From Dust to Planets -- A Chemical Perspective
Klaus Mezger, Jonas Pape, Aryavart Anand, Pascal M. Kruttasch, Hauke Vollstaedt, Jan Hoffmann

TL;DR
This paper reviews the chemical and chronological evidence from meteorites to reconstruct the early solar system's evolution, planetesimal formation, and Earth's development into a habitable planet.
Contribution
It provides a comprehensive overview of the processes and events that shaped the chemical composition and differentiation of planetary bodies in the early Solar System.
Findings
Planetesimal formation began within 1 million years of Solar System formation.
Streaming instabilities and bow shocks played key roles in planetesimal formation.
Earth's habitability was influenced by a late collision with a volatile-rich body.
Abstract
Chemical and chronological information preserved in meteorites permits the reconstruction of events and processes in the solar nebula from the formation of the first solids to the accretion of planetary bodies and their subsequent differentiation. The path from a gas-dust cloud to differentiated planets includes intervals of steady evolution interrupted by singular events that dramatically altered this steady path, leading to planetary bodies with distinct chemical compositions and different degrees of internal differentiation. The dominant continuous process in the early Solar System was the cooling of the gas-dust cloud, which caused a steady condensation of elements into solid compounds and a continuous increase in the dust/gas ratio. Planetesimal formation started within less than 1 Ma of Solar System formation and continued for ca. 3 Ma apparently in random regions within the disk.…
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