Detection of H 2 18O in Jupiter

Details Detection of H 2 18O in Jupiter Detection of H 2 18O in Jupiter

Nov 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...453l..49n&link_type=abstract

Astrophysical Journal Letters v.453, p.L49

Astronomy and Astrophysics

Astronomy

4

Infrared: Solar System, Planets And Satellites: Individual Jupiter, Solar System: Formation

Scientific paper

We report the detection of a single line of H218O in Jupiter at 1980.76 cm-1, the first detection of 18O in Jupiter. Models of the spectrum of Jupiter near this line imply that the Jovian isotopic abundance ratio 18O/16O is 1--3 times the terrestrial value. It is not possible to distinguish between the terrestrial ratio and highly anomalous oxygen isotope ratios of 2 or 3 times terrestrial because of the difficulties in modeling the spectrum and our reliance on a single H218O feature. Anomalous 18O in Jupiter could be caused by an intrinsic oxygen-isotope heterogeneity between solid and gaseous reservoirs in the preplanetary nebula, although given the constancy of 16O/18O in other solar system objects, such an explanation seems unlikely. Neither the isotopic anomalies in individual meteorite grains nor the differences in isotopic ratios between those in the solar system and in the interstellar medium would explain a gross enhancement of 18O in the outer solar system. The Galileo Probe Mass Spectrometer experiment may not allow a more accurate abundance determination of H218O because of the much larger amount of interfering 20Ne that may be present. It appears that no lines of H217O are detectable in the 5 mu m window.

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