Similarities between this numerical simulation of turbulent flow at a small scale within molecular clouds can be made with the much larger scale narrowband images, such as that of Sh2-135. The concentrations/densities of dust and hydrogen gas in the simulation reach ten orders of magnitude variation, with only partial physics included: viscous and magnetic driven turbulence together with sonic shock waves from dust particles moving through hydrogen.
The pattern of eddies mimics those in large scale images, and tends to follow a scale self-similar (fractal) geometry.
Only at the highest concentrations can hydrogen condense on the dust to begin star formation.
Taken from
Philip F. Hopkins, Hyunseok Lee, The fundamentally different dynamics of dust and gas in molecular clouds, Monthly Notices of the Royal Astronomical Society, Volume 456, Issue 4, 11 March 2016, Pages 4174–4190, https://doi.org/10.1093/mnras/stv2745