The spectrum of Saturn from 1990 to 2230/cm - Abundances of AsH3, CH3D, CO, GeH4, NH3, and PH3

Details The spectrum of Saturn from 1990 to 2230/cm - Abundances of AsH3, CH3D, CO, GeH4, NH3, and PH3 The spectrum of Saturn from 1990 to 2230/cm - Abundances of AsH3, CH3D, CO, GeH4, NH3, and PH3

Jan 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991icar...89..168n&link_type=abstract

Icarus (ISSN 0019-1035), vol. 89, Jan. 1991, p. 168-189.

Computer Science

48

Abundance, Ammonia, Carbon Monoxide, Infrared Spectra, Methane, Phosphines, Saturn Atmosphere, Visible Spectrum, Arsenic Compounds, Computerized Simulation, High Resolution, Vertical Distribution, Saturn, Spectra, Abundance, Carbon Monoxide, Ammonia, Gases, Models, Absorption, Vertical Distribution, Enrichment, Phosphine, Arsine, Earth-Based Observations, Infrared, Wavelengths, Laboratory Studies, Spectroscopy, Diagrams, Clouds, Thermal Properties, Radiation, Deuterium, Gemane, Procedure, Silane, Oxygen, He

Scientific paper

An analysis is presented of the abundances and vertical distributions of all known absorbers in the 5-micron spectrum of Saturn, in view of previously unpublished observations, synthetic spectra of each atmospheric constituent, and an atmospheric model for synthesizing Saturn's spectrum in order to make comparisons with observations. The model used encompasses the abundances of all gaseous absorbers, their vertical distributions, clouds, and the thermal and reflected solar components of planetary flux. A coherent understanding is in this way obtained of both the many variables affecting Saturn's 5-micron spectrum and the similarities between Jupiter and Saturn.

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