible chemisorption of water, formic acid and acetic acid on a thin amorphous aluminum oxide film, using inelastic tunneling spectroscopy. All of the tunnel junctions employed were Al-Al2O3-Pb junctions with the adsorbate on the Al2O3 surface between the Al2O3 and the Pb electrode. The results obtained include the finding that all Al2O3 surfaces prepared by oxidation of Al have free CH groups present on them.

Lewis, B. F.↗
NASA NTRS1975

Measurement of Raman spectra of H2O and SO4(-) in seawater

A study of applying laser Raman spectroscopy to remote sensing of the sulfate ion in sea water is in progress. The SO4 Raman spectrum has been obtained from true sea water samples in the laboratory using a CW laser Raman spectrometric system. Radiometric calculations indicate the feasibility of obtaining usable SO4 Raman signals in a field experiment. One of serious difficulties expected in the field experiment would be from fluorescence of phytoplankton and organics.

Houghton, W. M.↗
NASA NTRS1974

D/H and O-18/O-16 ratios of H2O in the 'rusty' breccia 66095 and the origin of 'lunar water'

A number of the rocks brought back from the Apollo 16 mission had a faint 'rusty' coating. It has been suggested that this coating might be hydrated iron oxide. A study was conducted of a sample of the lunar rock 66095, on which the 'rusty' coating was particularly prominent. An analysis showed that the sample contained between 20 and 40 micromoles of water per gram of rock. Taking into account aspects of isotopic composition and other factors, it is concluded that the water found in the analysis is probably not of lunar origin.

Epstein, S.↗