User: knarf Date: 2011/08/01 09:55 AM

Added: / TODO

Modified: / ET.tex

Log: a temporary TODO file

File Changes:

Directory: / ============

File [modified]: ET.tex Delta lines: +10 -6 =================================================================== --- ET.tex 2011-08-01 13:21:13 UTC (rev 94) +++ ET.tex 2011-08-01 14:55:33 UTC (rev 95) @@ -23,6 +23,8 @@

\graphicspath{{figures/}}

+\setcounter{secnumdepth}{5} + \def\grb#1{gamma-ray burst#1 (GRB#1)\gdef\grb{GRB}} \def\gw#1{gravitational wave#1 (GW#1)\gdef\gw{GW}} \def\bh#1{black hole#1 (BH#1)\gdef\bh{BH}} @@ -579,7 +581,7 @@ and conventions (see section~\ref{sec:base_modules}). Others provide initial data (see section~\ref{sec:initial_data}). These initial data have to be evolved, using different evolution methods, described in -sections~\ref{sec:Kevol} and~\ref{sec:GRHydro}. +section~\ref{sec:evol}. Simulations including matter require a description of the matter properties, encoded in equations of state (see section~\ref{sec:eoss}). @@ -965,7 +967,7 @@ the ODE solution nor the resulting density profile.

\subsection{Spacetime Curvature and Hydrodynamics Evolution} -\label{sec:Kevol} +\label{sec:evol} \todo{Christian in charge}

In the following, we assume that the reader is familiar with the @@ -1002,7 +1004,9 @@ the relativistic specific enthalpy with $\epsilon$ and $P$ being the specific internal energy and the pressure, respectively.

-\subsubsection{Spacetime Curvature Evolution} The Einstein Toolkit +\subsubsection{Spacetime Curvature Evolution} +\label{sec:Kevol} +The Einstein Toolkit curvature evolution code \codename{McLachlan}~\cite{brown:09,reisswig:11ccwave} is auto-generated from tensor equations via \codename{Kranc} (Sec.~\ref{sec:kranc}). It implements the Einstein equations in a @@ -1169,7 +1173,7 @@

-\subsubsection{Initial Conditions} +\paragraph{Initial Conditions}

Initial conditions from the ADM variables $g_{ij}$, $K_{ij}$, lapse $\alpha$, and shift $\beta^i$, as provided by the initial data @@ -1193,7 +1197,7 @@ then defined via the points in the interior and the previously calculated layers.

-\subsubsection{Boundary Conditions} +\paragraph{Boundary Conditions} \label{sec:curv_boundaries}

During time evolution, a Sommerfeld-type radiative boundary condition @@ -1262,7 +1266,7 @@ gauge conditions used in \codename{McLachlan}.

-\subsection{Hydrodynamics: \codename{GRHydro}} +\subsection{Hydrodynamics: \codename{GRHydro}}\pages{Christian} \label{sec:GRHydro}

File [added]: TODO Delta lines: +9 -0 =================================================================== --- TODO (rev 0) +++ TODO 2011-08-01 14:55:33 UTC (rev 95) @@ -0,0 +1,9 @@ +someone (1) : references! + +Ian Hinder : Expand section on Kranc, a bit +Christian Ott: Curvature evolution looks good, but what about GRHydro? + EOS? +Peter : Tools not ready (puncture and star tracker, but into analysis) +Roland : Merge AMR sections (4.2 and 5.8.3 currently) +Peter, Frsank, Bruno, Christian: Examples! +Frank : Future Work