| Full text | |
| Author(s): |
O'Brien, David P.
[1]
;
Izidoro, Andre
[2, 3]
;
Jacobson, Seth A.
[4, 5, 6]
;
Raymond, Sean N.
[3]
;
Rubie, David C.
[5]
Total Authors: 5
|
| Affiliation: | [1] Planetary Sci Inst, 1700 E Ft Lowell, Suite 106, Tucson, AZ 85719 - USA
[2] Univ Estadual Paulista, UNESP, Grp Dinam Orbital Planetol, BR-12516410 Sao Paulo - Brazil
[3] Univ Bordeaux, CNRS, Lab Astrophys Bordeaux, B18N, Allee Geoffroy St Hilaire, F-33615 Pessac - France
[4] Northwestern Univ, Dept Earth & Planetary Sci, Evanston, IL 60208 - USA
[5] Univ Bayreuth, Bayer Geoinst, D-95490 Bayreuth - Germany
[6] Observ Cote Azur, Bd Observ, CS 34229, F-06304 Nice 4 - France
Total Affiliations: 6
|
| Document type: | Review article |
| Source: | SPACE SCIENCE REVIEWS; v. 214, n. 1 FEB 2018. |
| Web of Science Citations: | 20 |
| Abstract | |
The planetary building blocks that formed in the terrestrial planet region were likely very dry, yet water is comparatively abundant on Earth. Here we review the various mechanisms proposed for the origin of water on the terrestrial planets. Various in-situ mechanisms have been suggested, which allow for the incorporation of water into the local planetesimals in the terrestrial planet region or into the planets themselves from local sources, although all of those mechanisms have difficulties. Comets have also been proposed as a source, although there may be problems fitting isotopic constraints, and the delivery efficiency is very low, such that it may be difficult to deliver even a single Earth ocean of water this way. The most promising route for water delivery is the accretion of material from beyond the snow line, similar to carbonaceous chondrites, that is scattered into the terrestrial planet region as the planets are growing. Two main scenarios are discussed in detail. First is the classical scenario in which the giant planets begin roughly in their final locations and the disk of planetesimals and embryos in the terrestrial planet region extends all the way into the outer asteroid belt region. Second is the Grand Tack scenario, where early inward and outward migration of the giant planets implants material from beyond the snow line into the asteroid belt and terrestrial planet region, where it can be accreted by the growing planets. Sufficient water is delivered to the terrestrial planets in both scenarios. While the Grand Tack scenario provides a better fit to most constraints, namely the small mass of Mars, planets may form too fast in the nominal case discussed here. This discrepancy may be reduced as a wider range of initial conditions is explored. Finally, we discuss several more recent models that may have important implications for water delivery to the terrestrial planets. (AU) | |
| FAPESP's process: | 16/19556-7 - Planetary Formation and Dynamics: from the Solar System to Exoplanets |
| Grantee: | André Izidoro Ferreira da Costa |
| Support Opportunities: | Scholarships in Brazil - Young Researchers |
| FAPESP's process: | 16/12686-2 - Planetary formation and dynamics: from the Solar System to exoplanets |
| Grantee: | André Izidoro Ferreira da Costa |
| Support Opportunities: | Research Grants - Young Investigators Grants |