Terrestrial Planet Formation in the Presence of Migrating Super-earths

A. Izidoro Alessandro Morbidelli 1 Sean N. Raymond 2
2 ECLIPSE 2014
L3AB - Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux, OASU - Observatoire aquitain des sciences de l'univers, LAB - Laboratoire d'Astrophysique de Bordeaux [Pessac], Université Sciences et Technologies - Bordeaux 1
Abstract : Super-Earths with orbital periods less than 100 days are extremely abundant around Sun-like stars. It is unlikely that these planets formed at their current locations. Rather, they likely formed at large distances from the star and subsequently migrated inward. Here we use N-body simulations to study the effect of super-Earths on the accretion of rocky planets. In our simulations, one or more super-Earths migrates inward through a disk of planetary embryos and planetesimals embedded in a gaseous disk. We tested a wide range of migration speeds and configurations. Fast-migrating super-Earths ($\tau_{mig} \sim$0.01-0.1 Myr) only have a modest effect on the protoplanetary embryos and planetesimals. Sufficient material survives to form rocky, Earth-like planets on orbits exterior to the super-Earths'. In contrast, slowly-migrating super-Earths shepherd rocky material interior to their orbits and strongly deplete the terrestrial planet-forming zone. In this situation any Earth-sized planets in the habitable zone are extremely volatile-rich and are therefore probably not Earth-like.
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Submitted on : Tuesday, September 9, 2014 - 11:39:12 AM
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A. Izidoro, Alessandro Morbidelli, Sean N. Raymond. Terrestrial Planet Formation in the Presence of Migrating Super-earths. Astrophysical Journal, American Astronomical Society, 2014, 749 (1), pp.id. 11. ⟨10.1088/0004-637X/794/1/11⟩. ⟨hal-01062140⟩



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