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Annual Review of Astronomy and Astrophysics

Volume 62, 2024

The Star–Planet Composition Connection

Abstract

The mantra “know thy star, know thy planet” has proven to be very important for many aspects of exoplanet science. Here I review how stellar abundances inform our understanding of planet composition and, thus, formation and evolution. In particular, I discuss how:

  • ▪  The strongest star–planet connection is still the giant planet–metallicity correlation, the strength of which may indicate a break point between the formation of planets versus brown dwarfs.
  • ▪  We do not have very good constraints on the lower metallicity limit for planet formation, although new statistics from TESS are helping, and it appears that, at low [Fe/H], α elements can substitute for iron as seeds for planet formation.
  • ▪  The depletion of refractory versus volatile elements in stellar photospheres (particularly the Sun) was initially suggested as a sign of small planet formation but is challenging to interpret, and small differences in binary star compositions can be attributed mostly to processes other than planet formation.
  • ▪  We can and should go beyond comparisons of the carbon-to-oxygen ratio in giant planets and their host stars, incorporating other volatile and refractory species to better constrain planet formation pathways.
  • ▪  There appears to be a positive correlation between small planet bulk density and host star metallicity, but exactly how closely small planet refractory compositions match those of their host stars—and their true diversity—is still uncertain.

Keyword(s): exoplanet compositions, exoplanets, host stars, planet formation, stellar abundances
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2024-09-13
2025-04-22
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The Star–Planet Composition Connection
Annual Review of Astronomy and Astrophysics 62, 333 (2024); https://doi.org/10.1146/annurev-astro-071221-053007
/content/journals/10.1146/annurev-astro-071221-053007
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