Cavitating bubbles in condensing gas as a means of forming clumps, chondrites, and planetesimals

TL;DR

This paper explores a hypothetical radiation-condensation instability in condensing gases that could lead to the formation of dense clumps, potentially explaining the assembly of planetesimals and chondrules in early solar system environments.

Contribution

It introduces a new theoretical model for how condensing vapor can fragment into overdense clumps through a radiation-driven instability, with initial calculations of bubble collapse dynamics.

Findings

Condensing silicate vapor bubbles can collapse rapidly, up to sonic speeds.

Adding non-condensible gases like hydrogen can prevent bubble collapse.

The mechanism may explain formation processes of chondrules and planetesimals.

Abstract

Vaporized metal, silicates, and ices on the verge of re-condensing into solid or liquid particles appear in many contexts: behind shocks, in impact ejecta, and within the atmospheres and outflows of stars, disks, planets, and minor bodies. We speculate that a condensing gas might fragment, forming overdensities within relative voids, from a radiation-condensation instability. Seeded with small thermal fluctuations, a condensible gas will exhibit spatial variations in the density of particle condensates. Regions of higher particle density may radiate more, cooling faster. Faster cooling leads to still more condensation, lowering the local pressure. Regions undergoing runaway condensation may collapse under the pressure of their less condensed surroundings. Particle condensates will compactify with collapsing regions, into overdense clumps or macroscopic solids (planetesimals). As a first step toward realizing this hypothetical instability, we calculate the evolution of a small volume of condensing silicate vapor -- a spherical test "bubble" embedded in a background medium whose pressure and radiation field are assumed fixed for simplicity. Such a bubble condenses and collapses upon radiating its latent heat to the background, assuming its energy loss is not stopped by background irradiation. Collapse speeds can range up to sonic, similar to cavitation in terrestrial settings. Adding a non-condensible gas like hydrogen to the bubble stalls the collapse. We discuss whether cavitation can provide a way for mm-sized chondrules and refractory solids to assemble into meteorite parent bodies, focusing on CB/CH chondrites whose constituents likely condensed from silicate/metal vapor released from the most energetic asteroid collisions.