Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1981
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....94..382b&link_type=abstract
Astronomy and Astrophysics, vol. 94, no. 2, Feb. 1981, p. 382-390.
Astronomy and Astrophysics
Astrophysics
31
Atmospheric Models, Atmospheric Scattering, Infrared Spectra, Line Spectra, Methane, Saturn Atmosphere, Anisotropy, Atmospheric Pressure, Atmospheric Temperature, Clouds (Meteorology), Computer Programs, Haze, Hydrogen, Microwave Interferometers, Radiation Absorption, Saturn, Atmosphere, Methane, Models, Interferometry, Spectrum, Data, Scattering, Comparisons, Clouds, Temperatures, Infrared, Wavelengths, Emissions, Pressure, Optical Properities, Thickness, Layers, Hydrogen, Element Ratios, Particles, Anisot
Scientific paper
We investigate in this paper constraints on models of the Saturn atmosphere given by the shapes of CHβ lines near 1.1 μ in an interferometric spectrum (effective limit of resolution: 0.2 cm-1). A new study of this spectral range in the laboratory (Pierre et al., 1980; de Bergh et al., 1980) allows us to consider numerous CH4 lines in addition to the 3ν3 lines, which were the only lines included in all previous analyses of the region 1.1 in Saturn spectra. The widening of the range of CH4 line intensities appears to improve the determination of the atmospheric parameters significantly. For a classical model including a clear atmosphere above a haze layer and a dense cloud below the haze, the range of possible values for the pressure at the top of the haze is restricted by our analysis to 0.17 ± 0.06 atm. The obtained values of the CH4/H2 ratio are more uncertain but they exclude the solar value (C/H =4.7 10-4; Lambert, 1978); we find (4±2) 10-3 for the CH4/H2 ratio in Saturn.
Buriez Jean-Claude
de Bergh Catherine
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