Criteria for gravitational instability and quasi-isolated gravitational
  collapse in turbulent medium
  We study the evolution of structures in turbulent, self-gravitating media,
and present an analytical criterion $M_{\rm crit} \approx \epsilon_{\rm
cascade}^{2/3} \eta^{-2/3} G^{-1} l^{5/3}$ (where $M_{\rm crit}$ is the
critical mass, $l$ is the scale, $\epsilon_{\rm cascade}\approx \eta
\sigma_{\rm v}^3 /l $ is the turbulence energy dissipation rate of the ambient
medium, $G$ is the gravitational constant, $\sigma_{\rm v}$ is the velocity
dispersion, $l$ is the scale and $\eta\approx 0.2$ is an efficiency parameter)
for an object to undergo quasi-isolated gravitational collapse. The criterion
also defines the critical scale ($l_{\rm crit} \approx \epsilon_{\rm
cascade}^{1/2} \eta^{-1/2} G^{-3/4} \rho^{-3/4}$) for turbulent gravitational
instability to develop. The analytical formalism explains the size dependence
of the masses of the progenitors of star clusters ($M_{\rm cluster} \sim R_{\rm
cluster}^{1.67}$) in our Galaxy.
