Abstract
We present models of giant planet formation, taking into account migration and disk viscous evolution. We show that migration can significantly reduce the formation timescale bringing it in good agreement with typical observed disk lifetimes. We then present a model that produces a planet whose current location, core mass and total mass are comparable with the one of Jupiter. For this model, we calculate the enrichments in volatiles and compare them with the one measured by the Galileo probe. We show that our models can reproduce both the measured atmosphere enrichments and the constraints derived by Guillot et al. (2004), if we assume the accretion of planetesimals with ices/rocks ratio equal to 4, and that a substantial amount of CO2 was present in vapor phase in the solar nebula, in agreement with ISM measurements.
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Alibert, Y., Mordasini, C., Mousis, O., Benz, W. (2005). Formation of Giant Planets — An Attempt in Matching Observational Constraints. In: Encrenaz, T., Kallenbach, R., Owen, T.C., Sotin, C. (eds) The Outer Planets and their Moons. Space Sciences Series of ISSI, vol 19. Springer, Dordrecht. https://doi.org/10.1007/1-4020-4038-5_6
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DOI: https://doi.org/10.1007/1-4020-4038-5_6
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