Venus cloud properties: Infrared opacity and mass mixing ratio |
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| Authors: | RE Samuelson RA Hanel LW Herath VG Kunde WC Maguire |
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| Institution: | Laboratory for Planetary Atmospheres, Goddard Space Flight Center, Greenbelt, Maryland 20771, USA |
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| Abstract: | By using the Mariner 5 temperature profile and a homogeneous cloud model, and assuming that CO2 and cloud particles are the only opacity sources, the wavelength dependence of the Venus cloud opacity is infrared from the infrared spectrum of the planet between 450 and 1250 cm?1. Justification for applying the homogeneous cloud model is found in the fact that numerous polarization and infrared data are mutually consistent within the framework of such a model; on the other hand, dense cloud models are not satisfactory.Volume extinction coefficients varying from 0.5 × 10?5 to 1.5 × 10?5 cm?1, depending on the wavelength, are determined at the tropopause level of 6110 km. By using all available data, a cloud mass mixing ratio of approximately 5 × 10?6 and a particle concentration of about 900 particles cm?3 at this level are also inferred. The derived cloud opacity compares favorably with that expected for a haze of droplets of a 75% aqueous solution of sulfuric acid. |
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