Chondrule formation by collisions of planetesimals containing volatiles triggered by Jupiter's formation

TL;DR

This paper proposes a novel model where collisions of volatile-rich planetesimals, triggered by Jupiter's formation, produce chondrules with observed sizes and cooling rates, linking planetary formation to meteorite characteristics.

Contribution

It introduces a new collision-based formation mechanism for chondrules that accounts for their size and cooling rate, connecting Jupiter's formation to meteoritic features.

Findings

Collisions induce silicate melt production consistent with chondrule properties

Expanding gas from volatiles disperses and cools melt droplets

Peak melt production aligns with Jupiter's runaway gas accretion

Abstract

Chondrules are spherical or subspherical particles of crystallized or partially crystallized liquid silicates that constitute large-volume fractions of most chondritic meteorites. Chondrules typically range $0.1-2\,$mm in size and solidified with cooling rates of $10-1000\,{\rm K\,h^{-1}}$, yet these characteristics prove difficult to reconcile with proposed formation models. We numerically show that collisions among planetesimals containing volatile material naturally explain both the sizes and cooling rates of chondrules. We show that the high-velocity collisions with volatile-rich planetesimals first induced in the solar nebula by Jupiter's formation produced increasing amounts of silicate melt for increasing impact velocities above $2\,{\rm km\,s^{-1}}$. We propose that the expanding gas formed from volatile materials by collisional heating dispersed and cooled the silicate melt, resulting in droplet sizes and cooling rates consistent with the observed sizes and inferred cooling rates. We further show that the peak melt production is linked to the onset of Jupiter's runaway gas accretion, and argue that the peak age of chondrules points to Jupiter's birth dating 1.8 Myr after CAIs.