Theoretical predictions of deuterium abundances in the Jovian planets
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.
- Research Organization:
- Arizona, University, Tucson, AZ
- OSTI ID:
- 5422887
- Journal Information:
- Icarus; (United States), Vol. 44
- Country of Publication:
- United States
- Language:
- English
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Related Subjects
GENERAL PHYSICS
DEUTERIUM
ABUNDANCE
JUPITER PLANET
ISOTOPE RATIO
NEPTUNE PLANET
SATURN PLANET
URANUS PLANET
AMMONIA
HYDROGEN
METHANE
PLANETARY EVOLUTION
WATER
ALKANES
ELEMENTS
HYDRIDES
HYDROCARBONS
HYDROGEN COMPOUNDS
HYDROGEN ISOTOPES
ISOTOPES
LIGHT NUCLEI
NITROGEN COMPOUNDS
NITROGEN HYDRIDES
NONMETALS
NUCLEI
ODD-ODD NUCLEI
ORGANIC COMPOUNDS
OXYGEN COMPOUNDS
PLANETS
SOLAR SYSTEM EVOLUTION
STABLE ISOTOPES
640107* - Astrophysics & Cosmology- Planetary Phenomena