The revised solar abundance of iron and the solar neutrino flux
Solar core opacity influence on revised photospheric iron abundances, discussing neutrino flux prediction doubling in solar models
Watson, W. D.↗
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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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Interferometric investigations of the atmosphere of Venus
Venus atmosphere opacity law determination as function of wavelength, comparing interferometric and integrated brightness temperatures with model calculations for various atmospheric compositions
Muhleman, D. O.↗
Metal-poor stars. II - Initial horizontal- branch models
Initial horizontal branch metal poor star models, examining opacities, luminosity and cluster ages of RR Lyrae stars
Rood, R. T.↗
Venus - Determination of atmospheric parameters from the microwave spectrum
Venus atmospheric parameters from microwave spectrum, discussing brightness temperature, carbon dioxide content, opacity, water vapor, dust and models
Morrison, D.↗
Stellar structure theory
Stellar structure theory, examining particle aggregates gravitational and pressure forces, energy flow, generation and opacity and equations of state
Iben, I., Jr.↗
Partition functions in ionizing plasmas
Ionizing plasmas partition functions, determining opacities and equations of state
Fischel, D.↗
The importance of methane to pressure-induced absorption in the atmospheres of the outer planets
Pressure-induced absorption in planetary atmospheres from hydrogen-methane collisions, stressing resulting thermal opacity
Fox, K.↗
Radiation beaming in pulsars
Pulsar radiation beaming due to strong magnetic field, computing Compton scattering and opacity
Canuto, V.↗
Nematic liquid crystals for optical shutters: A concept
Nonmechanical shutter utilizes nematic crystals to attenuate illumination, thus protecting light-sensitive devices such as vidicon or image orthicon tubes and phototubes. Opacity of liquid crystals is controlled by photosensor.
Imus, R. E.↗
Photochemistry of interstellar molecules
The photochemistry of two diatomic and eight polyatomic molecules is discussed quantitatively. For an interstellar molecule, the lifetime against photodecomposition depends upon the absorption cross section, the quantum yield or probability of dissociation following photon absorption, and the interstellar radiation field. The constant energy density of Habing is used for the unobserved regions of interstellar radiation field, and the field in obscuring clouds is estimated by combining the constant flux with the observed interstellar extinction curve covering the visible and ultraviolet regions. Lifetimes against photodecomposition in the unobscured regions and as a function of increasing optical thickness in obscuring clouds are calculated for the ten species. The results show that, except for CO, all the molecules have comparable lifetimes of less than one hundred years. Thus they can exist only in dense clouds and can never have been exposed to the unobscured radiation. The calculations further show that the lifetimes in clouds of moderate opacity are of the order of one million years.
Stief, L. J.↗
Infrared Absorption of Carbon Dioxide at High Densities With Application to the Atmosphere of Venus
Several new infrared absorptions were found in carbon dioxide. All are normally forbidden, and were collision-induced in an absorbing cell whose combination of pressure and path length has a unique sensitivity for induced absorptions. The new absorptions in the 2.3 micron region are attributed to transitions from ground to the 3(1)1 Fermi pair at 4248 and 4391/cm. Other absorptions are attributed to simultaneous CO2-N2 transitions and to the 00(0)0-00(0)2 transition in CO2 polarizability derivatives and regular progressions in strength versus increasing quantum number. The spectra were used to predict the radiative transfer in a dry CO2 model of the lower Venus atmosphere. The results indicate that the radiation balance in the lower atmosphere is adequately explained by a dry massive atmosphere of CO2 with a layer of infrared-opaque clouds. The absorptions in the 2.3 micron region are significant in accounting for the opacity to sustain Venus' 768 K surface temperature.
John Fitzallen Moore↗
More solar models and neutrino fluxes.
Derivation of neutrino fluxes from a sequence of solar models that differ from one another in regard to opacity, equation of state, and nuclear cross-section factors. Using current estimates of the relevant input parameters, capture rates are obtained that range between three and ten times the most recent result of the Davis Cl 37 neutrino-capture experiment. The contribution to a theoretical capture rate due to neutrinos from all reactions other than B 8 decay ranges from 0.5 to 1.5 times the latest observational result. Comparison with results of other solar model calculations indicates reasonable agreement when results are normalized to the same input parameters.
Abraham, Z.↗
A plausible energy source and structure for quasi-stellar objects.
If a collision of two large, massive, fast gas clouds occurs, their kinetic energy is converted to radiation in a pair of shock fronts at their interface. Basic constraints imposed on such a model by observations of QSOs are considered. It is shown that a very large shock area is required if such a collision process is to provide the energy for a QSO. Details regarding the anticipated spectrum are discussed together with the opacity of the neutral clouds.
Daltabuit, E.↗
Paschen beta emission in the spectrum of Omicron Ceti.
Evaluation of three infrared spectra of Omicron Ceti obtained on Aug. 7 to 11, 1969. The equivalent width of the Paschen beta emission line in these spectra was found to vary by a factor of 2 during this time period. The variation was similar to that for H gamma and H delta as measured by Odell et al. (1970) for the same time span. The equivalent widths of Paschen beta and H gamma on August 7 were used to estimate an opacity ratio of kappa (1.28 micron)/kappa (0.43 micron) about equal to 1:30 and a molecular/atomic hydrogen ratio of about 10. The variation in the strength of Paschen beta and H delta lines is considered to be intrinsic and to have a time scale of less than or about equal to 100,000 sec.
Kovar, R. P.↗
The bulk composition of Titan's atmosphere.
Consideration of the physical constraints for Titan's atmosphere leads to a model which describes the bulk composition of the atmosphere in terms of observable parameters. Intermediate-resolution photometric scans of both Saturn and Titan, including scans of the Q branch of Titan's methane band, constrain these parameters in such a way that the model indicates the presence of another important atmospheric gas, namely, another bulk constituent or a significant thermal opacity. Further progress in determining the composition and state of Titan's atmosphere requires additional observations to eliminate present ambiguities. For this purpose, particular observational targets are suggested.
Trafton, L.↗
Stardust.
Rocket experiments were conducted to collect particles from noctilucent clouds at Kiruna, Sweden. The Pandora II inflight shadowing technique considered by Hallgren and Hemenway (1971) was used in the experiments. This technique makes it possible to study the collected particles as a function of time and altitude intervals. The particles observed consisted of an irregular electron-opaque core surrounded by a rounded, low density material. X-ray and electron opacity data suggest that the abundances of the heavy elements, such as Hf and Ta, in the particles are comparable to those of the light elements, such as Al and Si.
Hemenway, C. L.↗
Model atmospheres for cool supergiant stars.
The results of an exploratory grid of model atmospheres for cool giant stars are used to illustrate the effect of varying the chemical composition of the atmosphere. The effects of composition changes (depletion of C and O, enrichment of N, and increase in the ratio C/O), which might be expected from processing of the original material of a star through the CNO cycle of nuclear burning, are studied. The models also include the important CN opacity. They are illustrated by giving several representative T-P and T-tau diagrams, spectral energy curves, and column density tables of molecules.
Alexander, D. R.↗
Stellar evolution of high mass based on the Ledoux criterion for convection
Theoretical evolutionary sequences of models for stars of 15 and 30 solar masses were computed from the zero-age main sequence to the end of core helium burning. During the earliest stages of core helium depletion, the envelope rapidly expands into the red-supergiant configuration. At 15 solar mass, a blue loop on the H-R diagram ensues if the initial metals abundance, initial helium abundance, or C-12 + alpha particle reaction rate is sufficiently large, or if the 3-alpha reaction rate is sufficiently small. These quantities affect the opacity of the base of the outer convection zone, the mass of the core, and the thermal properties of the core. The blue loop occurs abruptly and fully developed when the critical value of any of these quantities is exceeded, and the effective temperature range and fraction of the lifetime of core helium burning during the slow phase of the blue loop vary surprisingly little. At 30 solar mass no blue loop occurs for any reasonable set of input parameters.
Stothers, R.↗