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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 40)
by roland.haas＠physics.gatech.edu 28 Mar '11

28 Mar '11

User: rhaas Date: 2011/03/28 09:54 AM Modified: / ET.tex Log: add some text to Simulation Domain section mostly only name the thorns involved, what services they offer File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +38 -5 =================================================================== --- ET.tex 2011-03-28 13:38:16 UTC (rev 39) +++ ET.tex 2011-03-28 14:54:05 UTC (rev 40) @@ -903,9 +903,12 @@ -\subsection{Simulation Domain, Symmetries, Boundaries\pages{3 Roland?}} - +\subsection{Simulation Domain, Symmetries, Boundaries\pages{3 Roland}} +\unknowasdag \paragraph{Domains and Coordinates.} +The Einstein Toolkit provides a module \codename{CoordBase} to facilate +the specification of the simulation domain independend from the actual +evolution module used. The simulation domain is specified via the parameter file \todo{ES: ensure this has been defined above}. Cactus distinguishes between the \emph{physical} domain, which lives in the continuum, and @@ -924,23 +927,53 @@ the numerical resolution do not affect the extent of the physical domain, i.e.\ that the discrete domains converge to the physical domain in the limint of infinite resolution. +\codename{CoordBase} exposes a public interface that allows other +modules to query the domain and description in a uniform way. This +information is used e.g.\ by modules computing the total barionic mass of +the system to determine the region over which to intergrate the mass +density. Evolution modules use this information to decide which points +are evolved and therefore require the evaluation of the righ-hand-side +expression and which ones are set via boundary or symmetry conditions. \paragraph{Symmetries, Boundary Conditions.} +The Einstein Toolkit includes a set of modules, \codename{Boundary} +and \codename{SymBase}, to provide a generic interface to boundary and +symmetry conditions. The Einstein Toolkit offers a set of reflecting or rotating symmetry conditions that can be used to reduce the size of the simulation -domain. These symmetries include periodicity, reflections about the -coordinate planes, and $90^{\circ}$ and $180^{\circ}$ rotational +domain. These symmetries include periodicity +(via the \codename{Periodic} module), reflections about the +coordinate planes (via the \codename{Reflection} module), +and $90^{\circ}$ and $180^{\circ}$ rotational +(via the \codename{RotatingSymmetry90} and +\codename{RotatingSymmetry180} modules respectively) symmetries about the $z$ axis. In applying these symmetries, the transformation behaviour of tensorial quantities (including tensor densities and non-tensors such as Christoffel symbols) is correctly taken into account. - +The interpolation routines present in \codename{Cactus} automatically +take the existing symmetries into account, transparently mapping points +to the numerical domain and respecting the transformation behaviour of +tensorial quantities. Symmetries therefore are handled transparently +from the point of view of user modules. The Einstein Toolkit also offers a set of boundary conditions, including Dirichlet, von Neumann, and Robin (fall-off) boundary conditions, as well as extrapolation and radiative boundary conditions. +\comment{RH: Christian already describes NewRad's boundary conditions in +his section (these should be used for extrapolation and radiative +boundary conditions I think). Should they eventually be moved here (once +the paper is almost ready)?} \paragraph{Adaptive Mesh Refinement} +The \codename{Carpet} driver module provides adaptive mesh refinement and +Multi-Block capabilities to modules in the Einstein Toolkit. As in most +adaptive mesh refinement frameworks, care has been taken to separate +driver related code from physics codes. A typical evolution or analysis +code like \codename{McLachlan} or \codename{WeylScal4} is agnostic to +the mesh refinement. +\todo{RH: add description and motivation of/for Berger-Rigoustos scheme?} +\todo{RH: add interaction with MoL?} Carpet supports feature-based mesh refinement, which is based on extracting e.g.\ the locations of black holes or neutron stars, and then constructing a mesh hierarchy (stacks of refined regions) based

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 39)
by roland.haas＠physics.gatech.edu 28 Mar '11

28 Mar '11

User: rhaas Date: 2011/03/28 08:38 AM Added: / cuted.sty, flushend.sty Log: add missing style files required by widetext.sty missing at least on RH5 machines (from /macros/latex/contrib/sttools). File Changes: Directory: / ============ File [added]: cuted.sty Delta lines: +474 -0 =================================================================== --- cuted.sty (rev 0) +++ cuted.sty 2011-03-28 13:38:16 UTC (rev 39) @@ -0,0 +1,474 @@ +%% cuted.sty +%% Copyright 1997 Sigitas Tolu\v sis +%% VTeX Ltd., Akademijos 4, Vilnius, Lithuania +%% e-mail sigitas(a)vtex.lt +%% http://www.vtex.lt/tex/download/macros/ +%% +% This program can redistributed and/or modified under the terms +% of the LaTeX Project Public License Distributed from CTAN +% archives in directory macros/latex/base/lppl.txt; either +% version 1 of the License, or (at your option) any later version. +% +% PURPOSE: Insert some onecolumn material in full-width on double-column page. +% +% SHORT DESCRIPTION: +% +% It is denoted to place some material in full-width at any place +% on double-column page (\twocolumn mode). The part of material +% can be placed on the next page. Existing text is placed +% under inserted material in two columns (it is reformatted). +% +% Provides new environment: +% +% \begin{strip} ... \end{strip} +% ----------------------------- +% +% Puts \vbox{...} in full-width on double-column page. +% Adds \stripsep glue before and after +% (By default \stripsep=15pt plus2pt minus 2pt). +% It can be problems with floats and footnotes. In the case of +% problems with footnotes it is possible to correct the situation +% using commands \footnotemark and \footnotetext. +% +% Provides new command: +% \oldcolsbreak{#1} +% +% Adds #1 in place of original column break if strip is placed +% on the right column. +% +% \changes{1997/09/02}{improved column balancing} +% \changes{1997/09/03}{float control for \@colroom setting} +% \changes{1997/09/04}{improved \@colroom setting} +% \changes{1997/09/05}{checking for \@viper and \hold@viper} +% \changes{1997/09/09}{compatibility with flushend.sty} +% \changes{1997/09/22}{improved \output ir \@specialoutput} +% \changes{1997/10/01}{improved \output ir \@addviper} +% +\NeedsTeXFormat{LaTeX2e} +\ProvidesPackage{cuted}[1997/10/01] +% +\newtoks\At@ViperColsBreak \At@ViperColsBreak{} +\def\oldcolsbreak#1{\global\At@ViperColsBreak{#1}} +\newbox\v@aaa +\newbox\v@ccc +\@ifundefined{stripsep}{\newskip\stripsep\stripsep 15pt plus 2pt minus 2pt}{} +% +\@ifundefined{@viper}{\newbox\@viper}{} +\newif\if@lastviper \@lastviperfalse +\def\@outputdblcol{% + \if@firstcolumn + \global \@firstcolumnfalse + \global \setbox\@leftcolumn \box\@outputbox + \else + \global \@firstcolumntrue + \setbox\@outputbox \vbox {% + \hb@xt@\textwidth {% + \hb@xt@\columnwidth {% + \box\@leftcolumn \hss}% + \hfil + \vrule \@width\columnseprule + \hfil + \hb@xt@\columnwidth {% + \box\@outputbox \hss}% + }% + }% + \ifvoid\hold@viper + \else + \setbox\@outputbox \vbox{\box\hold@viper\box\@outputbox}% + \fi + \@combinedblfloats + \@outputpage + \begingroup + \@dblfloatplacement + \@startdblcolumn + \@whilesw\if@fcolmade \fi + {\@outputpage + \@startdblcolumn}% + \ifvoid\@viper + \else + \global\setbox\@viper\vbox{% + \vskip-\stripsep\unvbox\@viper}\@viperoutput + \fi + \endgroup + \fi +} +\mathchardef\@Mv=10005 +\newcount\viper@penalty +\def\strip{% + \ifinner + \@parmoderr\viper@penalty\z@ + \else + \viper@penalty=-\@Mv\relax + \fi + \global \setbox\@viper\vbox\bgroup% + \hsize\textwidth + \@parboxrestore + \col@number \@ne + \vrule height\topskip width0pt depth0pt +} +\def\endstrip{% + \egroup + \ifnum\viper@penalty <-\@Mii + \penalty -\@Miv + \@tempdima\prevdepth %% saving and restoring \prevdepth added + \vbox{}% %% 26 May 87 to prevent extra vertical + \prevdepth \@tempdima %% space when used in vertical mode + \penalty-\@Mv\relax + \fi +} +\gdef\@viperoutput{% + \global \setbox\@holdpg \vbox{% + \unvbox\@holdpg + \unvbox\@cclv + \setbox\@tempboxa \lastbox + \unskip + }% + \@pagedp \dp\@holdpg + \@pageht \ht\@holdpg + \ifvoid\@viper\else + \advance \@pageht \@pagedp + \ifvoid\footins \else + \advance \@pageht \ht\footins + \advance \@pageht \skip\footins + \advance \@pageht \dp\footins + \fi + \ifvbox \@kludgeins + \ifdim \wd\@kludgeins=\z@ + \advance \@pageht \ht\@kludgeins + \fi + \fi + \@reinserts + \@addviper + \fi +} +\gdef\@specialoutput{% + \ifnum \outputpenalty>-\@Mii + \@doclearpage + \else + \ifnum \outputpenalty<-\@Miii + \ifnum \outputpenalty<-\@MM \deadcycles \z@ \fi + \ifnum \outputpenalty=-10005 + \@viperoutput + \ifnum \outputpenalty<\z@ + \if@nobreak + \else + \addpenalty \interlinepenalty + \fi + \fi + \else + \global \setbox\@holdpg \vbox {\unvbox\@cclv}% + \fi + \else + \global \setbox\@holdpg \vbox{% + \unvbox\@holdpg + \unvbox\@cclv + \setbox\@tempboxa \lastbox + \unskip + }% + \@pagedp \dp\@holdpg + \@pageht \ht\@holdpg + \unvbox \@holdpg + \@next\@currbox\@currlist{% + \ifnum \count\@currbox>\z@ + \advance \@pageht \@pagedp + \ifvoid\footins \else + \advance \@pageht \ht\footins + \advance \@pageht \skip\footins + \advance \@pageht \dp\footins + \fi + \ifvbox \@kludgeins + \ifdim \wd\@kludgeins=\z@ + \advance \@pageht \ht\@kludgeins + \fi + \fi + \@reinserts + \@addtocurcol + \else + \@reinserts + \@addmarginpar + \fi + }\@latexbug + \ifnum \outputpenalty<\z@ + \if@nobreak + \else + \addpenalty \interlinepenalty + \fi + \fi + \fi + \fi +} +\@ifundefined{hold@viper}{\newbox\hold@viper}{} +\newdimen\ht@viper +\def \@addviper {% + \if@firstcolumn + \@insertfalse + \@reqcolroom .5\@pageht + \ht@viper\@reqcolroom + \advance \@reqcolroom \ht\@viper + \advance \@reqcolroom \stripsep + \ifvoid\hold@viper\@tempdima=\z@\else\@tempdima\ht\hold@viper\fi +% + \@tempdimb \ht@viper + \loop + \setbox\v@aaa\copy\@holdpg + \setbox\v@ccc\vbox to\@tempdimb{% + \vsplit\v@aaa to\@tempdimb\vss\vsplit\v@aaa to\@tempdimb}% + \wlog{Extra height:\the\ht\v@aaa\space when \the\@tempdimb}% + \ifvoid\v@aaa \else \advance\@tempdimb 1pt \repeat% + \loop + \setbox\v@aaa\copy\@holdpg + \setbox\v@ccc\vbox to\@tempdimb{% + \vsplit\v@aaa to\@tempdimb\vss}% + \wlog{(2)Left:\the\ht\v@ccc\space Right:\the\ht\v@aaa\space Output:\the\@tempdimb}% + \ifdim \ht\v@ccc<\ht\v@aaa \@tempdimb \the\ht\v@aaa \repeat% + \wlog{- LAST -^^JLeft:\the\ht\v@ccc^^JRight:\the\ht\v@aaa^^JOutput:\the\@tempdimb}% + \setbox\v@ccc\vbox to\@tempdimb{% + \vsplit\@holdpg to\@tempdimb\vss}% +% + \setbox\@tempboxa \vbox {% + \hb@xt@\textwidth {% + \hb@xt@\columnwidth {% +% \vbox to\ht@viper{\vsplit\@holdpg to\ht@viper\vss} \hss}% + \vbox to\ht@viper{\box\v@ccc\vss} \hss}% + \hfil + \vrule \@width\columnseprule + \hfil + \hb@xt@\columnwidth {% + \vbox to\ht@viper{\box\@holdpg\vss} \hss}% + }% + }% + \ifvoid\hold@viper + \global\setbox\hold@viper \vbox {% + \unvbox\@tempboxa + \penalty\interlinepenalty + \vskip\stripsep + \ifnum\outputpenalty <-\@Mii \vskip -\parskip\fi + \outputpenalty \z@ + }% + \else + \global\setbox\hold@viper \vbox {% + \unvbox\hold@viper + \unvbox\@tempboxa + \penalty\interlinepenalty + \vskip\stripsep + \ifnum\outputpenalty <-\@Mii \vskip -\parskip\fi + \outputpenalty \z@ + }% + \fi + \ifdim \@colroom>\@reqcolroom + \global\setbox\hold@viper \vbox {% + \unvbox\hold@viper + \box\@viper + \penalty\interlinepenalty + \vskip\stripsep + \ifnum\outputpenalty <-\@Mii \vskip -\parskip\fi + \outputpenalty \z@ + }% + \@inserttrue + \advance\@tempdima by-\ht\hold@viper + \global \advance \@colht \@tempdima + \ifdim \@colht<2.5\baselineskip + \@latex@warning@no@line {Optional argument of \noexpand\twocolumn + too tall on page \thepage (1 stulpelis)}% + \@emptycol + \if@firstcolumn + \else + \@emptycol + \fi + \global\@lastvipertrue + \else + \global \vsize \@colht + \global \@colroom \@colht + \check@floats + \ifdim\@tempdima>\z@ + \global\advance\@colroom by-\@tempdima + \fi + \ifdim\@colroom<\z@ + \global\@colroom 1pt + \ifdim\@tempdima>\@colht + \@latex@warning@no@line {TOP ir/ar BOT FLOAT's + netelpa lape \thepage (1 stulpelis)}% + \fi + \@emptycol + \if@firstcolumn + \else + \@emptycol + \fi + \global\@lastvipertrue + \fi + \fi + \fi + \else + \@insertfalse + \@reqcolroom\@colht + \advance\@reqcolroom \@pageht + \ht@viper.5\@reqcolroom + \@reqcolroom\ht@viper + \advance \@reqcolroom \ht\@viper + \advance \@reqcolroom \stripsep + \global\setbox\@holdpg\vbox{\unvbox\@leftcolumn + \setbox\@tempboxa\lastbox\unskip\the\At@ViperColsBreak\unvbox\@holdpg}% + \global\At@ViperColsBreak{}% + \ht@viper .5\ht\@holdpg + \ifvoid\hold@viper\@tempdima=\z@\else\@tempdima\ht\hold@viper\fi +% + \@tempdimb \ht@viper + \loop + \setbox\v@aaa\copy\@holdpg + \setbox\v@ccc\vbox to\@tempdimb{% + \vsplit\v@aaa to\@tempdimb\vss\vsplit\v@aaa to\@tempdimb}% + \wlog{Extra height:\the\ht\v@aaa\space when \the\@tempdimb}% + \ifvoid\v@aaa \else \advance\@tempdimb 1pt \repeat% + \loop + \setbox\v@aaa\copy\@holdpg + \setbox\v@ccc\vbox to\@tempdimb{% + \vsplit\v@aaa to\@tempdimb\vss}% + \wlog{(2)Left:\the\ht\v@ccc\space Right:\the\ht\v@aaa\space Output:\the\@tempdimb}% + \ifdim \ht\v@ccc<\ht\v@aaa \@tempdimb \the\ht\v@aaa \repeat% + \wlog{- LAST -^^JLeft:\the\ht\v@ccc^^JRight:\the\ht\v@aaa^^JOutput:\the\@tempdimb}% + \setbox\v@ccc\vbox to\@tempdimb{% + \vsplit\@holdpg to\@tempdimb\vss}% +% + \setbox\@tempboxa\vbox{% + \hb@xt@\textwidth {% + \hb@xt@\columnwidth {% +% \vbox to\ht@viper{\vsplit\@holdpg to \ht@viper\vss} \hss}% + \vbox to\ht@viper{\box\v@ccc\vss} \hss}% + \hfil + \vrule \@width\columnseprule + \hfil + \hb@xt@\columnwidth {% + \vbox to\ht@viper{\box\@holdpg\vss} \hss}% + }% + }% + \ifvoid\hold@viper + \global\setbox\hold@viper \vbox {% + \unvbox\@tempboxa + \penalty\interlinepenalty + \vskip\stripsep + \ifnum\outputpenalty <-\@Mii \vskip -\parskip\fi + \outputpenalty \z@ + }% + \else + \global\setbox\hold@viper \vbox {% + \unvbox\hold@viper + \unvbox\@tempboxa + \penalty\interlinepenalty + \vskip\stripsep + \ifnum\outputpenalty <-\@Mii \vskip -\parskip\fi + \outputpenalty \z@ + }% + \fi + \ifdim \@colht>\@reqcolroom + \global\setbox\hold@viper \vbox {% + \unvbox\hold@viper + \box\@viper + \penalty\interlinepenalty + \vskip\stripsep + \ifnum\outputpenalty <-\@Mii \vskip -\parskip\fi + \outputpenalty \z@ + }% + \@inserttrue + \global\@firstcolumntrue + \advance\@tempdima by-\ht\hold@viper + \global \advance \@colht \@tempdima + \ifdim \@colht<2.5\baselineskip + \@latex@warning@no@line {Optional argument of \noexpand\twocolumn + too tall on page \thepage (2 stulpelis)}% + \@emptycol + \if@firstcolumn + \else + \@emptycol + \fi + \global\@lastvipertrue + \else + \global \vsize \@colht + \global \@colroom \@colht + \check@floats + \ifdim\@tempdima>\z@ + \global\advance\@colroom by-\@tempdima + \fi + \ifdim\@colroom<\z@ + \global\@colroom 1pt + \ifdim\@tempdima>\@colht + \@latex@warning@no@line {TOP ir/ar BOT FLOAT's + netelpa lape \thepage (2 stulpelis)}% + \fi + \@emptycol + \if@firstcolumn + \else + \@emptycol + \fi + \global\@lastvipertrue + \fi + \fi + \fi + \fi + \if@insert + \else + \advance\@tempdima by-\ht\hold@viper + \global \advance \@colht \@tempdima + \global\setbox\hold@viper \vbox {% + \unvbox\hold@viper + \vsplit\@viper to \@colht + \vss + }% + \vbox{}% + \global\@firstcolumnfalse + \newpage + \fi +} + +\def \check@floats {% + \global\@tempdima\z@ + \let \@elt \ht@comflelt + \ifx \@toplist\@empty \else\@toplist \fi + \ifx \@botlist\@empty \else\@botlist \fi +} +\def\ht@comflelt#1{\setbox\@tempboxa\vbox{\copy #1\vskip\floatsep}% +\global\advance\@tempdima\ht\@tempboxa} + +\output {% + \let \par \@@par + \ifnum \outputpenalty<-\@M + \@specialoutput + \else + \@makecol + \@opcol + \@startcolumn + \@whilesw \if@fcolmade \fi + {% + \@opcol\@startcolumn}% + \fi + \ifnum \outputpenalty>-\@Miv + \ifdim \@colroom<1.5\baselineskip + \ifdim \@colroom<\textheight + \@latex@warning@no@line {Text page \thepage\space + contains only floats}% + \if@lastviper\else\@emptycol\fi + \if@twocolumn + \if@firstcolumn + \else + \@emptycol + \fi + \fi + \global\@lastviperfalse + \else + \global \vsize \@colroom + \fi + \else + \global \vsize \@colroom + \fi + \else + \ifnum\outputpenalty<-100005 + \global \vsize \maxdimen + \else + \global \vsize \@colroom + \fi + \fi +} +\endinput + + + + File [added]: flushend.sty Delta lines: +141 -0 =================================================================== --- flushend.sty (rev 0) +++ flushend.sty 2011-03-28 13:38:16 UTC (rev 39) @@ -0,0 +1,141 @@ +%% flushend.sty +%% Copyright 1997 Sigitas Tolu\v sis +%% VTeX Ltd., Akademijos 4, Vilnius, Lithuania +%% e-mail sigitas(a)vtex.lt +%% http://www.vtex.lt/tex/download/macros/ +%% +% This program can redistributed and/or modified under the terms +% of the LaTeX Project Public License Distributed from CTAN +% archives in directory macros/latex/base/lppl.txt; either +% version 1 of the License, or (at your option) any later version. +% +% PURPOSE: Balanced columns on last page in twocolumn mode. +% +% SHORT DESCRIPTION: +% +% \flushend (loaded by default) +% --------- +% Switches on column balancing at last page +% +% \raggedend +% ---------- +% Switches off column balancing at last page +% +% \atColsBreak={#1} +% ------------------ +% Adds #1 in place of original column break (without balancing) +% Example: \atColsBreak{\vskip-2pt} +% +% \showcolsendrule +% ---------------- +% Adds rule to the bottom of columns (just for debugging) +% +% P.S. To stretch right column by #1 add command \vskip-#1 just before +% command \end{document}. +% TO shrink right column by #1 add command \vskip#1 just before +% command \end{document}. +% Example: \vskip-10pt +% \end{document} +% +% \changes{1997/05/16}{first version} +% \changes{1997/09/09}{support for compatibility with cuted.sty} +% \changes{1997/10/01}{\vipersep changed to \stripsep for compatibility with cuted.sty} +% +\NeedsTeXFormat{LaTeX2e} +\ProvidesPackage{flushend}[1997/10/01] +% +\newbox\@aaa +\newbox\@ccc +\@ifundefined{@viper}{\newbox\@viper}{} +\@ifundefined{hold@viper}{\newbox\hold@viper}{} +\newtoks\atColsBreak \atColsBreak={} +\newdimen\@extra@skip \@extra@skip\z@ +\newdimen\@nd@page@rule \@nd@page@rule\z@ +\def\last@outputdblcol{% + \if@firstcolumn + \global \@firstcolumnfalse + \global \setbox\@leftcolumn \box\@outputbox + \else + \global \@firstcolumntrue + \if@lastpage + \@tempdima\ht\@leftcolumn + \splittopskip\topskip\splitmaxdepth\maxdepth + \setbox\@tempboxa\vbox{% + \unvbox\@leftcolumn\setbox0\lastbox\unskip% + \the\atColsBreak% + \unvbox\@outputbox\setbox0\lastbox\unskip}% + \@tempdimb .5\ht\@tempboxa% + \loop + \setbox\@aaa\copy\@tempboxa% + \setbox\@ccc\vbox to\@tempdimb{% + \vsplit\@aaa to\@tempdimb\vss\vsplit\@aaa to\@tempdimb}% + \wlog{Extra height:\the\ht\@aaa\space when \the\@tempdimb}% + \ifvoid\@aaa \else \advance\@tempdimb 1pt \repeat% + \loop + \setbox\@aaa\copy\@tempboxa% + \setbox\@ccc\vbox to\@tempdimb{% + \vsplit\@aaa to\@tempdimb\vss}% + \wlog{(2)Left:\the\ht\@ccc\space Right:\the\ht\@aaa\space Output:\the\@tempdimb}% + \ifdim \ht\@ccc<\ht\@aaa \@tempdimb \the\ht\@aaa \repeat% + \wlog{- LAST -^^JExtra skip:\the\@extra@skip^^JLeft:\the\ht\@ccc^^JRight:\the\ht\@aaa^^JOutput:\the\@tempdimb}% + \setbox\@ccc\vbox to\@tempdimb{% + \vsplit\@tempboxa to\@tempdimb\vss}% + \setbox\@leftcolumn\vbox to\@tempdima{% + \vbox to\@tempdimb{\unvbox\@ccc}% + \hrule\@height\@nd@page@rule% + \vss}% + \setbox\@outputbox\vbox to\@tempdima{% + \vbox to\@tempdimb{\unvbox\@tempboxa\vfilneg\vskip\@extra@skip}% + \hrule\@height\@nd@page@rule% + \vss}% + \setbox\@outputbox \vbox {% + \hb@xt@\textwidth {% + \hb@xt@\columnwidth {% + \box\@leftcolumn \hss}% + \hfil + \vrule \@width\columnseprule + \hfil + \hb@xt@\columnwidth {% + \box\@outputbox \hss}% + }% + }% + \else + \setbox\@outputbox \vbox {% + \hb@xt@\textwidth {% + \hb@xt@\columnwidth {% + \box\@leftcolumn \hss}% + \hfil + \vrule \@width\columnseprule + \hfil + \hb@xt@\columnwidth {% + \box\@outputbox \hss}% + }% + }% + \fi + \ifvoid\hold@viper + \else + \setbox\@outputbox \vbox{\box\hold@viper\box\@outputbox}% + \fi + \@combinedblfloats + \@outputpage + \begingroup + \@dblfloatplacement + \@startdblcolumn + \@whilesw\if@fcolmade \fi + {\@outputpage + \@startdblcolumn}% + \ifvoid\@viper + \else + \global\setbox\@viper\vbox{% + \vskip-\stripsep\unvbox\@viper}\@viperoutput + \fi + \endgroup + \fi +} +\let\prev@enddocument\enddocument +\newif\if@lastpage \@lastpagefalse +\def\enddocument{\global\@lastpagetrue\let\@outputdblcol\last@outputdblcol\prev@enddocument} +\def\raggedend{\global\let\enddocument\prev@enddocument} +\def\flushend{\gdef\enddocument{\global\@lastpagetrue\let\@outputdblcol\last@outputdblcol\prev@enddocument}} +\def\showcolsendrule{\global\@nd@page@rule=.4pt} +\endinput

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 38)
by cott＠tapir.caltech.edu 26 Mar '11

26 Mar '11

User: cott Date: 2011/03/26 09:28 PM Modified: / ET.tex Log: * more evolution text File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +19 -11 =================================================================== --- ET.tex 2011-03-26 15:14:54 UTC (rev 37) +++ ET.tex 2011-03-27 02:28:19 UTC (rev 38) @@ -553,6 +553,9 @@ Alcubierre~\cite{alcubierre:08} and Baumgarte \& Shapiro~\cite{baumgarte:10}. GR hydrodynamics has been reviewed by Font~\cite{font:08}. +\todo{state Einstein equations, mention conventions, give stress +energy tensor} + \subsubsection{Spacetime Curvature Evolution} The Einstein Toolkit curvature evolution code \codename{McLachlan}~\cite{brown:09} is auto-generated from tensor equations via \codename{Kranc} @@ -561,26 +564,31 @@ \cite{york:79}. For this, the Baumgarte-Shapiro-Shibata-Nakamura (BSSN) conformal-tracefree reformulation \cite{shibata:95,baumgarte:95,alcubierre:00} of the original -Arnowitt-Deser-Misner formalism~\cite{adm:62} is employed. +Arnowitt-Deser-Misner (ADM) formalism~\cite{adm:62} is employed. -This leads to the following set of evolved variables: -\todo{continue editing here} +The evolved variables are the conformal factor $\Phi$, the conformal +3-metric $\tilde{gamma}_{ij}$, the trace $K$ of the extrinsic curvature, +the trace free extrinsic curvature $A_{ij}$ and the conformal connection +functions $\tilde{\Gamma}^i$. These are defined in terms of the +standard ADM 4-metric $g_{ij}$, 3-metric $\gamma{ij}$, and extrinsic +curvature $K_{ij}$ by + \begin{eqnarray} - \phi & := & \log \left[ \frac{1}{12} \det \gamma_{ij} \right] + \phi & := & \log \left[ \frac{1}{12} \det \gamma_{ij} \right]\,, \\ - \tilde\gamma_{ij} & := & e^{-4\phi}\; \gamma_{ij} + \tilde\gamma_{ij} & := & e^{-4\phi}\; \gamma_{ij}\,, \\ - K & := & g^{ij} K_{ij} + K & := & g^{ij} K_{ij}\,, \\ - \tilde A_{ij} & := & e^{-4\phi} \left[ K_{ij} - \frac{1}{3} g_{ij} K + \tilde A_{ij} & := & e^{-4\phi} \left[ K_{ij} - \frac{1}{3} g_{ij} K\,, \right] \\ \tilde\Gamma^i & := & \tilde\gamma^{jk} \tilde\Gamma^i_{jk} . \end{eqnarray} -Our exact evolution equations are as described by Eqs.~(3) to (10) of -\cite{ES-Brown2007b}, which we list here for completeness: + +The evolution equations are then: \begin{widetext} \begin{eqnarray} \partial_0 \alpha & = & -\alpha^2 f(\alpha, \phi, x^\mu) (K - @@ -661,13 +669,13 @@ variables are lapse $\alpha$, shift $\beta^i$, and a quantity $B^i$ related to the time derivative of the shift. The gauge parameters $f$, $G$, $H$, and $\eta$ are determined by our choice of a $1+\log$ -slicing: +\cite{alcubierre:03a} slicing: \begin{eqnarray} f(\alpha,\phi,x^\mu) & := & 2/\alpha \\ K_0(x^\mu) & := & 0 \end{eqnarray} -and $\Gamma$-driver shift condition: +and $\Gamma$-driver shift condition \cite{alcubierre:03a}: \begin{eqnarray} G(\alpha,\phi,x^\mu) & := & (3/4)\, \alpha^{-2} \\

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 37)
by cott＠tapir.caltech.edu 26 Mar '11

26 Mar '11

User: cott Date: 2011/03/26 10:14 AM Added: / widetext.sty /local_bibtex/ ott_references.bib Modified: / ET.tex Log: * bunch of changes; copied in some text from another paper that needs massaging File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +282 -4 =================================================================== --- ET.tex 2011-03-22 15:00:14 UTC (rev 36) +++ ET.tex 2011-03-26 15:14:54 UTC (rev 37) @@ -16,6 +16,7 @@ \usepackage[hyphens]{url} \usepackage{wrapfig} \usepackage{multicol} +\usepackage{widetext} \usepackage[bookmarks, bookmarksopen, bookmarksnumbered]{hyperref} \usepackage[all]{hypcap} @@ -388,6 +389,7 @@ supercomputers to run the same simulation there. \subsection{Kranc\pages{1 Ian}} +\label{sec:kranc} Kranc\cite{Husa:2004ip,kranc04,krancweb} is a Mathematica application which converts a high-level continuum description of a PDE into a highly optimised module for @@ -542,13 +544,289 @@ the \codename{TwoPunctures} module can also be used to construct neutron star black hole binary initial data, when being coupled with \codename{TOVSolver}. -\subsection{Evolution Methods\pages{4 Christian}} +\subsection{Spacetime Curvature and Hydrodynamics Evolution} +\todo{Christian in charge} -\paragraph{Spacetime} +In the following, we assume that the reader is familiar with the +basics of numerical relativity and GR hydrodynamics. Detailed +introductions to numerical relativity have recently been given by +Alcubierre~\cite{alcubierre:08} and Baumgarte \& Shapiro~\cite{baumgarte:10}. +GR hydrodynamics has been reviewed by Font~\cite{font:08}. -\paragraph{Relativistic Matter} +\subsubsection{Spacetime Curvature Evolution} The Einstein Toolkit +curvature evolution code \codename{McLachlan}~\cite{brown:09} is +auto-generated from tensor equations via \codename{Kranc} +(Sec.~\ref{sec:kranc}). It implements the Einstein equations in a +$3+1$ split as a Cauchy initial boundary value problem +\cite{york:79}. For this, the Baumgarte-Shapiro-Shibata-Nakamura +(BSSN) conformal-tracefree reformulation +\cite{shibata:95,baumgarte:95,alcubierre:00} of the original +Arnowitt-Deser-Misner formalism~\cite{adm:62} is employed. +This leads to the following set of evolved variables: +\todo{continue editing here} + +\begin{eqnarray} + \phi & := & \log \left[ \frac{1}{12} \det \gamma_{ij} \right] + \\ + \tilde\gamma_{ij} & := & e^{-4\phi}\; \gamma_{ij} + \\ + K & := & g^{ij} K_{ij} + \\ + \tilde A_{ij} & := & e^{-4\phi} \left[ K_{ij} - \frac{1}{3} g_{ij} K + \right] + \\ + \tilde\Gamma^i & := & \tilde\gamma^{jk} \tilde\Gamma^i_{jk} . +\end{eqnarray} +Our exact evolution equations are as described by Eqs.~(3) to (10) of +\cite{ES-Brown2007b}, which we list here for completeness: +\begin{widetext} +\begin{eqnarray} + \partial_0 \alpha & = & -\alpha^2 f(\alpha, \phi, x^\mu) (K - + K_0(x^\mu)) + \\ + \partial_0 K & = & -e^{-4\phi} \left[ \tilde{D}^i \tilde{D}_i \alpha + + 2 \partial_i \phi \cdot \tilde{D}^i \alpha \right] + \alpha + \left( \tilde{A}^{ij} \tilde{A}_{ij} + \frac{1}{3} K^2 \right) - \alpha S + \\ + \partial_0 \beta^i & = & \alpha^2 G(\alpha,\phi,x^\mu) B^i + \\ + \partial_0 B^i & = & e^{-4\phi} H(\alpha,\phi,x^\mu) + \partial_0\tilde{\Gamma}^i - \eta^i(B^i,\alpha,x^\mu) + \\ + \partial_0 \phi & = & -\frac{\alpha}{6}\, K + + \frac{1}{6}\partial_k\beta^k + \\ + \partial_0 \tilde{\gamma}_{ij} & = & -2\alpha\tilde{A}_{ij} + + 2\tilde{\gamma}_{k(i}\partial_{j)}\beta^k + - \frac{2}{3}\tilde{\gamma}_{ij}\partial_k\beta^k + \\ + \partial_0 \tilde{A}_{ij} & = & e^{-4\phi}\left[ + \alpha\tilde{R}_{ij} + \alpha R^\phi_{ij} - \tilde{D}_i\tilde{D}_j\alpha + + 4\partial_{(i}\phi\cdot\tilde{D}_{j)}\alpha\right]^{TF} + \nonumber\\ + & & {} + \alpha K\tilde{A}_{ij} - 2\alpha\tilde{A}_{ik}\tilde{A}^k_{\; j} + + 2\tilde{A}_{k(i}\partial_{j)}\beta^k + - \frac{2}{3}\tilde{A}_{ij}\partial_k\beta^k + - \alpha e^{-4\phi} \hat{S}_{ij} + \\ + \partial_0\tilde{\Gamma}^i & = & + \tilde{\gamma}^{kl}\partial_k\partial_l\beta^i + + \frac{1}{3} \tilde{\gamma}^{ij}\partial_j\partial_k\beta^k + + \partial_k\tilde{\gamma}^{kj} \cdot \partial_j\beta^i + - \frac{2}{3}\partial_k\tilde{\gamma}^{ki} \cdot \partial_j\beta^j + \nonumber\\ + & & {} - 2\tilde{A}^{ij}\partial_j\alpha + + 2\alpha\left[ (m-1)\partial_k\tilde{A}^{ki} - \frac{2m}{3}\tilde{D}^i K + + m(\tilde{\Gamma}^i_{\; kl}\tilde{A}^{kl} + 6\tilde{A}^{ij}\partial_j\phi) + \right] - S^i +\end{eqnarray} +\end{widetext} +with the momentum constraint damping constant set to $m=1$. The stress +energy tensor $T_{\mu\nu}$ is incorporated via the projections +\begin{eqnarray} + \rho & := & \frac{1}{\alpha^2} \left( T_{00} - 2 \beta^i T_{0i} + + \beta^i \beta^j T^{ij} \right) + \\ + S & := & g^{ij} T_{ij} + \\ + S_i & := & - \frac{1}{\alpha} \left( T_{0i} - \beta^j T_{ij} \right) . +\end{eqnarray} +We have introduced the notation $\partial_0 = \partial_t - +\beta^j\partial_j$. All quantities with a tilde $\tilde{~}$ refer to +the conformal 3-metric $\tilde{\gamma}_{ij}$, which is used to +raise and lower indices. In particular, $\tilde{D}_i$ and +$\tilde{\Gamma}^k_{ij}$ refer to the covariant derivative and the +Christoffel symbols with respect to $\tilde{\gamma}_{ij}$. The +expression $[ \cdots ]^{TF}$ denotes the trace-free part of the +expression inside the parentheses, and we define the Ricci tensor +contributions +\begin{widetext} +\begin{eqnarray} +\tilde{R}_{ij} + &=& -\frac{1}{2} \tilde{\gamma}^{kl}\partial_k\partial_l\tilde{\gamma}_{ij} + + \tilde{\gamma}_{k(i}\partial_{j)}\tilde{\Gamma}^k + - \tilde{\Gamma}_{(ij)k}\partial_l\tilde{\gamma}^{lk} + + \tilde{\gamma}^{ls}\left( 2\tilde{\Gamma}^k_{\; l(i}\tilde{\Gamma}_{j)ks} + + \tilde{\Gamma}^k_{\; is}\tilde{\Gamma}_{klj} \right) +\\ +R^\phi_{ij} &=& -2\tilde{D}_i\tilde{D}_j\phi + - 2\tilde{\gamma}_{ij} \tilde{D}^k\tilde{D}_k\phi + + 4\tilde{D}_i\phi\, \tilde{D}_j\phi + - 4\tilde{\gamma}_{ij}\tilde{D}^k\phi\, \tilde{D}_k\phi . +\end{eqnarray} +\end{widetext} +This is a so-called $\phi$-variant of BSSN. The evolved gauge +variables are lapse $\alpha$, shift $\beta^i$, and a quantity $B^i$ +related to the time derivative of the shift. The gauge parameters $f$, +$G$, $H$, and $\eta$ are determined by our choice of a $1+\log$ +slicing: +\begin{eqnarray} + f(\alpha,\phi,x^\mu) & := & 2/\alpha + \\ + K_0(x^\mu) & := & 0 +\end{eqnarray} +and $\Gamma$-driver shift condition: +\begin{eqnarray} + G(\alpha,\phi,x^\mu) & := & (3/4)\, \alpha^{-2} + \\ + H(\alpha,\phi,x^\mu) & := & \exp\{4\phi\} + \\\label{eq:eta} + \eta(B^i,\alpha,x^\mu) & := & (1/2)\, B^i q(r) . +\end{eqnarray} +The expression $q(r)$ attenuates the $\Gamma$-driver depending on the +radius as described below. + +The $\Gamma$-driver shift condition is symmetry-seeking, +driving the shift $\beta^i$ to a state that renders the conformal +connection functions $\tilde\Gamma^i$ +stationary. Of course, such a stationary state cannot be achieved +while the metric is evolving, but in a stationary spacetime the time +evolution of the shift +$\beta^i$ and thus that of the spatial coordinates $x^i$ will be exponentially +damped. This damping time scale is set by the gauge parameter $\eta$ +(see Eq.~\ref{eq:eta}) which has dimension $1/T$ (inverse time). +As described, e.g., in \cite{Muller:2009jx, ES-Schnetter2010a}, this +time scale may need to be adapted in different regions of the domain +to avoid spurious high-frequency behavior in regions that otherwise +evolve only very slowly, e.g., far away from the source. + +Here we use the simple damping mechanism described in Eq.~(12) of +\cite{ES-Schnetter2010a}, which is defined as +\begin{eqnarray} + \label{eq:varying-simple} + q(r) & := & \left\{ + \begin{array}{llll} + 1 & \mathrm{for} & r \le R & \textrm{(near the origin)} + \\ + R/r & \mathrm{for} & r \ge R & \textrm{(far away)} + \end{array} + \right. +\end{eqnarray} +with a constant $R$ defining the transition radius between the +interior, where $q\approx1$, and the exterior, where $q$ falls off as +$1/r$. Eq.~\ref{eq:eta} describes how $q$ appears in the gauge +parameters. In this paper we use $R=250\,M_\odot$ ($R = +369.2\,\mathrm{km}$). + +We implement the above BSSN equations and gauge conditions in the +{\tt McLachlan} code \cite{ES-Brown2007b, ES-mclachlanweb} which is +freely available as part of the {\tt EinsteinToolkit}. {\tt McLachlan} is +auto-generated from the definition of the variables and equations in the +{\tt Mathematica} format by the {\tt Kranc} code generator \cite{kranc04, + Husa:2004ip, krancweb}. {\tt Kranc} is a suite of {\tt Mathematica} packages +comprising a computer algebra toolbox for numerical relativists. {\tt Kranc} +can be used as a ``rapid prototyping'' system for physicists or +mathematicians handling complex systems of partial differential +equations, and through integration into the {\tt Cactus} framework one can +also produce efficient production codes. + +We use fourth-order accurate finite differencing for the spacetime +variables and add a fifth-order Kreiss-Oliger dissipation term to +remove high frequency noise. We use a fourth-order Runge-Kutta time +integrator for all evolved variables. + +\subsubsection{Initial Conditions} + +We set up our initial condition from the ADM variables $g_{ij}$, +$K_{ij}$, lapse $\alpha$, and shift $\beta^i$, as provided by the +initial data discussed in Sec.~\ref{sec:initial_models}. From these we +calculate the BSSN quantities via their definition, setting $B^i=0$, +and using cubic extrapolation for $\tilde\Gamma^i$ at the outer +boundary. This extrapolation is necessary since the $\tilde\Gamma^i$ are +calculated from derivatives of the metric, and one cannot use centered +finite differencing stencils near the outer boundary. We assume that +one could instead also use one-sided derivatives to calculate +$\tilde\Gamma^i$ on the boundary. + +The extrapolation stencils distinguish between points on the faces, +edges, and corners of the grid. Points on the faces are extrapolated +via stencils perpendicular to that face, while points on the edges and +corners are extrapolated with stencils aligned with the average of the +normals of the adjoining faces. For example, points on the $(+x,+y)$ +edge are extrapolated in the $(1,1,0)$ direction, while points in the +$(+x,+y+z)$ corner are extrapolated in the $(1,1,1)$ direction. Since +several layers of boundary points have to be filled for higher order +schemes (e.g., three layers for a fourth order scheme), we proceed +outwards starting from the innermost layer. Each subsequent layer is +then defined via the points in the interior and the previously +calculated layers. + +\subsubsection{Boundary Conditions} + +During time evolution, we apply a Sommerfeld-type radiative boundary +condition to all components of the evolved BSSN variables as described +in \cite{Alcubierre2000}. The main feature of this boundary condition +is that it assumes approximate spherical symmetry of the solution, +while applying the actual boundary condition on the boundary of a +cubic grid where the face normals are not aligned with the radial +direction. This boundary condition defines the right hand side +of the BSSN state vector on the outer boundary, which is then +integrated in time as well, so that the boundary and interior are +calculated with the same order of accuracy. + +The main part of the boundary condition assumes that we have an +outgoing radial wave with some speed $v_0$: +\begin{eqnarray} + X & = & X_0 + \frac{u(r - v_0 t)}{r} +\end{eqnarray} +where $X$ is any of the tensor components of evolved variables, $X_0$ +the value at infinity, and $u$ a spherically symmetric perturbation. +Both $X_0$ and $v_0$ depend on the particular variable and have to be +specified. This implies the following differential equation: +\begin{eqnarray} + \partial_t X & = & - v^i \partial_i X - v_0\, \frac{X - X_0}{r}\,, +\end{eqnarray} +where $v^i = v_0\, x^i/r$. The spatial derivatives $\partial_i$ are +evaluated using centered finite differencing where possible, and +one-sided finite differencing elsewhere. We use second order stencils +in our implementation. + +In addition to this main part, we also account for those parts of the +solution that do not behave as a pure wave, e.g., Coulomb type terms +caused by infall of the coordinate lines. We assume that these parts +decay with a certain power $p$ of the radius. We implement this by +considering the radial derivative of the source term above, and +extrapolating according to this power-law decay. + +Given a source term $(\partial_t X)$, we define the corrected source +term $(\partial_t X)^*$ via +\begin{eqnarray} + (\partial_t X)^* & = & (\partial_t X) + \left( \frac{r}{r - n^i + \partial_i r} \right)^p\; n^i \partial_i (\partial_t X)\,, +\end{eqnarray} +where $n^i$ is the normal vector of the corresponding boundary face. +The spatial derivatives $\partial_i$ are evaluated by comparing +neighbouring grid points, corresponding to a second-order stencil +evaluated in the middle between the two neighbouring grid points. We +assume a second-order decay, i.e., we choose $p=2$. + +As with the initial conditions above, this boundary condition is +evaluated on several layers of grid points, starting from the +innermost layer. Both the extrapolation and radiative boundary +condition algorithms are implemented in the publicly available +\texttt{NewRad} component of the Einstein Toolkit. + +This boundary condition is only a coarse approximation of the actual +decay behavior of the BSSN state vector, and it does not capture the +correct behavior of the evolved variables. However, we observe that +this boundary condition leads to stable evolutions if applied +sufficiently far from the source. Errors introduced at the boundary +(both errors in the geometry and constraint violations) propagate +inwards with the speed of light \cite{ES-Brown2007b}. Gauge changes +introduced by the boundary condition, which are physically not +observable, propagate faster, with a speed up to $\sqrt{2}$ for our +gauge conditions. + + + + + +\subsubsection{Hydrodynamics: \codename{GRHydro}} + + + \subsection{Analysis\pages{4 Tanja}} Any simulated system may have many applicable quantities for analysis which @@ -696,6 +974,6 @@ \bibliographystyle{amsplain-url} -\bibliography{manifest/einsteintoolkit} +\bibliography{manifest/einsteintoolkit,local_bibtex/ott_references} \end{document} File [added]: widetext.sty Delta lines: +86 -0 =================================================================== --- widetext.sty (rev 0) +++ widetext.sty 2011-03-26 15:14:54 UTC (rev 37) @@ -0,0 +1,86 @@ +\NeedsTeXFormat{LaTeX2e} +\ProvidesPackage{widetext} + +%% Mimics the widetext environment of revtex4 for any other class package +%% Eg: article.cls +%% +%% Compiled by: Anjishnu Sarkar +%% +%% Advantages: +%% *) Supports float (eg: figure) in two column format (Advantage over +%% multicol package) +%% *) One and twocolumn exist on the same page +%% *) Flow of text shown via rule +%% *) Equal height of text when in two column format +%% +%% Acknowledgment(s): +%% 1. Instead of re-inventing the wheel, two packages (flushend, cuted) of +%% the sttools bundle are used. The sttools bundle is available from CTAN. +%% Lisence of these packages rests with their corresponding author. +%% Any bug/problem with flushend and cuted should be forwarded to their +%% corresponding package authors. +%% 2. The idea of the rule came from the following latex community website +%% http://www.latex-community.org/forum/viewtopic.php?f=5&t=2770 +%% +%% This package just defines the widetext environment and the rules. +%% +%% Usage: +%% \documentclass[a4paper,12pt,twocolumn]{article} +%% \usepackage{widetext} +%% +%% \begin{document} +%% +%% Some text in twocolumn +%% +%% \begin{widetext} +%% Text in onecolumn format. +%% \end{widetext} +%% +%% Some more text in twocolumn +%% +%% \end{document} +%%%%%%%%%%%%%%%%%%%% + +%% Package required for equal height while in 2 columns format +\IfFileExists{flushend.sty} + {\RequirePackage{flushend}} + {\typeout{} + \typeout{Package widetext error: Install the flushend package which is + a part of sttools bundle. Available from CTAN.} + \typeout{} + \stop + } + +%% Package required for onecolumn and twocolumn to exist on the same page. +%% and also required for widetext environment. +\IfFileExists{cuted.sty} + {\RequirePackage{cuted}} + {\typeout{} + \typeout{Package widetext error: Install the cuted package which is + a part of sttools bundle. Available from CTAN.} + \typeout{} + \stop + } + + +\newlength\@parindent +\setlength\@parindent{\parindent} + +\if@twocolumn + \newenvironment{widetext} + {% + \begin{strip} + \rule{\dimexpr(0.5\textwidth-0.5\columnsep-0.4pt)}{0.4pt}% + \rule{0.4pt}{6pt} + \par %\vspace{6pt} + \parindent \@parindent + }% + {% + \par + \hfill\rule[-6pt]{0.4pt}{6.4pt}% + \rule{\dimexpr(0.5\textwidth-0.5\columnsep-1pt)}{0.4pt} + \end{strip} + } +\else + \newenvironment{widetext}{}{} +\fi Directory: /local_bibtex/ ========================= File [added]: ott_references.bib Delta lines: +104 -0 =================================================================== --- local_bibtex/ott_references.bib (rev 0) +++ local_bibtex/ott_references.bib 2011-03-26 15:14:54 UTC (rev 37) @@ -0,0 +1,104 @@ +@incollection{york:79, + author = "York, James W.", + title = "Kinematics and Dynamics of General Relativity", + pages = "83--126", + editor = "Larry L. Smarr", + booktitle = "Sources of Gravitational Radiation", + publisher = "Cambridge University Press", + address = "Cambridge, UK", + year = 1979, + snote = "Proceedings of the Battelle Seattle Workshop, + 24 July -- 4 August, 1978", +} + +@Book{adm:62, +author = {R.~Arnowitt and S.~Deser and C.~Misner}, +title = {Dynamics of General Relativity, in "Gravitation: An Introduction to Current Research"}, +publisher = {Wiley, New York}, +year = {1962}, +} + +@article{shibata:95, + key = {Shibata95}, + author = {Masaru Shibata and Takashi Nakamura}, + journal = {Phys. Rev. D}, + title = {Evolution of three-dimensional gravitational waves: + {H}armonic slicing case}, + volume = {52}, + year = {1995}, + pages = {5428} +} + +@article{baumgarte:95, + key = {Baumgarte99}, + author = {Thomas W. Baumgarte and Stuart L. Shapiro}, + title = {On the numerical integration of {E}instein's field + equations}, + journal = {Phys. Rev. D}, + year = 1999, + volume = 59, + pages = 024007, +} + +@article{alcubierre:00, + author = {M. Alcubierre and B. Br\"{u}gmann and T. Dramlitsch and J. A. Font + and Philippos Papadopoulos and E. Seidel and N. Stergioulas and R. Takahashi}, + title = {Towards a stable numerical evolution of strongly gravitating + systems in general relativity: The conformal treatments}, + journal = {Phys. Rev. D}, + volume = {62}, + year = 2000, + pages = 044034, +} + + +@article{alcubierre:03a, + author = {Miguel Alcubierre and Bernd Br\"ugmann and Peter Diener and + Michael Koppitz and Denis Pollney and Edward Seidel and Ryoji Takahashi}, + title = "Gauge conditions for long-term numerical black hole + evolutions without excision", + journal = {Phys. Rev. D}, + volume = {67}, + pages = {084023}, + year = 2003, +} + +@BOOK{alcubierre:08, + author = {{Alcubierre}, M.}, + title = "{Introduction to 3+1 Numerical Relativity}", +booktitle = {Introduction to 3+1 Numerical Relativity}, + year = 2008, + editor = "{Alcubierre, M.}", +publisher = {Oxford University Press}, +} + +@BOOK{baumgarte:10, + author = {{Baumgarte}, T.~W. and {Shapiro}, S.~L.}, + title = "{Numerical Relativity: Solving Einstein's Equations on the Computer}", + year = 2010, + publisher = "Cambridge University Press", +} + + +@ARTICLE{font:08, + author = {{Font}, J.~A.}, + title = "{Numerical Hydrodynamics and Magnetohydrodynamics in General Relativity}", + journal = {Liv. Rev. Rel.}, + keywords = {Hydrodynamics, Relativistic hydrodynamics, Numerical relativity, Magnetohydrodynamics}, + year = 2008, + month = sep, + volume = 11, + pages = {7}, +} + +@Article{brown:09, + author = {David Brown and Peter Diener and Olivier Sarbach and + Erik Schnetter and Manuel Tiglio}, + title = {Turduckening black holes: an analytical and + computational study}, + journal = {Phys. Rev. D}, + year = 2009, + volume = 79, + pages = 044023, +} +

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[svn:einsteintoolkit] Paper_EinsteinToolkit_LR/ (Rev. 1)
by knarf＠cct.lsu.edu 23 Mar '11

23 Mar '11

User: knarf Date: 2011/03/23 01:00 PM Added: / test Log: test commit messages File Changes: Directory: / ============ File [added]: test Delta lines: +0 -0 Added: test

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[svn:einsteintoolkit] Paper_EinsteinToolkit_LR/ (Rev. 2)
by knarf＠cct.lsu.edu 23 Mar '11

23 Mar '11

User: knarf Date: 2011/03/23 12:22 PM Removed: / test Log: test commit messages File Changes: Directory: / ============ File [removed]: test Delta lines: +0 -0 Deleted: test

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/figures/ (Rev. 36)
by knarf＠cct.lsu.edu 22 Mar '11

22 Mar '11

User: knarf Date: 2011/03/22 10:00 AM Added: /figures/ Log: add figures directory

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 35)
by knarf＠cct.lsu.edu 22 Mar '11

22 Mar '11

User: knarf Date: 2011/03/22 09:55 AM Modified: / ET.tex Log: add comments with names and length to sections File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +37 -54 =================================================================== --- ET.tex 2011-03-14 15:08:29 UTC (rev 34) +++ ET.tex 2011-03-22 14:55:47 UTC (rev 35) @@ -29,7 +29,9 @@ \def\gt#1{Georgia Tech#1 (GaTech#1)\gdef\gt{GaTech}} \newcommand{\codename}[1]{\texttt{#1}} -\newcommand{\todo}[1]{{\color{blue}$\blacksquare$~\textsf{[TODO: #1]}}} +\newcommand{\todo}[1]{{\color{red}$\blacksquare$~\textsf{[TODO: #1]}}} +\newcommand{\comment}[1]{{\color{blue}$\blacksquare$~\textsf{[Comment: #1]}}} +\newcommand{\pages}[1]{{\color{blue}$\blacksquare$~\textsf{[#1]}}} % Don't use tt font for urls \urlstyle{rm} @@ -69,19 +71,16 @@ -\thanks{{}$^{(1)}$ Department of Computer Science, - Louisiana State University, Baton Rouge, LA 70803, USA} +%\thanks{{}$^{(1)}$ Department of Computer Science, +% Louisiana State University, Baton Rouge, LA 70803, USA} +%\thanks{{}$^{(2)}$ Department of Physics \& Astronomy, +% Louisiana State University, Baton Rouge, LA 70803, USA} +%\thanks{{}$^{(3)}$ Center for Computation \& Technology, +% Louisiana State University, Baton Rouge, LA 70803, USA} +%\thanks{{}$^{(4)}$ Center for Computational Relativity \& Gravitation, +% School of Mathematical Sciences, +% Rochester Institute of Technology, Rochester, New York 14623, USA} -\thanks{{}$^{(2)}$ Department of Physics \& Astronomy, - Louisiana State University, Baton Rouge, LA 70803, USA} - -\thanks{{}$^{(3)}$ Center for Computation \& Technology, - Louisiana State University, Baton Rouge, LA 70803, USA} - -\thanks{{}$^{(4)}$ Center for Computational Relativity \& Gravitation, - School of Mathematical Sciences, - Rochester Institute of Technology, Rochester, New York 14623, USA} - % TODO: Already add a few affiliations which we know are going % to be used @@ -91,8 +90,11 @@ \maketitle +% We will remove this at the end, but we leave it in for ourselfes now +\tableofcontents -\section{Introduction} +\section{Introduction\pages{1 Frank}} +\comment{About 1 page} Scientific progress in the field of numerical relativity has always been closely tied with the availability and ease-of-use of enabling @@ -168,7 +170,7 @@ -\section{Requirements} +\section{Requirements\pages{2 Frank}} \subsection{Scientific} @@ -246,7 +248,7 @@ other areas of science and hereby providing an immediate application of their research. -\section{Design and Strategy for the Einstein Toolkit} +\section{Design and Strategy\pages{1 Frank}} The mechanisms for the development and support of the Einstein Toolkit are designed to be open, transparent and community driven. All the source code, @@ -274,10 +276,9 @@ Einstein Toolkit Maintainer, and is generally open for discussion on the users mailing list. -\section{Core Technologies} +\section{Core Technologies\pages{0.5 Frank}} -\subsection{Cactus Framework} -\todo{1/2 page Gab} +\subsection{Cactus Framework\pages{1 Gab}} The \textbf{Cactus Framework}~\cite{CS_cactus_web,CS_Goodale02a,CS_cactususersguide} is @@ -311,7 +312,7 @@ The Einstein Toolkit now collects the widely used parts of CactusEinstein, combined with contributions from the community. -\subsection{Adaptive Mesh Refinement} +\subsection{Adaptive Mesh Refinement\pages{1 Erik}} \todo{ES: add/check citations} \todo{ES: remove names} @@ -354,7 +355,7 @@ % E. Schnetter \todo{ES: do we want names here?} and is funded via several % NSF awards \todo{ES: list them somewhere}. -\subsection{Simulation Factory} +\subsection{Simulation Factory\pages{1 Erik/Michael}} It is unfortunate that today's supercomputers differ significantly in their hardware configuration, available software, directory structure, @@ -386,8 +387,7 @@ The exact same set of commands can be used on all other supported supercomputers to run the same simulation there. -\subsection{Kranc} -\todo{1/3 page Ian} +\subsection{Kranc\pages{1 Ian}} Kranc\cite{Husa:2004ip,kranc04,krancweb} is a Mathematica application which converts a high-level continuum description of a PDE into a highly optimised module for @@ -424,9 +424,9 @@ as well as the wave extraction thorn WeylScal4, are both generated using Kranc, and hence support all the above features. -\section{Components} +\section{Components\pages{0.5 Frank}} -\subsection{Base Modules} +\subsection{Base Modules\pages{4 Frank}} \label{sec:base_modules} Modular designs have proven to be essential for distributed development of complex software systems, and require the use of well defined interfaces. @@ -485,8 +485,7 @@ to the Faraday tensor and the unit normal of the foliation of spacetime $n^\mu$. -\subsection{Initial Data} -\todo{1/2 page Josh, Bruno} +\subsection{Initial Data\pages{4 Josh/Bruno}} The Einstein Toolkit contains many modules used to generate initial data for general relativistic simulations, including both vacuum and hydrodynamical configurations. @@ -543,16 +542,14 @@ the \codename{TwoPunctures} module can also be used to construct neutron star black hole binary initial data, when being coupled with \codename{TOVSolver}. -\subsection{Evolution Methods} -\todo{1/2 page Christian} +\subsection{Evolution Methods\pages{4 Christian}} \paragraph{Spacetime} \paragraph{Relativistic Matter} -\subsection{Analysis} -%\todo{1/2 page Tanja} +\subsection{Analysis\pages{4 Tanja}} Any simulated system may have many applicable quantities for analysis which are most efficiently calculated during evolution. The Einstein Toolkit @@ -589,8 +586,7 @@ Weyl scalars, as well as any other quantity, can be projected onto a basis of spin-weighted spherical harmonics using the \codename{Multipole} module. -\subsection{Relativity Tools} -\todo{1/2 page Peter} +\subsection{Relativity Tools\pages{3 Peter}} \paragraph{Black Hole Excision} @@ -621,8 +617,7 @@ -%\subsection{Infrastructure and Numerical Methods} -\subsection{Simulation Domain, Symmetries, Boundaries} +\subsection{Simulation Domain, Symmetries, Boundaries\pages{3 Roland?}} \paragraph{Domains and Coordinates.} The simulation domain is specified via the parameter file \todo{ES: @@ -671,36 +666,24 @@ -\section{Examples} -\todo{2 pages in total, 1 plot per paragraph, Frank coordinates} +\section{Examples\pages{0.5 Frank}} -\paragraph{Kerr-Schild} -\todo{1/2 page, Bruno} -Show stable Kerr-evolution. What is commonly shown for this nowadays, the -spectrum of the ringdown of a perturbation? +\subsection{Vacuum\pages{2 Bruno}} -\paragraph{BH-binary} -\todo{1/2 page, Peter} -Show binary merger and plot of waveform in either time or frequency domain. +\subsection{TOV\pages{2 Frank}} +Show stable TOV evolution -\paragraph{TOV+mEOS} -\todo{1/2 page, Frank} -Show stable TOV evolution, once with Polytropes and once with mEOS, -both including oscillation spectra - -\paragraph{Collapse} -\todo{1/2 page, Frank, Christian} +\subsection{Collapse\pages{2 Christian}} Show TOV collapse and BH formation -\section{Future Work} -\todo{Frank} +\section{Future Work\pages{1 Frank}} - MHD - massively parallel AMR - radiation transport - advanced wave extraction -\section*{Acknowledgments} +\section*{Acknowledgments\pages{0.5 All}} \todo{Frank, ADDME} The Einstein Toolkit is directly supported by the National Science Foundation under the grant numbers 0903973/0903782/0904015 (CIGR).

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[svn:einsteintoolkit] EOS_Omni/trunk/src/nuc_eos/ (Rev. 38)
by cott＠tapir.caltech.edu 20 Mar '11

20 Mar '11

User: cott Date: 2011/03/20 02:46 PM Modified: /trunk/src/nuc_eos/ nuc_eos.F90 Log: * improve error handling in nuc_eos a bit. File Changes: Directory: /trunk/src/nuc_eos/ ============================== File [modified]: nuc_eos.F90 Delta lines: +10 -5 =================================================================== --- trunk/src/nuc_eos/nuc_eos.F90 2011-02-07 05:36:36 UTC (rev 37) +++ trunk/src/nuc_eos/nuc_eos.F90 2011-03-20 19:46:09 UTC (rev 38) @@ -48,11 +48,13 @@ keyerrr = 0 if(xrho.gt.eos_rhomax) then - call CCTK_WARN(0, "nuc_eos: rho > rhomax") + keyerr = 103 + return endif if(xrho.lt.eos_rhomin) then - call CCTK_WARN (0, "nuc_eos: rho < rhomin") + keyerr = 104 + return endif if(xye.gt.eos_yemax) then @@ -228,7 +230,8 @@ keyerrr = 0 if(xrho.gt.eos_rhomax) then - call CCTK_WARN (0, "nuc_eos: rho > rhomax") + keyerr = 103 + return endif if(xrho.lt.eos_rhomin*1.126d0) then @@ -351,7 +354,8 @@ keyerrt = 0 if(xrho.gt.eos_rhomax) then - call CCTK_WARN (0, "nuc_eos: rho > rhomax") + keyerr = 103 + return endif if(xrho.lt.eos_rhomin*1.126d0) then @@ -430,7 +434,8 @@ keyerrt = 0 if(xrho.gt.eos_rhomax) then - call CCTK_WARN (0, "nuc_eos: rho > rhomax") + keyerr = 103 + return endif if(xrho.lt.eos_rhomin*1.126d0) then

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 34)
by schnetter＠cct.lsu.edu 14 Mar '11

14 Mar '11

User: eschnett Date: 2011/03/14 10:08 AM Modified: / ET.tex Log: Remove Schnetter's name from code description File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +10 -4 =================================================================== --- ET.tex 2011-03-07 15:53:14 UTC (rev 33) +++ ET.tex 2011-03-14 15:08:29 UTC (rev 34) @@ -289,7 +289,7 @@ formats. Generic interfaces are used, making it possible to use external packages and improved modules which are immediately available to its users. Cactus is involved in the NSF Blue Waters consortium -for petascale computing, has funding from NSF SDCI (PI Schnetter) to +for petascale computing, has funding from NSF SDCI to develop new application level tools for performance and correctness, as well as the current NSF XiRel award for scalable AMR\@. \S\ref{broader} describes the growing impact of Cactus in other @@ -313,6 +313,11 @@ \subsection{Adaptive Mesh Refinement} +\todo{ES: add/check citations} +\todo{ES: remove names} +\todo{ES: describe grants in acknowledgements, also in introduction, + but not in individual sections} + In Cactus, infrastructure capabilities such as memory management, parallelisation, time evolution, mesh refinement, and I/O are delegated to a set of special \emph{driver} components. This helps @@ -344,9 +349,10 @@ hours) were used via Carpet by more than a dozen research groups world-wide. To date, more than 90 peer-reviewed publication and more than 15 student theses are based on Carpet \todo{ES: update these numbers} -\cite{CarpetCode:web}. Carpet's continued development is overseen by -E. Schnetter \todo{ES: do we want names here?} and is funded via several -NSF awards \todo{ES: list them somewhere}. +\cite{CarpetCode:web}. +% Carpet's continued development is overseen by +% E. Schnetter \todo{ES: do we want names here?} and is funded via several +% NSF awards \todo{ES: list them somewhere}. \subsection{Simulation Factory}

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