RAYMOND, Sean N.; IZIDORO, A.

doi:10.1016/j.icarus.2017.06.030

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RAYMOND, Sean N.
ECLIPSE 2017

IZIDORO, A.
Universidade Estadual Paulista Júlio de Mesquita Filho = São Paulo State University [UNESP]
ECLIPSE 2017

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Article de revue

Ce document a été publié dans

Icarus. 2017-07, vol. 297, p. 134-148

Elsevier

Résumé en anglais

There is a long-standing debate regarding the origin of the terrestrial planets' water as well as the hydrated C-type asteroids. Here we show that the inner Solar System's water is a simple byproduct of the giant planets' formation. Giant planet cores accrete gas slowly until the conditions are met for a rapid phase of runaway growth. As a gas giant's mass rapidly increases, the orbits of nearby planetesimals are destabilized and gravitationally scattered in all directions. Under the action of aerodynamic gas drag, a fraction of scattered planetesimals are deposited onto stable orbits interior to Jupiter's. This process is effective in populating the outer main belt with C-type asteroids that originated from a broad (5-20 AU-wide) region of the disk. As the disk starts to dissipate, scattered planetesimals reach sufficiently eccentric orbits to cross the terrestrial planet region and deliver water to the growing Earth. This mechanism does not depend strongly on the giant planets' orbital migration history and is generic: whenever a giant planet forms it invariably pollutes its inner planetary system with water-rich bodies.< Réduire

Mots clés en anglais

Astrophysics - Earth and Planetary Astrophysics

Astrophysics - Solar and Stellar Astrophysics

DOI

http://dx.doi.org/10.1016/j.icarus.2017.06.030

Project ANR

Modélisation du processus de croissance des planètes Joviennes/ - ANR-13-BS05-0003

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Importé de hal

Unités de recherche

Laboratoire d'Astrophysique de Bordeaux (LAB) - UMR 5804