Title: An Expanded Theoretical Interpretation of the Venus 1.05-MICRON co, Line and the Venus 0.8226-MICRON h, O Line
Abstract: view Abstract Citations (7) References (20) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS An Expanded Theoretical Interpretation of the Venus 1.05-MICRON co, Line and the Venus 0.8226-MICRON h, O Line Regas, James L. ; Giver, Lawrence P. ; Boese, Robert W. ; Miller, Jacob H. Abstract We have reanalyzed lines in the 1 .05- CO2 band using the synthetic spectrum technique and the revised Mariner 5 atmospheric structure. Our Venus model atmosphere takes into account both isotropic scattering and inhomogeneity. The revised Mariner 5 atmospheric structure does not substantially modify the scattering properties of our earlier cloud models determined with the preliminary Mariner 5 atmospheric structure. The anisotropic scattering mean free path for our single-cloud-layer models at the 0.2 atm level is about 0.17 km, a value typical of terrestrial cirrus or stratus clouds. We find that the two-layer model of Hunt requires an anisotropic scattering mean free path at the 0.2-atm level of 0.01 km, a value similar to that for terrestrial cumulus clouds. We find that the observed 0.8226- H2O line requires an H2O volume mixing ratio in the range 1.5 x 10- to 4.8 x 10-' and permits an aqueous HCl solution cloud at the 10-16 mb level, a location which puts the cloud in the cold trap at 80 km indicated by the revised Mariner data. We conclude that an HCl solution cloud over either a series of condensation cloud layers or a dust cloud or perhaps some combination of dust and condensation cloud layers is consistent with all of the CO2 spectroscopic data. Subject headings: atmospheres, planetary - planets - spectra, planetary - Venus Publication: The Astrophysical Journal Pub Date: October 1973 DOI: 10.1086/152426 Bibcode: 1973ApJ...185..383R full text sources ADS |