Theoretical predictions of deuterium abundances in the Jovian planets

Details Theoretical predictions of deuterium abundances in the Jovian planets Theoretical predictions of deuterium abundances in the Jovian planets

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980icar...44..676h&link_type=abstract

Icarus, vol. 44, Dec. 1980, p. 676-682.

Astronomy and Astrophysics

Astronomy

57

Abundance, Astronomical Models, Deuterium, Gas Giant Planets, Planetary Evolution, Ammonia, Hydrogen, Methane, Water

Scientific paper

Current concepts for the origin of the Jovian planets and current constraints on their interior structure are used to support the argument that the presence of large amounts of 'ice' (H2O, CH4, and NH3) in Uranus and Neptune indicates temperature low enough to condense these species at the time Uranus and Neptune formed. Such low temperatures, however, imply orders-of-magnitude fractionation effects for deuterium into the 'ice' component if isotopic equilibration can occur. The present models thus imply that Uranus and Neptune should have D/H ratio at least four times primordial, contrary to observation for Uranus. It is found that the Jovian and Saturnian D/H should be close to primordial regardless of formation scenario.

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