Spectroscopic identification of planetary cloud and haze compositions

Details Spectroscopic identification of planetary cloud and haze compositions Spectroscopic identification of planetary cloud and haze compositions

Jul 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980ceht.confq....c&link_type=abstract

American Society of Mechanical Engineers and American Institute of Chemical Engineers, Joint National Heat Transfer Conference,

Astronomy and Astrophysics

Astronomy

Astronomical Spectroscopy, Cloud Cover, Haze, Infrared Absorption, Planetary Composition, Saturn Atmosphere, Ammonia, Ice Clouds, Ice Formation, Io, Sulfur Dioxides, Voyager 1 Spacecraft

Scientific paper

Reflection spectra showing absorption bonds at 8.89, 9.40, 10.00 and 11.24 microns coincide with observed absorption features within Saturn's spectrum but only for rapid deposition of an NH3 frost layer at formation temperatures below 130 K. This suggests that Saturn's features may be due in part to an NH3 ice cloud. However, absorption features matching is not achieved if the laboratory frost layer is formed slowly or the temperature is 150 K or higher. The same premise holds true for an SO2 layer at 80 K, exhibiting an absorption band at 7.5 microns, consistent with the possible identification of such a band within the atmosphere of Io by Voyager I.

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