Sub-structure formation in starless cores

TL;DR

This paper investigates how small density perturbations in starless cores evolve, showing they often dissipate before collapsing, but vortical modes may lead to fragmentation, impacting star formation understanding.

Contribution

It introduces an analytical and numerical framework for understanding the evolution and dissipation of density perturbations in contracting starless cores, highlighting the role of solenoidal modes.

Findings

Perturbations are amplified during contraction but often dissipate before gravitational collapse.

Solenoidal modes grow faster and may promote core fragmentation.

Most perturbations dissipate prior to reaching gravitational instability.

Abstract

Motivated by recent observational searches of sub-structure in starless molecular cloud cores, we investigate the evolution of density perturbations on scales smaller than the Jeans length embedded in contracting isothermal clouds, adopting the same formalism developed for the expanding Universe and the solar wind. We find that initially small amplitude, Jeans-stable perturbations (propagating as sound waves in the absence of a magnetic field), are amplified adiabatically during the contraction, approximately conserving the wave action density, until they either become nonlinear and steepen into shocks at a time $t_{\rm nl}$, or become gravitationally unstable when the Jeans length decreases below the scale of the perturbations at a time $t_{\rm gr}$. We evaluate analytically the time $t_{\rm nl}$ at which the perturbations enter the non-linear stage using a Burgers' equation approach, and we verify numerically that this time marks the beginning of the phase of rapid dissipation of the kinetic energy of the perturbations. We then show that for typical values of the rms Mach number in molecular cloud cores, $t_{\rm nl}$ is smaller than $t_{\rm gr}$, and therefore density perturbations likely dissipate before becoming gravitational unstable. Solenoidal modes grow at a faster rate than compressible modes, and may eventually promote fragmentation through the formation of vortical structures.