The cosmochemistry of planetary systems

TL;DR

This review explores how the chemical and isotopic compositions of Solar System materials inform planetary formation processes, emphasizing pebble accretion's role in shaping planetary habitability and atmospheric composition.

Contribution

It highlights that planetesimal formation via streaming instability and pebble accretion explains most Solar System chemical observables, impacting habitability considerations.

Findings

Pebble accretion reproduces Solar System chemical signatures.

Volatiles are accreted early during planetary growth.

Chemical inventories influence atmospheric composition and habitability.

Abstract

Planets form and obtain their compositions from the leftover material present in protoplanetary disks of dust and gas surrounding young stars. The chemical make-up of a disk influences every aspect of planetary composition including their overall chemical properties, volatile content, atmospheric composition, and potential for habitability. This Review discusses our knowledge of the chemical and isotopic composition of Solar System materials and how this information can be used to place constraints on the formation pathways of terrestrial planets. We conclude that planetesimal formation by the streaming instability followed by rapid accretion of drifting pebbles within the protoplanetary disk lifetime reproduces most of the chemical and isotopic observables in Solar System. This finding has important implications for planetary habitability beyond the Solar System because in pebble accretion, volatiles important for life are accreted during the main growth phase of rocky planets as opposed to the late-stage. Finally, we explore how bulk chemical inventories and masses of planetary bodies control the composition of their primordial atmospheres and their potential to develop habitable conditions.