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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 253 records · Page 14
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NASA NTRS1974

Electronic-to-vibrational energy transfer efficiency in the O/1 D/-N2 and O/1 D/-CO systems

With the aid of a molecular resonance fluorescence technique, which utilizes optical pumping from the v = 1 level of the ground state of CO by A 1 Pi-X 1 Sigma radiation, a study is made of the efficiency of E-V transfer from O(1 D) to CO. O(1 D) is generated at a known rate by O2 photodissociation at 1470 A in an intermittent mode, and the small modulation of the fluorescent signal associated with CO (v = 1) above the normal thermal background is interpreted in terms of E-V transfer efficiency. The CO (v = 1) lifetime in this system is determined mainly by resonance trapping of the IR fundamental band, and is found to be up to ten times longer than the natural radiative lifetime. For CO, (40 plus or minus 8)% of the O(1 D) energy is converted into vibrational energy. By observing the effect of N2 on the CO (v = 1) fluorescent intensity and lifetime, it is possible to obtain the E-V transfer efficiency for the system O(1 D)-N2 relative to that for O(1 D)-CO. The results indicate that the efficiency for N2 is (83 plus or minus 10)% of that for CO.

Slanger, T. G.↗
NASA NTRS1974

Chlorine-bearing molecules in interstellar clouds

The reaction Cl(+) + H2 yielding HCl(+) + H is rapid, and it leads to the formation of the molecules HCl(+), H2Cl(+), and HCl. It may be possible to detect HCl(+) near 3600 A, and HCl may be observable at 1291 A. Also, photodissociation of HCl(+) may be a significant source of protons within clouds, and chemical heating resulting from the destruction of chlorine-bearing molecules may account for perhaps 1-10 per cent of the expected cooling from diffuse interstellar clouds.-

Jura, M.↗
NASA NTRS1974

Dual photon effects in nitrogen dioxide photolysis

A previous study demonstrated two-photon consecutive absorption as being the most probable mechanism for the photodissociation of NO2 using a pulsed ruby laser at 6943 A. Additional data discussed here confirmed this and also examined an associated phenomenon, that of multiphoton induced fluorescence. The dissociation of NO2 by ON-O bond cleavage requires 3.4 eV, while the laser energy corresponds to 1.785 eV. The pooling of the energy of two photons would give more than enough energy to dissociate the NO2 into NO + O. Several mechanisms including (1) simultaneous absorption of two photons; (2) reaction of two singly excited NO2; (3) reaction of a singly excited NO2 with a ground state NO2; and (4) consecutive absorption of two photons were examined.

Hakala, D.↗
NASA NTRS1974

Model systems for life processes on Mars

In the evolution of life forms nonphotosynthetic mechanisms are developed. The question remains whether a total life system could evolve which is not dependent upon photosynthesis. In trying to visualize life on other planets, the photosynthetic process has problems. On Mars, the high intensity of light at the surface is a concern and alternative mechanisms need to be defined and analyzed. In the UV search for alternate mechanisms, several different areas may be identified. These involve activated inorganic compounds in the atmosphere, such as the products of photodissociation of carbon dioxide and the organic material which may be created by natural phenomena. In addition, a life system based on the pressure of the atmospheric constituents, such as carbon dioxide, is a possibility. These considerations may be important for the understanding of evolutionary processes of life on another planet. Model systems which depend on these alternative mechanisms are defined and related to presently planned and future planetary missions.

Mitz, M. A.↗
NASA NTRS1974

Vacuum UV photolysis of N2O

Emission from N2 B (3 Pi g) and O(1 S) produced during vacuum UV irradiation of N2O was studied as a function of the wavelength of the incident radiation. Two different processes were responsible for producing N2(B 3 Pi g) close to its production threshold. One process formed B 3 Pi g molecules directly and one indirectly via an unidentified precursor having a lifetime about 27 microsec. The quantum yield of O(1 S) atoms produced by photodissociation of N2O was determined as a function of incident photon energy. This yield is near 100% at 129 nm.

Mcewan, M. J.↗
NASA NTRS1975

The electron density in the direction of zeta Oph

It is shown that photoionization of vibrationally excited H2 and photodissociation of the H2(+) ions produced thereby constitute a significant electron production route in high UV flux situations. A significant fraction of the electron density in the direction of zeta Oph (-15 km per sec cloud) deduced from observations may be expected to arise in this way.

Stecher, T. P.↗
NASA NTRS1976

The neutral coma of comets: A review

The hypothesis that water snow controls the vaporization of the nucleus of some comets seems verified from the general order of magnitude of the size of their nucleus and of their nuclear albedo; the largest observed production rates are H and OH which both seem to originate from the photodissociation of H2O, as also confirmed by the scale length of the invisible parent molecule producing OH. However, comet Encke is not uniformly covered by water snow, as it produces only one tenth of the expected vaporization. Early results on comet Kohoutek suggest that the conclusions could be slightly different for some of the new comets in Oort's sense. If the far ultraviolet observations confirm the early assessments of the production rates of C, O and H, then at least another major constituent competing with water has not yet been detected. Such a major constituent is suggested by the ratios C/O = 0.24 and H/O = 2.5.

Delsemme, A. H.↗
NASA NTRS1976

Gas phase chemistry in comets

The significance of gas phase reactions in determining the nuclear structure of comets is discussed. The sublimation of parent molecules such as H2O, CH4, CO2, and NH3 from the surface of the nucleus and their subsequent photodissociation and ionization in forming observed cometary molecular species are elaborated.

Oppenheimer, M.↗
NASA NTRS1976

Analysis of NH spectrum

The A3Pi to X3Sigma- transition of NH is a common feature of cometary spectra. Since the NH molecule is likely to be formed by photodissociation of molecules such as ammonia or hydrazine, identifying the final states of the photolysis would shed light on the identity of the parent. It is shown that the transition rate for the a 1Delta to X3Sigma- transition is sufficiently fast to deplete any a1Delta concentration formed in the original photolysis process. This analysis focused on experimental spectra obtained for the comet Kohoutek. The fluorescence pumping of the NH molecule is calculated for November 29, 1973 and January 25, 1974 using the model of radiative equilibrium which assumes no collisions.

Krauss, M.↗
NASA NTRS1976

Cooling and recombination processes in cometary plasma

The ion electron plasma in comets is examined for cooling processes which result from its interactions with the neutral coma. A cometary coma model is formulated that is composed predominantly of H2O and its decomposition products where electrons are cooled in a variety of processes at rates varying with energy. It is shown that solar plasma plus accumulated cometary ions and electrons is affected very strongly as it flows into the coma. The electrons are rapidly cooled and all but some 10% of the ions undergo charge exchange. Photodissociation of H2O is assumed where ion electron recombination is the dominant loss process.

Wallis, M. K.↗
NASA NTRS1976

In situ measurements of the mesosphere and stratosphere

The operation of a subsonic, Gerdien condenser probe for in situ measurements of the mesosphere and stratosphere is presented. The inclusion of a flashing Lyman alpha ultraviolet source provides an artifically produced ionization of particular constituents. Detailed theory of operation is presented and the data results from two flights are shown. A great deal of fine structure in mobility is observed due to the presence of various hydrated positive ions. The effect of the Lyman alpha source in the 35 km region was to dissociate a light hydrate ion rather than produce additional ionization. At the 70 km region, photodissociation of the heaviest ions (probably ice crystals) was also observed.

Crosky, C.↗
NASA NTRS1975

Ultraviolet remote sensing of atmospheric ozone from payloads using Shuttle capabilities

Previous atmospheric ozone observations using an ultraviolet double monochromator to measure the absorption of back-scattered solar radiation between 255 nm and 340 nm have provided information on the global total ozone distribution as well as its vertical profile. This information can be used to structure the comprehensive ozone observations that are needed to provide a better understanding of ozone formation and destruction mechanisms. Some potential ozone threats, especially that from photodissociation of fluorocarbons, make Shuttle-based observations especially timely. Because of the nature of the global ozone-transport process, measurements must be performed from space on a global scale with sufficient resolution and accuracy to determine the total amount of atmospheric ozone. A better understanding of ozone processes in global regions inaccessible from previous platforms is needed to complete this ozone data base. This paper describes the potential for Shuttle payloads to provide the required information.

Krueger, A. J.↗
NASA NTRS1975

Stratospheric distributions of odd nitrogen and odd hydrogen in a two-dimensional model

A two-dimensional pole-to-pole chemical model of the stratosphere is developed which extends from 8 to 38 km in altitude. Atmospheric motions are simulated by mean vertical and meridional winds and eddy diffusion coefficients. Seasonally averaged distributions of important odd nitrogen (NO, NO2, and HNO3) and odd hydrogen (H, OH, HO2, H2O2) compounds are computed. Photodissociation of N2O leads to production of odd nitrogen in the stratosphere, and the odd nitrogen is ultimately removed by downward transport into the troposphere and by rain-out (modeled by a rain-out lifetime of 30 days below 8-km altitude). Results are presented for a quasi-steady state in which seasonal cycles repeat themselves. These results show significant latitudinal as well as vertical variations in the predicted species which emphasize the need for at least two dimensions in accurate stratospheric modeling. Computed concentrations are compared with observations when they exist.

Prinn, R. G.↗
NASA NTRS1976

Diurnal and seasonal variations in atomic and molecular oxygen inferred from Atmosphere Explorer-C

Mass-spectrometer measurements of O and N2, obtained with the Atmosphere Explorer-C satellite during December 1974 and January 1975, are used to derive the O2 concentration near 250 km from several ionization reactions. In order to separate temperature effects from diffusion effects, the measured O and inferred O2 concentrations are employed to determine, under the assumption of diffusive equilibrium, the O/N2 and O2/N2 ratios at 120 km. It is found that the latitudinal and diurnal variations in the O concentration at 120 km are consistent with previous results obtained with OGO 6 and that the O2 concentration in the Northern (winter) Hemisphere is about twice as high as that in the Southern (summer) Hemisphere. The possible importance of photodissociation in the diurnal O2 variations is discussed.

Mayr, H. G.↗
NASA NTRS1975

Absorption coefficient of HCl in the region 1400 to 2200 A

The results of absorption coefficient measurements of HCl in the region 1400 to 2200 A are reported and compared with those previously published. It is concluded that the present results represent the best compromise of all measurements and should be used for any calculations on the photodissociation rate of HCl in planetary atmospheres.

Inn, E. C. Y.↗
NASA NTRS1976

Nitric oxide formation by meteoroids in the upper atmosphere

The process of nitric oxide formation during atmospheric entry of meteoroids is analyzed theoretically. An ablating meteoroid is assumed to be a point source in a uniform flow with a continuum regime evolving in its wake. The amount of nitric oxide produced by high-temperature reactions of air in the continuum regime is calculated by numerical integration of chemical-rate equations. The results, when summed over the observed mass, velocity, and entry-angle distributions of meteoroids, provide annual global production rates of nitric oxide as a function of altitude. The peak production of nitric oxide is found to occur at altitudes between 90 and 100 km, the total annual rate being about 40 million kg. The present results suggest that the large concentration of nitric oxide observed below 95 km could be attributed to meteoroids instead of photodissociation of nitrogen.

Menees, G. P.↗
NASA NTRS1976

The structure of cometary ionospheres. I - H2O dominated comets

A hydrodynamic description of the density distributions of the ionic products of H2O and CO in the atmosphere of an H2O-dominated comet having 10% CO is given. Two models are discussed. In the first, the effecs of photodissociation, photoionization, and gas-phase reactions are considered. In the second, the effect of an internal ionization source is also included. It is found that while the observed morphology of the H2O(+) coma of Comet Kohoutek (1973f) cannot be explained by gas-phase reactions alone, it is consistent with the presence of a strong internal source of ionization, presumably an electric current flowing through the inner coma. In the latter case the number densities of H2O(+) and CO(+) remain more or less constant within the scale lengths against collisional dissociation by the electron flux of their neutrals. While the abundance ratio of CO(+) to H2O(+) remains considerably less than unity when the internal ionization source is neglected, it is significantly larger than unity when the internal ionization source is included. Consequently, even the so-called 'CO-rich' comets may in reality be H2O-dominated, provided a strong internal source of ionization is operative.

Ip, W.-H.↗
NASA NTRS1976

Radiative processes affecting the abundance of interstellar OH

Photodissociation of OH dominates its destruction for a significant range of density and shielding in H I regions. Although inverse predissociation may provide an observable flux of ultraviolet recombination photons, it can provide only a small fraction of the total observed OH in most H I regions.

Smith, w. H.↗