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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 361 records · Page 20
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NASA NTRS1979

Abundance of organic compounds photochemically produced in the atmospheres of the Outer Planets

Organic photochemical syntheses in the Jovian atmosphere was simulated by irradiating, at 147 nm, gaseous mixtures of methane and ammonia with varying amounts of hydrogen. Some results relevant to the photochemistry of the Jupiter atmosphere at several tens of kilometers above the clouds were obtained: (1) a favorable effect of the pressure of high amounts of H2 on the yield of hydrocarbon synthesis when NH3 is mixed with CH4; (2) a very low yield of synthesis of unsaturated hydrocarbons in such conditions; and (3) the possibility of formation of detectable amounts of HCN and CH3CN.

Raulin, F.↗
NASA NTRS1979

Minor constituents in the stratosphere and mesosphere

A review of the research in minor constituents in the stratosphere and mesosphere, carried out between 1975 and 1978, is presented. Much of the theoretical research was done with the aid of one-dimensional models. Different aspects of these models are discussed. Measurements of the chlorofluoromethanes, hydrochloric acid, nitric oxide, nitrous oxide, and hydrogen oxide were conducted. It is noted that the hydrogen oxides are now assuming a larger role in stratospheric photochemistry than have been postulated before. The effect of water vapor and the hydrogen oxides on the overall chemistry of the stratosphere was investigated theoretically, along with the possible relationship between solar activity and atmospheric ozone. The mesosphere study included ozone, water vapor, nitric oxide, and odd nitrogen investigations.

Hudson, R. D.↗
NASA NTRS1979

F-region dynamics

The U.S. research efforts in the last four years, relating to an understanding of upper atmosphere or thermosphere and F-region dynamics are reported. Simultaneous measurements of atmospheric parameters from the Atmosphere Explorer satellites were used in photochemistry and photoenergetics studies. Studies of the magnetosphere as a major source of energy and momentum for the thermosphere are outlined. Time-dependent ionosphere models which describe the thermal structure, composition, photoelectron spectrum, and airglow emissions in F-regions are discussed. Solar tides, magnetic disturbances, and gravity waves in the thermosphere are considered. It is noted that planetary explorations will help to understand scientific problems of the space environment.

Mayr, H. G.↗
NASA NTRS1979

Numerical simulation of ozone production, transport and distribution with a global atmospheric general circulation model

The production, transport, and distribution of ozone are simulated for a January with a global atmospheric general circulation model. In this model, the ozone influences the radiational heating and the photochemical ozone production and destruction, the radiational heating influences the atmospheric circulation, and the circulation redistributes the ozone. The model has simulated the synoptic and time-averaged observed large-scale fields of temperature, mass, and velocity in the troposphere and stratosphere, although with deficiencies which are seen in the time-averaged O3 distribution. Transport of ozone in the summer and winter hemispheres, in different seasons, and in various latitudes is discussed, and it is concluded that the divergence of the ozone transport maintains it below its photochemical equilibrium concentration in the tropics and subtropics, and the convergence of the ozone transport maintains it above its photochemical equilibrium concentration in the middle and high latitudes of both hemispheres. Thus, both the atmospheric motions and the O3 photochemistry determine the O3 sources and sinks.

Schlesinger, M. E.↗
NASA NTRS1979

The evolution and variability of atmospheric ozone over geological time

The rise of atmospheric O3 as a function of the evolution of O2 has been investigated using a one-dimensional steady-state photochemical model based on the chemistry and photochemistry of Ox(O3, O, O(1D)), N2O, NOx(NO, NO2, HNO3), H2O, and HOx(H, OH, HO2, H2O2) including the effect of vertical eddy transport on the species distribution. The total O3 column density was found to maximize for an O2 level of 0.1 present atmospheric level (PAL) and exceeded the present total O3 column by about 40%. For that level of O2, surface and tropospheric O3 densities exceeded those of the present atmosphere by about an order of magnitude. Surface and tropospheric OH densities of the paleoatmosphere exceeded those of the present atmosphere by orders of magnitude. It was also found that in the O2-deficient paleoatmosphere, N2O (even at present atmospheric levels) produces much less NOx than it does in the present atmosphere.

Levine, J. S.↗
NASA NTRS1979

The effect of paleoatmospheric ozone on surface temperature

Photochemical and radiative-convective calculations are performed to evaluate the influence of ozone in determining the surface temperature of the paleoatmosphere prior to the buildup of molecular oxygen to its present atmospheric level. Possible effects of atmospheric dynamics on the photochemistry and thermal structure of the paleoatmosphere are neglected, and the present atmospheric values are assumed for the tropospheric water-vapor relative-humidity distribution and lapse rate as well as for the fractional cloud amount and cloud reflectivity. It is found that the radiative effects (at IR and solar wavelengths) of ozone for a molecular oxygen level of one-tenth the present atmospheric level resulted in a globally averaged surface-temperature increase of about 4.5 K for the present solar constant. Implications of the results for paleoclimate are briefly considered.

Levine, J. S.↗
NASA NTRS1979

Thermal structure and relaxation rates of the perturbed atmosphere - A study with a photochemical radiative convective model

A radiative-photochemical model is developed to evaluate the temperature distribution in the earth's atmosphere between the ground and 70 km. The model takes into account the interaction between photochemistry and temperature. Results are reported for a number of experiments performed with this model to assess the climatic effects of varying the ozone distribution and the ozone overburden. An evaluation of the relaxation rates of both ozone and temperature is also reported. In particular, the importance of the ozone distribution with respect to the greenhouse effect is further investigated.

Alimandi, G.↗
NASA NTRS1979

Energy transduction in Halobacterium halobium

The properties and functions of the light-energy-transducing purple membrane of Halobacterium halobium are reviewed. Consideration is given to the protein structure and composition of the membrane and the photochemistry of the protein-retinal complex known as bacteriorhodopsin. The role of bacteriorhodpsin in establishing and maintaining an electrochemical (H(+)) gradient is examined, and interactions of this gradient with Na(+) and K(+) gradients, the light-induced transport of amino acids and the light-induced phosphorylation of ADP are considered. Bacteriorhodopsin and the respiratory chain are discussed as alternative sources of energy for the maintenance of the H(+) gradient. Advantages of the Halobacterium purple membrane system for studies of membrane energetics and the confirmation of the chemiosmotic hypothesis are also noted.

Lanyi, J. K.↗
NASA NTRS1978

The chemistry of Venus' atmosphere

A model for the Venus atmosphere involving photochemistry of oxygen, hydrogen, chlorine and sulfur species is presented. Sulfur reaction schemes and hydrogen and chlorine reaction schemes were included. The impact of sulfur on the oxygen budget and the subsequent production of H2SO4 molecules for the Venus cloud deck were explored. A major new reaction scheme for production of H2SO4 molecules involving sulfur and oxygen chemistry was established shown to dominate over the odd hydrogen scheme proposed earlier. The efficiency of the scheme in formation of H2SO4 is only about 50%, with the remaining sulfur residing in SO2 molecules. The calculated downward flux of H2SO4 may be sufficient to maintain a steady state sulfuric acid cloud if the resident time of H2SO4 droplets in the cloud is as long as a few years. If however, the resident time is half a year or shorter, additional chemistry capable of more efficient conversion of SO2 to SO3 is required.

Sze, N. D.↗
NASA NTRS1980

The stratcom 8 effort

The ozone-nitrogen oxides ultraviolent flux interactions were investigated to obtain data on stratospheric photochemistry. The balloon, rocket, and aircraft operations are described along with the instruments, parameter measurements, and payloads.

Reed, E. I.↗
NASA NTRS1980

Studies of the earth-limb absorptions in the near ultraviolet

The use of solar occultation techniques as a means of obtaining data on the photochemistry of the ozone layer was investigated. A spectrometer equipped with a photomultiplier detector and associated electronics necessary to amplify the output of the detector up to a level suitable for on-board recording and also for telemetering to the ground, was packaged with a solar telescope and flown by balloon in order to obtain solar spectra in the region between 3080 A and 3100 A with a resolution of close to 0.05 A. Data reduction techniques required to remove solar OH lines from atmospheric OH line spectra are described as well as the instrument package.

Murcray, D. G.↗
NASA NTRS1979

Organic chemistry on Titan

Features taken from various models of Titan's atmosphere are combined in a working composite model that provides environmental constraints within which different pathways for organic chemical synthesis are determined. Experimental results and theoretical modeling suggest that the organic chemistry of the satellite is dominated by two processes: photochemistry and energetic particle bombardment. Photochemical reactions of CH4 in the upper atmosphere can account for the presence of C2 hydrocarbons. Reactions initiated at various levels of the atmosphere by cosmic rays, Saturn 'wind', and solar wind particle bombardment of a CH4-N2 atmospheric mixture can account for the UV-visible absorbing stratospheric haze, the reddish appearance of the satellite, and some of the C2 hydrocarbons. In the lower atmosphere photochemical processes will be important if surface temperatures are sufficiently high for gaseous NH3 to exist. It is concluded that the surface of Titan may contain ancient or recent organic matter (or both) produced in the atmosphere.

Chang, S.↗
NASA NTRS1980

Atmospheric bromine and ozone perturbations in the lower stratosphere

The role of bromine compounds in the photochemistry of the natural and perturbed stratosphere has been reexamined using an expanded reaction scheme and the results of recent laboratory studies of several key reactions. The most important finding is that through the reaction BrO + ClO yielding Br + Cl + O2 there is a synergistic effect between bromine and chlorine which results in an efficient catalytic destruction of ozone in the lower stratosphere. One-dimensional photochemical model results indicate that BrO is the major bromine species throughout the stratosphere, followed by BrONO2, HBr, HOBr and Br. It is shown from the foregoing that bromine is more efficient than chlorine as a catalyst for destroying ozone, and the implications for stratospheric ozone of possible future growth in the industrial and agricultural use of bromine are discussed. Bromine concentrations of 20 pptv (2 x 10 to the -11th power), as suggested by recent observations, can decrease the present-day integrated ozone column density by 2.4%, and can enhance ozone depletion from steady-state chlorofluoromethane release at 1973 rates by a factor of 1.1-1.2.

Yung, Y. L.↗
NASA NTRS1980

Observations of the spectrum of Jupiter from 1500 to 2000 A with the IUE

The paper examines the far-UV spectrum of Jupiter recorded by observations with the International Ultraviolet Explorer, noting that only the upper levels of the plant's atmosphere are sampled. It is shown that there are several absorptions caused by C2H2 and indications that NH3 may also be present at these altitudes. In addition, it is suggested that PH3 may also play a role as a continuum absorber, and a new upper limit of 5 x 10 to the -9 on H2S/H2 forbidden line ratio. It is concluded that these results are consistent with existing models for Jovian photochemistry and atmospheric structure.

Owen, T.↗
NASA NTRS1980

Possible existence and chemistry of ClO.O2 in the stratosphere

The influence of the existence and chemistry of the possible atmospheric constituent ClO.O2 on current models of stratospheric photochemistry is discussed. It is suggested that the formation of an asymmetric ClO.O2 complex may explain the observed suppression of the quantum yield in the chlorine-photosensitized decomposition of ozone in the presence of O2, and that the presence of the ClO.O2 formed may account for the current discrepancy between measurements and theoretical predictions of stratospheric ClO mixing ratio profiles. The presence of stratospheric ClO.O2 is also invoked as a possible mitigating influence on present estimates of ozone destruction due to chlorofluoromethane release.

Prasad, S. S.↗
NASA NTRS1980

Stratospheric free chlorine measured by balloon-borne in situ resonance fluorescence

Eight balloon-borne in situ measurements of ClO in the stratosphere are analyzed and are compared with recent model calculations. While the use of in situ stratospheric studies of free radicals to test models by comparing observed and predicted concentration profiles is essential for a prognosis of changes in stratospheric ozone, resulting from future changes in stratospheric ozone, such studies provide only limited insight into the nature of stratospheric photochemistry, because natural variability and the large number of fast reactions which compete in the coupling among the key radicals frustrate a detailed comparison between a mean distribution provided by the models and an instantaneous distribution provided by a single observation.

Anderson, J. G.↗
NASA NTRS1980

The ultraviolet dayglow. I - Far UV emissions of N and N2

Far ultraviolet rocket spectra of N I and N2 dayglow emissions have been analyzed by using AE-E photoelectron spectra, laboratory-measured excitation cross sections, and photochemical models of atomic nitrogen. A self-consistent picture of both optically thick and thin emission features is found by using a model in which the principal production mechanism for N I 1200-A and 1493-A photons is photodissociative excitation of N2. The aeronomic data require that 50-70% of the excited 4 P atoms produced dissociatively have velocities within the Doppler core of the ambient nitrogen atoms, contrary to the expectation that those atoms are produced with large excess kinetic energy. The derived atomic nitrogen density has a maximum density of 2.7 x 10 to the 7th per cu cm at 170 km, a value that is within 40% of that from recent models of odd nitrogen photochemistry.

Meier, R. R.↗
NASA NTRS1980

Neutral cometary atmospheres. I - An average random walk model for photodissociation in comets

A method for constructing physically realistic photochemical models, taking into account the isotropic ejection of dissociated molecular fragments as well as radiation pressure acceleration, has been developed using Monte Carlo techniques. The effect of the isotropic ejection, as opposed to the radial motion arbitrarily assumed in Haser's model, is adequately described by a simple average random walk model. It is shown that measured radial (Haser) scale lengths are in fact only lower limits to a range of possible true scale lengths for a given brightness profile, which explains the current discrepancies between observed scale lengths and those predicted by photochemistry.

Combi, M. R.↗