Saturn's internal structure and carbon enrichment

被引：0
|
作者：
Mousis, O. [1 ]
Alibert, Y. [2 ]
Benz, W. [2 ]
机构：
[1] Observatoire de Besançon, CNRS - UMR 6091, BP 1615, 25010 Besançon Cedex, France
[2] Physikalisches Institut, University of Bern, Sidlerstrasse 5, 3012 Bern, Switzerland
来源：
Astronomy and Astrophysics | 1600年 / 449卷 / 01期
关键词：
We use the clathrate hydrate trapping theory to calculate the enrichments in O; N; S; Xe; Ar and Kr compared to solar in Saturn's atmosphere. For this; we calibrate our calculations using two different carbon abundance determinations that cover the domain of measurements published in recent decades: one derived from the NASA Kuiper Airborne Observatory measurements and the other obtained from the Cassini spacecraft observations. We show that these two carbon abundances imply a different minimum heavy element content for Saturn. Using the Kuiper Airborne Observatory measurement for calibration; the amount of ices accreted by Saturn is found to be consistent with current interior models of this planet. On the other hand; using the Cassini measurement for calibration leads to an ice content in the planet's envelope that is higher than the one derived from the interior models. In this case; reconciling the interior models with the amount of C measured by the Cassini spacecraft requires that significant differential sedimentation of water and volatile species has taken place in Saturn's interior during its lifetime. © ESO 2006;
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页码：411 / 415
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