deletions | additions       diff --git a/The simulation.tex b/The simulation.tex  index a1c1de1..82e7878 100644  --- a/The simulation.tex  +++ b/The simulation.tex 
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We simulated the collapse of a turbulent molecular cloud, treating gravity and hydrodynamics. The initial conditions were taken from a periodic turbulent cube simulated with the ATHENA code \citep{2005JCoPh.205..509G,2008JCoPh.227.4123G,2008ApJS..178..137S,2009NewA...14..139S}. The turbulence was generated in a manner very similar to that of \citet{http://adsabs.harvard.edu/abs/2008ApJ...682L..97L} \citet{2008ApJ...682L..97L}  and \citet{http://adsabs.harvard.edu/abs/2009ApJ...691.1092L}. \citet{2009ApJ...691.1092L}.  Briefly, on a $768^{3}$ grid we applied divergence-free velocity perturbations at every timestep to an initially uniform medium. The perturbations had a Gaussian random distribution with a Fourier power spectrum \begin{equation}  \left{|} d {\bf v}_{k}^{2} \right{|} \propto 
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The turbulence was driven until it saturated at a Mach number of roughly 8, then allowed to decay to Mach 7.   We then carved a sphere of diameter 512 out of the turbulent box to use as our initial cloud. Upon scaling to physical units, the cloud consisted of $5\times10^{4}$ M$_\sun$ of gas in a sphere with radius 12.5 pc. The further evolution of the cloud is performed with the adaptive mesh refinement (AMR) code RAMSES \citep{http://adsabs.harvard.edu/abs/2002A%26A...385..337T} \citep{2002A&A...385..337T}