The theory of globulettes: candidate precursors of brown dwarfs and free floating planets in H II regions

TL;DR

This paper reviews globulettes in H II regions, models their structure as pressure confined Bonnor-Ebert spheres, and discusses their stability, evolution, and potential as precursors to free-floating planets and brown dwarfs.

Contribution

It provides a theoretical framework for globulette structure and evolution, demonstrating their stability and potential to form brown dwarfs or planets during collisions or perturbations.

Findings

Globulettes are well described by pressure confined Bonnor-Ebert spheres.

Mass approximately proportional to radius squared due to column density threshold.

Globulettes are stable against collapse within H II regions.

Abstract

Large numbers of small opaque dust clouds - termed 'globulettes' by Gahm et al - have been observed in the H II regions surrounding young stellar clusters. With masses typically in the planetary (or low mass brown dwarf) regime, these objects are so numerous in some regions (e.g. the Rosette) that, if only a small fraction of them could ultimately collapse, then they would be a very significant source of free floating planets. Here we review the properties of globulettes and present a theoretical framework for their structure and evolution. We demonstrate that their interior structure is well described by a pressure confined isothermal Bonnor-Ebert sphere and that the observed mass-radius relation (mass approximately proportional to the radius squared) is a systematic consequence of a column density threshold below which components of the globulette are not identified. We also find that globulettes with this interior structure are very stable against collapse within H II regions. We follow Gahm et al in assuming that globulettes are detached from the tips of pillars protruding in from the swept up shell that borders the expanding H II region and produce a model for their dynamics, finding that globulettes will eventually impact the shell. We derive an expression for the time it takes to do so and show that dissipation of energy via dust cooling allows all globulettes to survive this encounter and escape into the wider ISM. Once there the ambient pressure drops and they disperse on timescales around 30-300 kyr and should be observable using ALMA out to distances of order a parsec. Since we find that globulettes are stable, the only route via which they might still form brown dwarfs or planets is during their collision with the shell or some other violent perturbative event.