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\section{Initial Conditions}  \subsection{Non-neutrino Physics}  \begin{enumerate}  \item Progenitor: $20\,M_\odot$ model from \cite{WOOSLEY_2007}. This model is available from the authors. Ideally, we would compare both a successful explosion and a failed explosion to test codes in both regimes. For this, we may need to add a second progenitor at a later stage. After seeing the outcome of these simulations.  \item For mapping the progenitor, we will use density, temperature, and ye. Careful to note the definition of the radial coordinate in the initial model (radial coordinate is the location of the outer edge of the zone, the velocity is also defined at this radius, the remaining required quantities (rho, temperature, ye) are defined as cell averages).  \item Equation of state: The SFHo nuclear equation of state from \cite{Steiner_2013} available from \url{http://phys-merger.physik.unibas.ch/~hempel/eos.html} or \url{http://www.stellarcollapse.org/equationofstate}. This EOS extends down to densities of $1\,\mathrm{g}\,\mathrm{cm}^{-3}$. In this EOS, NSE is assumed down to these densities (which is incorrect for supernovae). However, to eliminate (for now) issues related to low density equations of state and nuclear reaction networks, this study will use only the SFHo equation of state for all densities, temperatures, and ye's.  \item Boundary and Boundary Conditions: The SFHo EOS only goes down to $0.1\,$MeV, therefore the outer boundary must be closer than $1.2\times 10^9\,\mathrm{cm}$. For this comparison, we would like the outer boundary to be taken as $10^9\,\mathrm{cm}$. For the outer boundary conditions, fix the density and velocity so as to maintain a constant mass accretion rate. This is not the most physical boundary condition, but ensures the same condition is used by different groups.