Saturn's internal structure and carbon enrichment

Abstract

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 the last decades: one derived from the NASA $Kuiper$ Airborne Observatory measurements and the other obtained from the Cassini spacecraft observations. We show that these two different carbon abundances imply quite 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 which is higher than the one derived from the interior models. In this latter 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 have taken place in Saturn's interior during its lifetime.

accepted in A&A

References in corpus (7)

• Models of Giant Planet formation with migration and disc evolution
• Shock Compression of Deuterium and the Interiors of Jupiter and Saturn
• Migration and giant planet formation
• New Jupiter and Saturn formation models meet observations
• Effects of Helium Phase Separation on the Evolution of Extrasolar Giant Planets
• Chemical Constraints on the Water and Total Oxygen Abundances in the Deep Atmosphere of Saturn
• On the volatile enrichments and composition of Jupiter

Cited by in corpus (10)

• Determination of the minimum masses of heavy elements in the envelopes of Jupiter and Saturn
• Scientific rationale for Uranus and Neptune in situ explorations
• Volatile inventories in clathrate hydrates formed in the primordial nebula
• Scientific rationale of Saturn's in situ exploration
• The Origin of Nitrogen on Jupiter and Saturn from the ${}^{15}$N/${}^{14}$N Ratio
• Composition of Ices in Low-Mass Extrasolar Planets
• The deep composition of Uranus and Neptune from in situ exploration and thermochemical modeling
• On the volatile enrichments and heavy element content in HD 189733b
• Sequestration of noble gases by H3+ in protoplanetary disks and outer solar system composition
• On the possible noble gas deficiency of Pluto's atmosphere