User: knarf Date: 2011/08/01 11:06 AM
Modified: / ET.tex
Log: get some of the structure of the evolution methods straight
File Changes:
Directory: / ============
File [modified]: ET.tex Delta lines: +5 -6 =================================================================== --- ET.tex 2011-08-01 15:50:41 UTC (rev 97) +++ ET.tex 2011-08-01 16:05:59 UTC (rev 98) @@ -966,9 +966,8 @@ one may also apply a uniform velocity to the neutron star, though this does not affect the ODE solution nor the resulting density profile.
-\subsection{Spacetime Curvature Evolution} +\subsection{Spacetime Curvature Evolution}\todo{Peter: move} \label{sec:evol} -\todo{Josh and Christian in charge}
In the following, we assume that the reader is familiar with the basics of numerical relativity and GR hydrodynamics. Detailed @@ -1004,7 +1003,7 @@ the relativistic specific enthalpy with $\epsilon$ and $P$ being the specific internal energy and the pressure, respectively.
-\subsubsection{Spacetime Curvature Evolution} +\subsection{Spacetime Curvature Evolution} \label{sec:Kevol} The Einstein Toolkit curvature evolution code \codename{McLachlan}~\cite{brown:09,reisswig:11ccwave} is @@ -1173,7 +1172,7 @@
-\paragraph{Initial Conditions} +\subsubsection{Initial Conditions}
Initial conditions from the ADM variables $g_{ij}$, $K_{ij}$, lapse $\alpha$, and shift $\beta^i$, as provided by the initial data @@ -1197,7 +1196,7 @@ then defined via the points in the interior and the previously calculated layers.
-\paragraph{Boundary Conditions} +\subsubsection{Boundary Conditions} \label{sec:curv_boundaries}
During time evolution, a Sommerfeld-type radiative boundary condition @@ -1266,7 +1265,7 @@ gauge conditions used in \codename{McLachlan}.
-\subsection{Hydrodynamics: \codename{GRHydro}}\pages{Christian and Josh} +\subsection{Hydrodynamics Evolution}\pages{Christian and Josh} \label{sec:GRHydro}
{\color{red} This text is copied from Reisswig et al. It needs to be expanded a bit and we probably want to talk about the numerical methods a bit more.}