Jupiter and Saturn formation models

Details Jupiter and Saturn formation models Jupiter and Saturn formation models

Aug 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005dps....37.2902a&link_type=abstract

American Astronomical Society, DPS meeting #37, #29.02; Bulletin of the American Astronomical Society, Vol. 37, p.673

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We use our extended core accretion models of planet formation, including migration and disk evolution (see Alibert et al. 2004,2005) to calculate models of Jupiter and Saturn formation. We show that we can form these two planets in the same disk, and in a few Myr. The starting location of the two planets is respectively of 9 and 12 AU. At the end of the formation process, when the disk has disappeared, the two planets show properties (total mass, core mass, mass of heavy elements, distance to the sun) comparable to the one of the two planets. Moreover, the calculation of the disk evolution gives us the thermodynamical properties inside the disk. Using the clathrate hydrate trapping theory (Lunine and Stevenson 1987), we calculate the composition of planetesimals as a function of the distance to the sun. Knowing this composition, as well as the amount of planetesimals accreted as a function of the heliocentric distance, we can finally calculate the content of the two planets in some volatile elements (C, N, S, Ar, Kr, Xe). We obtain enrichments in the atmospheres of the two planets that are consistent with the one measured by the Galileo probe (for Jupiter) and from the earth (for Saturn).
This work was supported in part by the Swiss National Science Foundation.

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