The Compositional Dimension of Planet Formation
arXiv:2302.08317 · doi:10.1142/9781800613140_0001
Abstract
The great diversity of the thousands of planets known to date is proof of the multitude of ways in which formation and evolution processes can shape the life of planetary systems. Multiple formation and evolution paths, however, can result in the same planetary architecture. Because of this, unveiling the individual histories of planetary systems and their planets can prove a challenging task. The chemical composition of planets provides us with a guiding light for navigate this challenge, but to understand the information it carries we need to properly link it to the chemical composition and characteristics of the environments in which the planets formed. To achieve this goal it is necessary to combine the information and perspectives provided by a growing number of different fields of study, spanning the whole lifecycle of stars and their planetary systems. The aim of this chapter is to provide the unifying perspective needed to understand and connect such diverse information, and illustrate the process through which we can decode the message contained into the composition of planetary bodies.
45 pages, 7 figures, 4 tables; accepted as a chapter in the book "Planetary systems now", eds. Luisa M. Lara and David Jewitt, World Scientific Publishing Co Pte Ltd
References in corpus (18)
- The imprint of exoplanet formation history on observable present-day spectra of hot Jupiters
- The elemental composition of the Sun II. The iron group elements Sc to Ni
- The elemental composition of the Sun I. The intermediate mass elements Na to Ca
- Mass-Metallicity Trends in Transiting Exoplanets from Atmospheric Abundances of HO, Na, and K
- Setting the volatile composition of (exo)planet-building material. Does chemical evolution in disk midplanes matter?
- How drifting and evaporating pebbles shape giant planets I: Heavy element content and atmospheric C/O
- Planet-forming material in a protoplanetary disc: the interplay between chemical evolution and pebble drift
- Oxygen fugacities of extrasolar rocks: Evidence for an Earth-like geochemistry of exoplanets
- Thermal desorption of circumstellar and cometary ice analogs
- How drifting and evaporating pebbles shape giant planets II: Volatiles and refractories in atmospheres
- Connecting planet formation and astrochemistry: A main sequence for C/O in hot-exoplanetary atmospheres
- High gas/dust size ratio indicating efficient radial drift in the mm-faint CX Tau disk
- The origin of the high metallicity of close-in giant exoplanets: Combined effect of the resonant and aerodynamic shepherding
- On the secular evolution of the ratio between gas and dust radii in protoplanetary discs
- Formation of Venus, Earth and Mars: Constrained by isotopes
- Exploring the link between star and planet formation with Ariel
- Ariel: Enabling planetary science across light-years
- Effects of disc midplane evolution on CO snowline location