The late formation of chondrites as a consequence of Jupiter-induced gaps and rings

TL;DR

This paper proposes that Jupiter's early formation created disk structures that caused a second wave of planetesimal formation, explaining the delayed formation of chondrites in the early Solar System.

Contribution

It demonstrates through simulations that Jupiter-induced disk gaps and rings led to a second-generation planetesimal population, accounting for the age difference in chondrites.

Findings

Jupiter's formation caused pressure bumps and dust traps in the protoplanetary disk.

A second planetesimal population formed 2-3 Myr after Solar System start.

Jupiter's influence prevented inward migration of terrestrial embryos.

Abstract

The accretion ages of the first planetesimals-the parent bodies of magmatic iron meteorites-suggest they formed within the first 0.5-1 Myr of Solar System history. Yet, planetesimal formation appears to have occurred in at least two distinct phases. A temporal offset separates early-forming bodies from later-forming chondrite parent bodies, which accreted 2-3 Myr after the Solar System onset - an unresolved aspect of Solar System formation. Here we use numerical simulations to show that Jupiter's early formation reshaped its natal protoplanetary disk. Jupiter's rapid growth depleted the inner disk gas and generated pressure bumps and dust traps that manifested as rings. These structures caused dust to accumulate and led to a second-generation planetesimal population, with ages matching those of non-carbonaceous chondrites. Meanwhile, the evolving gas structure suppressed terrestrial embryos' inward migration, preventing them from reaching the innermost regions. Jupiter likely played a key role in shaping the inner Solar System, consistent with structures observed in Class II and transition disks.