Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion
By S. Raymond, A. Izidoro. 2017
238 citations recorded by the source corpus.
Abstract 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.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/99e00e83aac9487da5365f5f9a8883a21d61991d
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In Astronomy and Astrophysics
Citations in the corpus
- The Non-carbonaceous–Carbonaceous Meteorite Dichotomy (2020, background): “…is consistent with evidence for the addition of CC material to the eucrite and angrite parent bodies (both are NC bodies) at ∼ 4–5 Ma after CAI formation (Sarafian et al. 2017, 2014), which may be related to inward scattering of CC bodies by a nearly fully-formed Jupiter (Raymond and Izidoro 2017).”
- The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites (2017, methodology): “Our approach is similar to that taken by Raymond & Izidoro (2017) in their treatment of how Jupiter’s growth will scatter planetesimals; they parameterized Jupiter’s growth as linear on a timescale ∼ 105 yr.”
- The composition of Mars (2019, background): “These differences likely originated because of a limited radial transport in the accretion disk, which may have been controlled by an early-formed young Jupiter (Walsh et al., 2011; Kruijer et al., 2017a; Raymond and Izidoro, 2017; Desch et al., 2018).”