The 12- to 20-micron spectrum of Venus - Implications for temperature and cloud structure

Details The 12- to 20-micron spectrum of Venus - Implications for temperature and cloud structure The 12- to 20-micron spectrum of Venus - Implications for temperature and cloud structure

May 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979icar...38..251a&link_type=abstract

Icarus, vol. 38, May 1979, p. 251-266.

Physics

3

Astronomical Spectroscopy, Atmospheric Temperature, Cloud Physics, Venus Atmosphere, Brightness Temperature, Carbon Dioxide, High Altitude, Spectrum, Venus, Carbon Dioxide, Absorption Spectra, Sulfuric Acid, Clouds, Models, Aerosols, Temperatures, Radio Occultation, Mariner 5, Mariner 10, Observations, Atmosphere, Pioneer Venus Orbiter, Infrared, Experiments, Emissions, Thermal Properties, Structure

Scientific paper

The spectrum of Venus was measured between approximately 500 and 800 kaysers (12 to 20 microns) at a resolution of 3.12 kaysers from the NASA C141 G. P. Kuiper Airborne Observatory on 22 and 24 February 1977. The spectrum clearly shows the detailed structure of CO2 absorption in the vicinity of the nu-2 fundamental band at 667 kaysers. In addition, details of model fitting demonstrate the possibility for a cold and thin haze of sulfuric acid droplets along with an optically opaque cloud top near 250 K. Such clouds represent major differences from other H2SO4 main cloud deck models in the recent literature and may be indicative of changes in the vertical distribution of aerosols on a global scale. The temperatures retrieved for pressures at or below 10 mbar are largely independent of the cloud model assumed and they are some 16 to 20 K warmer than the 1972 NASA model. All retrieved temperatures lie within the range of Mariner 5 and Mariner 10 radio occultation inversion results.

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