Water condensed as ice beyond the water snowline, the location in the Sun’s natal gaseous disk where temperatures were below 170 K. As the disk evolved and cooled, the snowline moved inwards.
A low temperature in the terrestrial planet-forming region is unlikely to be the origin of water on the planets, and the distinct isotopic compositions of planetary objects formed in the inner and outer disks suggest limited early mixing of inner and outer Solar System materials.
Water in our terrestrial planets has rather been derived from H-bearing materials indigenous to the inner disk and delivered by water-rich planetesimals formed beyond the snowline and scattered inwards during the growth, migration, and dynamical evolution of the giant planets.
Andre Izidoro, Laurette Piani (CRPG)
Subjects: Earth and Planetary Astrophysics (astro-ph.EP); Geophysics (physics.geo-ph) Cite as: arXiv:2302.02674 [astro-ph.EP] (or arXiv:2302.02674v1 [astro-ph.EP] for this version) Journal reference: Elements, 2022, 18 (3), pp.181-186 Related DOI: https://doi.org/10.2138/gselements.18.3.181 Focus to learn more Submission history From: Laurette Piani [v1] Mon, 6 Feb 2023 10:24:30 UTC (1,881 KB) https://arxiv.org/abs/2302.02674 Astrobiology