Molecular Clouds as Gravitational Instabilities in Rotating Disks: A Modified Stability Criterion

TL;DR

This paper introduces a 3D stability criterion for molecular gas disks, revealing that vertical perturbations enable gravitational fragmentation even when traditional 2D Toomre stability suggests the disks are stable.

Contribution

It develops a modified stability criterion incorporating vertical structure, showing that molecular disks can fragment via 3D instabilities despite being Toomre stable.

Findings

3D perturbations lower the stability threshold for molecular disks.

Fragmentation can occur on scales larger than the Jeans length.

Growth rates of 3D instabilities are comparable to or faster than Toomre instabilities.

Abstract

Molecular gas disks are generally Toomre stable ($Q_T>$1) and yet clearly gravitationally unstable to structure formation as evidenced by the existence of molecular clouds and ongoing star formation. This paper adopts a 3D perspective to obtain a general picture of instabilities in flattened rotating disks, using the 3D dispersion relation to describe how disks evolve when perturbed over their vertical extents. By explicitly adding a vertical perturbation to an unperturbed equilibrium disk, stability is shown to vary with height above the mid-plane. Near to $z$=0 where the equilibrium density is roughly constant, instability takes on a Jeans-like quality, occurring on scales larger than the Jeans length and subject to a threshold $Q_M=\kappa^2/(4\pi G\rho)=1$ or roughly $Q_T\approx 2$. Far from the mid-plane, on the other hand, stability is pervasive, and the threshold for the total disk (out to $z=\pm\infty$) to be stabilized is lowered to $Q_T=1$ as a consequence. In this new framework, gas disks are able to fragment through partial 3D instability even where total 2D instability is suppressed. The growth rates of the fragments formed via 3D instability are comparable to, or faster than, Toomre instabilities. The rich structure in molecular disks on the scale of 10s of pc can thus be viewed as a natural consequence of their 3D nature and their exposure to a variety of vertical perturbations acting on roughly a disk scale height, i.e. due to their situation within the more extended galaxy potential, participation in the disk-halo flow, and exposure to star formation feedback.