# Dust Condensation in Evolving Discs and the Composition of Planetary Building Blocks

## TL;DR

This paper develops a physical-chemical model of dust condensation in evolving protoplanetary discs to predict the chemical makeup of planetary building blocks, comparing two condensation models and analyzing their implications for Solar System bodies.

## Contribution

It introduces a comprehensive model combining disc evolution and dust condensation, comparing temperature-based and equilibrium-based condensation methods, to better understand planetary composition formation.

## Key findings

- Models predict compositions similar to certain chondrites under specific decoupling timescales.
- Condensation models show systematic differences of about 10% depending on conditions.
- Short decoupling timescales lead to compositions deviating from observed values.

## Abstract

Partial condensation of dust from the Solar nebula is likely responsible for the diverse chemical compositions of chondrites and rocky planets/planetesimals in the inner Solar system. We present a forward physical-chemical model of a protoplanetary disc to predict the chemical compositions of planetary building blocks that may form from such a disc. Our model includes the physical evolution of the disc and the condensation, partial advection, and decoupling of the dust within it. The chemical composition of the condensate changes with time and radius. We compare the results of two dust condensation models: one where an element condenses when the midplane temperature in the disc is lower than the 50\% condensation temperature ($\rm T_{50}$) of that element and the other where the condensation of the dust is calculated by a Gibbs free energy minimization technique assuming chemical equilibrium at local disc temperature and pressure. The results of two models are generally consistent with some systematic differences of $\sim 10$\% depending upon the radial distance and an element's condensation temperature. Both models predict compositions similar to 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 too short, the composition deviates significantly from the measured values. These models may contribute to our understanding of the chemical compositions of chondrites, and ultimately the terrestrial planets in the solar system, and may constrain the potential chemical compositions of rocky exoplanets.