[Commits] [svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 95)

[knarf at cct.lsu.edu]

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