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Hf-W chronology of the accretion and early evolution of asteroids and terrestrial planets
The 182 Hf– 182 W systematics of meteoritic and planetary samples provide firm constraints on the chronology of the accretion and earliest evolution of asteroids and terrestrial planets and lead to
The Crust of the Moon as Seen by GRAIL
TLDR
The Moon's gravity field shows that the lunar crust is less dense and more porous than was thought, and high-resolution gravity data obtained from the dual Gravity Recovery and Interior Laboratory (GRAIL) spacecraft show that the bulk density of the Moon's highlands crust is substantially lower than generally assumed.
EARLY CRUSTAL EVOLUTION OF MARS 1
▪ Abstract The bulk of the ∼50-km-thick Martian crust formed at ∼4.5 Gyr B.P., perhaps from a magma ocean. This crust is probably a basaltic andesite or andesite and is enriched in incompatible and
Energetics of the Core
This chapter reviews theoretical approaches to calculating the energy and entropy budgets of the Earth's core. The energy budget allows the growth of the inner core with time to be calculated; the
Transient Water Vapor at Europa’s South Pole
TLDR
Europa's Plumes Jupiter's moon Europa has a subsurface ocean and a relatively young icy surface, and spectral images taken by the Hubble Space Telescope show ultraviolet emissions from the moon's atmosphere that are consistent with two 200-km-high plumes of water vapor.
A Hadean to Paleoarchean geodynamo recorded by single zircon crystals
TLDR
Full-vector paleointensity measurements of Archean to Hadean zircons bearing magnetic inclusions from the Jack Hills conglomerate are reported to reconstruct the early geodynamo history and imply that early atmospheric evolution on both Earth and Mars was regulated by dynamo behavior.
Heterogeneous accretion, composition and core–mantle differentiation of the Earth
A model of core formation is presented that involves the Earth accreting heterogeneously through a series of impacts with smaller differentiated bodies. Each collision results in the impactor's
The Pluto system: Initial results from its exploration by New Horizons
TLDR
The New Horizons encounter revealed that Pluto displays a surprisingly wide variety of geological landforms, including those resulting from glaciological and surface-atmosphere interactions as well as impact, tectonic, possible cryovolcanic, and mass-wasting processes.
Estimates of Martian crustal thickness from viscous relaxation of topography
Isostatically compensated crustal thickness variations and associated topographic contrasts at the surface of a planet result in lateral pressure gradients, which may cause the lower crust to flow
Shear heating as the origin of the plumes and heat flux on Enceladus
TLDR
It is shown that the most likely explanation for the heat and vapour production is shear heating by tidally driven lateral (strike-slip) fault motion with displacement of ∼0.5 m over a tidal period, suggesting that the ice shell is decoupled from the silicate interior by a subsurface ocean.
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