Making the Planetary Material Diversity During the Early Assembling of the Solar System

TL;DR

This paper presents a numerical model of the early Solar System's formation, showing how cloud collapse and disk processes created diverse planetary materials and explaining the presence of refractory inclusions and their rapid formation.

Contribution

It introduces a novel 1D simulation of Solar Nebula assembly that accounts for physical and chemical processes affecting material diversity during early planetary formation.

Findings

Refractory inclusions formed during the initial disk assembly.

Local mixing of solids with different thermal histories occurs.

Refractory materials are overabundant far from the Sun and form rapidly.

Abstract

Chondritic meteorites, the building blocks of terrestrial planets, are made of an out-of-equilibrium assemblage of solids formed at high and low temperatures, either in our Solar system or previous generations of stars. This was considered for decades to result from large scale transport processes in the Sun's isolated accretion disk. However, mounting evidences suggest that refractory inclusions in chondrites formed contemporaneously with the disk building. Here we numerically investigate, using a 1D model and several physical and chemical processes, the formation and transport of rocky materials during the collapse of the Sun's parent cloud and the consequent Solar Nebula assembling. The interplay between the cloud collapse, the dynamics of gas and dust, vaporization, recondensation and thermal processing of different species in the disk, results in a local mixing of solids with different thermal histories. Moreover, our results also explains the overabundance of refractory materials far from the Sun and their short formation timescales, during the first tens of kyr of the Sun, corresponding to class 0-I, opening new windows into the origin of the compositional diversity of chondrites.