Planetesimal Compositions in Exoplanet Systems

TL;DR

This study models the composition of planetesimals beyond the snow line in exoplanet systems, highlighting how stellar C/O ratios influence icy and refractory material proportions, impacting planetary formation and atmospheres.

Contribution

It provides a self-consistent model linking stellar composition to planetesimal makeup, emphasizing the role of C/O ratios in determining icy versus refractory dominance.

Findings

Sub-solar C/O systems produce water ice-rich planetesimals.

Super-solar C/O systems yield planetesimals with high refractory content.

C/O ratio significantly affects volatile and ice composition in planetesimals.

Abstract

We have used recent surveys of the composition of exoplanet host stars to investigate the expected composition of condensed material in planetesimals formed beyond the snow line in the circumstellar nebulae of these systems. Of the major solid forming elements, we find that, as for the Sun, the C and O abundances (and particularly the C/O abundance ratio) have the most significant effect on the composition of icy planetesimals formed in these systems. The calculations use a self-consistent model for the condensation sequence of volatile ices from the nebula gas after refractory (silicate and metal) phases have condensed. The resultant proportions of refractory phases and ices were calculated for a range of nebular temperature structure and redox conditions. Planetesimals in systems with sub-solar C/O should be water ice-rich, with lower than solar mass fractions of refractory materials, while in super-solar C/O systems planetesimals should have significantly higher fractions of refractories, in some cases having little or no water ice. C-bearing volatile ices and clathrates also become increasingly important with increasing C/O depending on the assumed nebular temperatures. These compositional variations in early condensates in the outer portions of the nebula will be significant for the equivalent of the Kuiper Belt in these systems, icy satellites of giant planets and the enrichment (over stellar values) of volatiles and heavy elements in giant planet atmospheres.