Mapping of CO millimeter-wave lines in Mars' atmosphere: The spatial variability of carbon monoxide on Mars

Properties and Composition of the Terrestrial Oceans and of the Atmospheres of the Earth and Other Planets

Near-infrared spectra of a bright and a dark thermal emission feature on the night side of Venus have been obtained from 2.2 to 2.5 microns at a spectral resolution of 1200 to 1500. Both bright and dark features show numerous weak absorption bands produced by CO2, CO, water vapor, and other gases. The bright feature emits more radiation than the dark feature throughout this spectral region, but the largest contrasts occur between 2.21 s 2.32 microns, where H2SO4 clouds and a weak CO2 band provide the only known sources of extinction. The contrast decreases by 55 to 65 percent at wavelengths longer than 2.34 microns, where CO, clouds, and water vapor also absorb and scatter upwelling radiation. This contrast reduction may provide direct spectroscopic evidence for horizontal variations in the water vapor concentrations in the Venus atmosphere at levels below the cloud tops.

Spectroscopic Observations of Bright and Dark Emission Features on the Night Side of Venus

Near-infrared images of Venus, obtained from a global network of ground-based observatories during January and February 1990, document the morphology and motions of the night-side near-infrared markings before, during, and after the Galileo Venus encounter. A dark cloud extended halfway around the planet at low latitudes (>±40°) and persisted throughout the observing program. It had a rotation period of 5.5 ± 0.15 days. The remainder of this latitude band was characterized by small-scale (400 to 1000 kilometers) dark and bright markings with rotation periods of 7.4 ± 1 days. The different rotation periods for the large dark cloud and the smaller markings suggests that they are produced at different altitudes. Mid-latitudes (±40° to 60°) were usually occupied by bright east-west bands. The highest observable latitudes (±60° to 70°) were always dark and featureless, indicating greater cloud opacity. Maps of the water vapor distribution show no evidence for large horizontal gradients in the lower atmosphere of Venus.

Ground-based near-infrared imaging observations of venus during the galileo encounter.

Earth-based, earth-orbital, and spacecraft observational data are used in the present evaluation of Venus atmosphere-surface interactions to quantitatively characterize the reactions between C, H, S, Cl, F, and N gases and plausible surface minerals. Calculation results are used to predict stable minerals and mineral assemblages on the Venus surface, in order to ascertain which (if any) of the atmospheric gases are buffeted by mineral assemblages. Chemical equilibrium calculations using extant thermodynamic data on scapolite minerals predict that carbonate-bearing scapolite and sulfate meionite are unstable on the surface of Venus, while chloride-bearing scapolite is stable.

Chemistry of atmosphere-surface interactions on Venus and Mars

The Nature and Level of Formation of the Near-Infrared Features on the Venus Night Side

Near-Infrared Images of the Venus Night Side Before and After the January, 18, 1990, Inferior Conjunction

Direct Measurements of Lower Themospheric Circulation on Venus Using Doppler-Limited Infrared Spectroscopy

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The Nature and Level of Formation of the Near-Infrared Features on the Venus Night Side

Near-Infrared Images of the Venus Night Side Before and After the January, 18, 1990, Inferior Conjunction

Direct Measurements of Lower Themospheric Circulation on Venus Using Doppler-Limited Infrared Spectroscopy