The atmospheric composition and structure of Jupiter and Saturn from ISO observations: a preliminary review

Details The atmospheric composition and structure of Jupiter and Saturn from ISO observations: a preliminary review The atmospheric composition and structure of Jupiter and Saturn from ISO observations: a preliminary review

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999p%26ss...47.1225e&link_type=abstract

Planetary and Space Science, Volume 47, Issue 10-11, p. 1225-1242.

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Scientific paper

Infrared spectra of Jupiter and Saturn have been recorded with the two spectrometers of the Infrared Space Observatory (ISO) in 1995-1998, in the 2.3-180 μm range. Both the grating modes (R=150-2000) and the Fabry-Pérot modes (R=8000-30,000) of the two instruments were used. The main results of these observations are (1) the detection of water vapour in the deep troposphere of Saturn; (2) the detection of new hydrocarbons (CH3C2H, C4H2, C6H6, CH3) in Saturn's stratosphere; (3) the detection of water vapour and carbon dioxide in the stratospheres of Jupiter and Saturn; (4) a new determination of the D/H ratio from the detection of HD rotational lines. The origin of the external oxygen source on Jupiter and Saturn (also found in the other giant planets and Titan in comparable amounts) may be either interplanetary (micrometeoritic flux) or local (rings and/or satellites). The D/H determination in Jupiter, comparable to Saturn's result, is in agreement with the recent measurement by the Galileo probe (Mahaffy, P.R., Donahue, T.M., Atreya, S.K., Owen, T.C., Niemann, H.B., 1998. Galileo probe measurements of D/H and 3He/4He in Jupiters atmosphere. Space Science Rev. 84 251-263) the D/H values on Uranus and Neptune are significantly higher, as expected from current models of planetary formation.

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