[Commits] [svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 184)

[knarf at cct.lsu.edu]

User: knarf
Date: 2011/11/11 09:27 AM

Modified:
 /
  ET.tex

Log:
 some rewording from Dennis

File Changes:

Directory: /
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File [modified]: ET.tex
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--- ET.tex	2011-11-11 15:13:47 UTC (rev 183)
+++ ET.tex	2011-11-11 15:27:00 UTC (rev 184)
@@ -121,25 +121,22 @@
 %       to be used
     
 \begin{abstract}
-We describe the Einstein Toolkit, a community-driven, freely
-accessible computational infrastructure intended for use in numerical
-relativity, relativistic astrophysics, and other applications.  The
-Toolkit, developed by a collaboration involving researchers from
-several institutions around the world, combines a core set of
-components needed to simulate astrophysical objects including black
-holes, compact objects, and collapsing stars, as well as a full suite
-of analysis tools.  The Einstein Toolkit is based on the Cactus
-Framework for high-performance computing and the Carpet adaptive mesh
-refinement driver. It implements spacetime evolution via the BSSN
-evolution system and general-relativistic hydrodynamics in a
-finite-volume discretization. The toolkit is under continuous
-development and contains many new code components that have been
-publicly released for the first time and are described in this
-article.  We discuss the motivation behind the release of the toolkit,
-the philosophy underlying its development, and the goals of the
-project.  A summary of the implemented numerical techniques is
-included, as are results of numerical test covering a variety of
-sample astrophysical problems. 
+We describe the Einstein Toolkit, a community-driven, freely accessible
+computational infrastructure intended for use in numerical relativity,
+relativistic astrophysics, and other applications.  The Toolkit, developed by a
+collaboration involving researchers from several institutions around the world,
+combines a core set of components needed to simulate astrophysical objects such
+as black holes, compact objects, and collapsing stars, as well as a full suite
+of analysis tools.  The Einstein Toolkit is based on the Cactus Framework for
+high-performance computing and the Carpet adaptive mesh refinement driver.  It
+implements spacetime evolution via the BSSN evolution system and
+general-relativistic hydrodynamics in a finite-volume discretization. The
+toolkit is under continuous development and contains many new code components
+that have been publicly released for the first time and are described in this
+article.  We discuss the motivation behind the release of the toolkit, the
+philosophy underlying its development, and the goals of the project.  A summary
+of the implemented numerical techniques is included, as are results of
+numerical test covering a variety of sample astrophysical problems. 
 \end{abstract}
 
 \pacs{04.25.D-, 04.30.-w, 04.70.-s, 07.05.Tp, 95.75.Pq}
@@ -166,7 +163,7 @@
 advances for the next few years~\cite{Shibata:1999wm,Shibata:2002jb,
 Shibata:2003ga,Shibata:2005ss,Shibata:2006nm}, systems containing BHs proved 
 much more numerically intractable until 2005.  That year, computational 
-breakthroughs were made in using a generalized harmonic gauge (GHG) 
+breakthroughs were made using a generalized harmonic gauge (GHG) 
 \cite{Pretorius:2005gq} and then a ``moving puncture'' approach 
 \cite{Campanelli:2005dd, Baker:2005vv} in the BSSN 
 (Baumgarte-Shapiro-Shibata-Nakamura) formalism~\cite{Shibata:1995we,Baumgarte:1998te} 
@@ -199,7 +196,7 @@
 on fixed background spacetimes has been implemented in multi-dimensional
 settings since the mid-1990s, focusing on BH accretion processes and 
 relativistic jet production and evolution
-(see, e.g.,~\cite{Font:2008aa} for a review of the numerical formalism, 
+(see~\cite{Font:2008aa} for a review of the numerical formalism
 and~\cite{Hawley2009apss} for a review of work on disk and jet models). 
 GRMHD coupled with
 curvature evolution, on the other hand, which is crucial for modeling large-scale bulk
@@ -209,7 +206,7 @@
 stable curvature evolution systems discussed above as well as improved GRMHD
 algorithms~(see~\cite{Font:2008aa} for a review). 
 In addition to these developments, substantial progress has been made 
-in using physically motivated equations of state (EOS), 
+using physically motivated equations of state (EOS), 
 including tabulated versions (e.g.,~\cite{Pandharipande:1989hn,
 Douchin:2001sv,Akmal:1998cf}) and temperature-dependent models 
 (e.g.,~\cite{Shen:1998by,Shen:1998gq,Lattimer:1991nc}).  Some codes also 
@@ -228,27 +225,27 @@
 now include GRMHD (used widely for NS-NS mergers, and for BH-NS mergers 
 in~\cite{Chawla:2010sw}, and some include microphysical effects as well.  
 The groups that have reported simulations of NS-NS or BH-NS mergers include:
-\begin{description}
-\item[AEI/Sissa]:  BH-NS mergers using GRHD~\cite{Loffler:2006nu} and NS-NS 
+\begin{itemize}
+\item {\bf AEI/Sissa}:  BH-NS mergers using GRHD~\cite{Loffler:2006nu} and NS-NS 
 mergers using GRHD~\cite{Baiotti:2008ra,Baiotti:2009gk,Baiotti:2010xh,
 Baiotti:2011am,Rezzolla:2010fd} and GRMHD~\cite{Giacomazzo:2009mp,
 Giacomazzo:2010bx,Rezzolla:2011da}.
-\item[Caltech/Cornell]: A {\em pseudospectral}, GRHD code has been used 
+\item {\bf Caltech/Cornell}: A {\em pseudospectral}, GRHD code has been used 
 to simulate BH-NS mergers~\cite{Duez:2008rb,Duez:2009yy,Foucart:2010eq}.
-\item[Illinois]: BH-NS mergers using GRHD~\cite{Etienne:2007jg,Etienne:2008re} 
+\item {\bf Illinois}: BH-NS mergers using GRHD~\cite{Etienne:2007jg,Etienne:2008re} 
 and NS-NS mergers using GRMHD~\cite{Liu:2008xy}.
-\item[Jena]: NS-NS mergers using GRHD~\cite{Thierfelder:2011yi}.
-\item[LSU/BYU/LIU]: BH-NS mergers using GRMHD~\cite{Chawla:2010sw} and 
+\item {\bf Jena}: NS-NS mergers using GRHD~\cite{Thierfelder:2011yi}.
+\item {\bf LSU/BYU/LIU}: BH-NS mergers using GRMHD~\cite{Chawla:2010sw} and 
 NS-NS mergers using GRHD~\cite{Anderson:2007kz} 
 and GRMHD~\cite{Anderson:2008zp}.
-\item[Princeton]:  BH-NS mergers using GRHD~\cite{Stephens:2011as}.
-\item[Tokyo/Kyoto]:  BH-NS mergers using GRHD~\cite{Shibata:2006bs,
+\item {\bf Princeton}:  BH-NS mergers using GRHD~\cite{Stephens:2011as}.
+\item {\bf Tokyo/Kyoto}:  BH-NS mergers using GRHD~\cite{Shibata:2006bs,
 Shibata:2006ks,Shibata:2007zm,Yamamoto:2008js,Shibata:2009cn,
 Kyutoku:2010zd,Shibata:2010zz} and NS-NS mergers using GRHD 
 \cite{Yamamoto:2008js,Kiuchi:2009jt, Kiuchi:2010ze,Hotokezaka:2011dh}, 
 most recently with the inclusion of neutrino cooling~\cite{Sekiguchi:2011zd}.
 \todo{Check for updates to list before submission!}
-\end{description}
+\end{itemize}
 
 In addition to studying binary mergers, numerical relativity is a necessary 
 element for understanding stellar collapse and dynamical instabilities 
@@ -261,31 +258,30 @@
 rapidly rotating polytropic NS models~\cite{Shibata:1999yx,Baiotti:2006wn,
 Manca:2007ca}.
  
-In parallel to the advances in both our physical understanding of 
+Simultanious to the advances in both our physical understanding of 
 relativistic dynamics and the numerical techniques required to study them,
 a set of computational tools and libraries has been developed with the
-aim of providing a computational core that can enable the new science,
+aim of providing a computational core that can enable new science,
 broaden the community, facilitate interdisciplinary research and take
 advantage of emerging petascale computers and advanced cyberinfrastructure:
-the {\tt Cactus} computational toolkit~\cite{Cactuscode:web}. While it was 
-developed in large part by
-computer scientists, its development was driven by the direct input from other
-fields, especially numerical relativity, succeeding in applying expertise in
-computer science directly to problems in numerical relativity.
+the Cactus computational toolkit~\cite{Cactuscode:web}. While it was 
+developed in large part by computer scientists, its development was driven by
+direct input from other fields, especially numerical relativity, and has
+succeeded in applying expertise in computer science directly to problems in
+numerical relativity.
 
 This success prompted usage of the {\tt Cactus} computational toolkit in other
 areas, such as ocean forecast models~\cite{Djikstra2005} and chemical reaction 
 simulations~\cite{Camarda2001}. At the same time, the growing
 number of results in numerical relativity increased the need for commonly
 available utilities such as comparison and analysis tools, typically
-those specifically designed for astrophysical problems. Including them 
-within the
-{\tt Cactus} computational toolkit was not felt to fit within its rapidly 
-expanding scope. This triggered
-the creation of the Einstein Toolkit~\cite{EinsteinToolkit:web}. While large 
-parts of the Einstein toolkit
-presently do make use of the {\tt Cactus} toolkit, this is not an requirement at all,
-and other contributions are welcome and have been accepted.
+those specifically designed for astrophysical problems. Including them within
+the {\tt Cactus} computational toolkit was not felt to fit within its rapidly
+expanding scope. This triggered the creation of the Einstein
+Toolkit~\cite{EinsteinToolkit:web}. Large parts of the Einstein toolkit
+presently do make use of the {\tt Cactus} toolkit, but this is not an
+requirement, and other contributions are welcome, encouraged and have been
+accepted in the past.
 
 \section{Requirements}