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| Titel |
The origin of volatiles on Titan and Enceladus |
| VerfasserIn |
Tobias Owen, H. B. Niemann, W. Kasprzak, S. K. Atreya, D. Gautier, J. Lunine |
| Konferenz |
EGU General Assembly 2010
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| Medientyp |
Artikel
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| Sprache |
Englisch
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| Digitales Dokument |
PDF |
| Erschienen |
In: GRA - Volume 12 (2010) |
| Datensatznummer |
250036523
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| Zusammenfassung |
| The apparent absence of Kr and Xe from Titan’s atmosphere can be convincingly attributed to
their intrinsically low abundances, provided Titan sampled a reservoir with similar
abundances to one of those on the Sun, Earth, Mars, Venus or meteorites. The remarkably
high value of 14N/36Ar provides the basic proof that Titan’s nitrogen originated as NH3, not
N2. This conclusion is supported by studies of nitrogen isotopes in Jupiter’s atmosphere,
comets and meteorites.
The value of D/H in the water ice sampled from Enceladus so far is isotopically the same as
values measured in comet nuclei originating from 3 different distances. This is consistent
with the model of Owen and Robert (2010) requiring all ice in the outer solar system to have
the same isotopic ratio, with the possible exception of Titan and the four large satellites of
Jupiter. |
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