NOTE: Upper Limits for Condensed O_2 on Saturn's Icy Satellites and Rings

Details NOTE: Upper Limits for Condensed O_2 on Saturn's Icy Satellites and Rings NOTE: Upper Limits for Condensed O_2 on Saturn's Icy Satellites and Rings

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998icar..136..349s&link_type=abstract

Icarus, Volume 136, Issue 2, pp. 349-352.

Physics

3

Scientific paper

New 4800-7200 A spectra of Saturn's rings, and the icy saturnian satellites Enceladus, Tethys, Dione, Rhea, and Iapetus, do not show the weak 5773 and 6275A absorption bands due to high-density condensed O_2 that are seen, with a maximum depth of 1.8%, on Ganymede's trailing side. The 5773A band depth must be <=0.6% (and very probably <=0.3%) on the rings, Tethys, Dione, Rhea, and the trailing side of Iapetus, and <=1.2% on the trailing side of Enceladus. The lack of detectable absorption does not rule out abundant O_2 molecules that are separated too well to produce these absorption bands. The observations show that the presence of O_3, recently detected on Rhea and Dione (Noll et al. 1997b, Nature 388, 45-47), does not require the presence of detectable quantities of high-density O_2. I discuss the implications of the new observations for models of O_2 formation on Ganymede.

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