Dust Condensation in Evolving Discs and the Composition of Meteorites, Planetesimals, and Planets

Abstract

Partial condensation of dust from the Solar nebula is thought to be responsible for the diverse chemical compositions of the rocky planets/planetesimals in the inner Solar system. Here we present a forward physical-chemical model of a protoplanetary disc to predict the chemical compositions of planetesimals that may form from such a disc. Our model includes the physical evolution of the disc and the condensation and partial advection and decoupling of the dust within it. The condensation of the dust is calculated by a Gibbs free energy minimization technique assuming chemical equilibrium. We show that the chemical composition of the condensate changes with time and radius. A simple model based on the 50% condensation temperatures (T_{50}) predicts compositions of resulting planetesimals that are broadly consistent with those of CM, CO, and CV chondrites provided that the decoupling timescale of the dust is on the order of the evolution timescale of the disc or longer. If the decoupling timescale is an order of magnitude shorter than the evolution timescale of the disc then the calculated chemical compositions of planetesimals significantly deviate from the measured values. The relative elemental abundances in the condensed dust are highly affected by the thermal history of the disc. Our model can explain the chemical compositions of some of the terrestrial planets in the solar system and may constrain the potential chemical compositions of rocky exoplanets.