Formation Location of Uranus and Neptune from D/H in satellites and comets

Details Formation Location of Uranus and Neptune from D/H in satellites and comets Formation Location of Uranus and Neptune from D/H in satellites and comets

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011epsc.conf.1442p&link_type=abstract

EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France. http://meetings.copernicus.org/epsc-dps2011, p.1442

Computer Science

Scientific paper

A comet's origins in the primitive nebula can be probed by examining the degree to which fossil deuterium is enriched compared to the protosolar abundance. Calculations of the temporal and radial evolution of the deuterium enrichment in the solar nebula can reproduce existing D/H measures for comets [1, 2, 3]. These calculations show that the deuterium enrichment in water ice strongly depends on the distance from the Sun at which the ice was formed. Comparing the D/H value measured in comets with those predicted by such models allows retrieval of their formation location. The measurement of the D/H ratio at Enceladus by the Ion and Neutral Mass Spectrometer aboard the Cassini spacecraft [5] provides a new, and tighter, constraint on the deuterium enrichment profile in the outer solar nebula prompting us to reconsider models presented in previous works [4].

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