deletions | additions       diff --git a/The simulation.tex b/The simulation.tex  index 59d5d24..fa0099a 100644  --- a/The simulation.tex  +++ b/The simulation.tex 
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Regions collapsing beyond this point were replaced by sink particles, using the sink implementation described in \citet{2010MNRAS.409..985D}, which largely follows the implementation of \citet{2004ApJ...611..399K}. The salient points of this implementation are that regions exceeding the Truelove density limit on the finest level of refinement and that are collapsing along all directions are replaced by sink particles. The sinks accrete gas in a momentum conserving fashion from a region 4 cells in radius ($\sim0.01$ pc) at the local Bondi-Hoyle rate in that region. While the sinks are addressed in this paper, we can approximate the integrated star formation efficiency as the mass in sinks.   We integrated the box through $\sim1.25$ $\sim2.1$  Myr of self gravitating evolution. Following \citet{2007ApJ...665..416K}'s definition of the turbulent turnover time in a box , $T_{turb} = S/(2 c_s \mathcal{M})$, we have $T_{turb} \sim 3$ Myr. The free-fall time $T_{ff} = [3\pi / (32 G \rho)]^{1/2}$, at the mean density of the simulation, is also roughly 3 Myr. In this paper we focus on moderately dense gas, with $10^3 < n/{\rm cm}^{-3} < 10^{4.5}$; at these densities we have $0.2 \lesssim T_{ff} / \rm{Myr} \lesssim 1.0$. At 1.25 After 1  Myr the global structure of the simulated box is thus still  dominated by the initial  turbulence, while the denser gas has had time to become organized by self gravity.