User: diener Date: 2011/08/21 03:30 PM

Modified: / ET.tex

Log: Add the first couple of plots for the distorted rotating black hole example.

File Changes:

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

File [modified]: ET.tex Delta lines: +20 -1 =================================================================== --- ET.tex 2011-08-21 20:29:34 UTC (rev 111) +++ ET.tex 2011-08-21 20:30:39 UTC (rev 112) @@ -2252,8 +2252,27 @@ resolution on the finest grid and the second number in parenthesis is the resolution on the coarsest grid. The runs where performed using the tapering evolution scheme in \codename{Carpet} in order to avoid interpolation in -time during prolongation. +time during prolongation. The initial data corresponds to a rotating black +hole perturbed by an $\ell =2, m=0$ Brill wave and as such has a non-zero +gravitational wave content. We evolved using 4th order finite differencing from +$T=0M$ until the black hole had settled down to a stationary state at $T=120M$.

+\begin{figure} + \includegraphics[width=0.33\textwidth,angle=-90]{examples/kerr/figs/waves} + \includegraphics[width=0.33\textwidth,angle=-90]{examples/kerr/figs/waves_conv} + \caption{The right plot shows the extracted $\ell =2, m=0$ mode of $\Psi_4$ + as function of time from the high resultion run. The extraction was + done at $R=30M$. Shown is both the real (solid red line) and the + imaginary (dashed green line) part of the waveform. The left plot + shows for the real part of the $\ell =2, m=0$ waveforms the + difference between the medium and low resolution runs (solid red + line), the difference between the high and medium resolution runs + (dashed green line) as well as the scaled (for 4th order + convergence) difference between the medium and low resolution runs + (dotted blue line).} + \label{fig:kerr_waves} +\end{figure} + \subsection{BHB\pages{2 Bruno}} \label{sec:bbh-example} %BCM: DONE:ID parameters, TP number of collocation points, grid structure,