deletions | additions       diff --git a/Initial Conditions.tex b/Initial Conditions.tex  index feb1564..9ae23e0 100644  --- a/Initial Conditions.tex  +++ b/Initial Conditions.tex 
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\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.  \item For multidimensional simulations, do collapse in 1D up to 15\,ms after bounce, then transition to 2D. Add perturbations via a clearly defined manner.  \item Perform simulations using both Newtonian gravity and and/or  some form of general relativistic gravity (either effective potential, true GR). \end{enumerate}  \subsection{Neutrino Physics}  \begin{enumerate}