Water and the interior structure of terrestrial planets and icy bodies
arXiv:1712.07539 · doi:10.1007/s11214-018-0473-x
Abstract
Water content and the internal evolution of terrestrial planets and icy bodies are closely linked. The distribution of water in planetary systems is controlled by the temperature structure in the protoplanetary disk and dynamics and migration of planetesimals and planetary embryos. This results in the formation of planetesimals and planetary embryos with a great variety of compositions, water contents and degrees of oxidation. The internal evolution and especially the formation time of planetesimals relative to the timescale of radiogenic heating by short-lived 26Al decay may govern the amount of hydrous silicates and leftover rock-ice mixtures available in the late stages of their evolution. In turn, water content may affect the early internal evolution of the planetesimals and in particular metal-silicate separation processes. Moreover, water content may contribute to an increase of oxygen fugacity and thus affect the concentrations of siderophile elements within the silicate reservoirs of Solar System objects. Finally, the water content strongly influences the differentiation rate of the icy moons, controls their internal evolution and governs the alteration processes occurring in their deep interiors.
45 pages, 13 figures, accepted in Space Sci. Rev
References in corpus (7)
- Origin of water in the inner Solar System: Planetesimals scattered inward during Jupiter and Saturn's rapid gas accretion
- Water Delivery and Giant Impacts in the 'Grand Tack' Scenario
- Highly Siderophile Elements in the Earth's Mantle as a Clock for the Moon-forming Impact
- Highly siderophile elements were stripped from Earth's mantle by iron sulfide segregation
- Main-Belt Comet P/2008 R1 (Garradd)
- Scaling of plate-tectonic convection with pseudoplastic rheology
- The persistence of oceans on Earth-like planets: insights from the deep-water cycle
Cited by in corpus (23)
- Bifurcation of planetary building blocks during Solar System formation
- A water budget dichotomy of rocky protoplanets from Al-heating
- Oxygen fugacities of extrasolar rocks: Evidence for an Earth-like geochemistry of exoplanets
- Habitability of Exoplanet Waterworlds
- Migration-driven diversity of super-Earth compositions
- Rocky super-Earths or waterworlds: the interplay of planet migration, pebble accretion and disc evolution
- Breaking Degeneracies in Formation Histories by Measuring Refractory Content in Gas Giants
- The Metal-Silicate Partitioning of Carbon During Earth's Accretion and its Distribution in the Early Solar System
- Magma ascent in planetesimals: control by grain size
- Plausible constraints on the range of bulk terrestrial exoplanet compositions in the Solar neighbourhood
- Dependence of Biological Activity on the Surface Water Fraction of Planets
- Anatomy of rocky planets formed by rapid pebble accretion I. How icy pebbles determine the core fraction and FeO contents
- System-level fractionation of carbon from disk and planetesimal processing
- Where are the Extrasolar Mercuries?
- Origin and dynamical evolution of the asteroid belt
- Distribution and kinematics of 26Al in the Galactic disc
- Proton dynamics in high-pressure ice-VII from density functional theory
- Crash Chronicles: relative contribution from comets and carbonaceous asteroids to Earth's volatile budget in the context of an Early Instability
- Planet formation: key mechanisms and global models
- Constraining the Origin of Mars via Simulations of Multi-Stage Core Formation
- DEWPython: A Python Implementation of the Deep Earth Water Model and Application to Ocean Worlds
- A compositional link between rocky exoplanets and their host stars
- Speed of sound of pure water to 700 MPa and an equation of state to 2300 MPa