[Commits] [svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 233)

[knarf at cct.lsu.edu]

User: knarf
Date: 2011/11/14 11:14 AM

Modified:
 /
  ET.tex

Log:
 spellcheck

File Changes:

Directory: /
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File [modified]: ET.tex
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--- ET.tex	2011-11-14 17:03:30 UTC (rev 232)
+++ ET.tex	2011-11-14 17:14:47 UTC (rev 233)
@@ -293,7 +293,7 @@
 attacked directly with fewer potential infrastructure problems, one
 of the goals of the Einstein Toolkit.
 
-While the Einstein Toolkit does have a large group of users, many of themdo not directly collaborate on science problems, and some compete.
+While the Einstein Toolkit does have a large group of users, many of them do not directly collaborate on science problems, and some compete.
 However, all groups agree that sharing the development
 of the underlying infrastructure is mutually beneficial for every group and the wider community as well.
 This is achieved by lifting  off the research groups' shoulders much of the
@@ -347,7 +347,7 @@
 starting with code generation all to way to archiving of simulation
 results: (i) the {\tt Cactus} framework ``flesh'' provides the underlying
 infrastructure to build complex simulation codes out of independently
-developed modules and facillates communication between these modules. (ii) the
+developed modules and facilities communication between these modules. (ii) the
 adaptive mesh refinement driver, {\tt Carpet}, is build on top of {\tt Cactus}
 and provides problem independent adaptive mesh refinement support for
 simulations that need to resolve physics on length scales differing by many
@@ -355,7 +355,7 @@
 internal details of the mesh refinement driver. (iii) {\tt Kranc}, which generates
 code in a computer language from a high-level description in Mathematica and
 (iv) the Simulation Factory, which provides a uniform, high-level interface to
-common operations, such submisson and restart of jobs, for a large number of
+common operations, such as submission and restart of jobs, for a large number of
 compute clusters.
 
 \subsection{Cactus Framework}
@@ -395,13 +395,13 @@
 group continues to be comprised of numerical relativists. 
 It is not surprising therefore, that one of the science modules provided in
 the Einstein Toolkit is a set of state of the art modules to simulate binary
-black hole mergers. All modules to simulate and analyse the data are provided
+black hole mergers. All modules to simulate and analyze the data are provided
 out of the box. This set of modules also provides a way of testing the
 Einstein Toolkit modules in a production type simulation rather than synthetic
 test cases. Some of these modules have been developed specifically for the
 Einstein Toolkit while others are modules used in previous publications and
 have been contributed to the toolkit. In these cases the Einstein Toolkit
-provides documenation and best practise guidelines for the contributed modules.
+provides documentation and best practice guidelines for the contributed modules.
 
 \subsection{Adaptive Mesh Refinement}
 
@@ -485,7 +485,7 @@
     This shows the time required per grid point,
     where smaller numbers are
     better (the ideal scaling is a horizontal line). This
-    demonstrates excellect scalability to up to more than 10,000
+    demonstrates excellent scalability to up to more than 10,000
     cores. Including hydrodynamics approximately doubles
     calculation times without negatively influencing scalability.}
   \label{fig:weak-scaling}
@@ -509,7 +509,7 @@
 
 Today's supercomputers differ significantly in
 their hardware configuration, available software, directory structure,
-queueing system, queuing policy, and many other user-visible
+queuing system, queuing policy, and many other user-visible
 properties. In addition, the system architectures and user interfaces
 offered by supercomputers are very different from those offered by
 laptops or workstations. This makes performing large,
@@ -988,7 +988,7 @@
 it to extend to spatial infinity.  Within each of the nested sub-domains, 
 fields are decomposed into Chebyshev modes radially and into spherical harmonics 
 in the angular directions, with elliptic equation solving reduced to a matrix 
-problem.  The nested sub-domains ineen not be perfectly spherical, and 
+problem.  The nested sub-domains need not be perfectly spherical, and 
 indeed one may modify the outer boundaries of each to cover any convex shape.  
 For NSs, this allows one to map the surface of a particular sub-domain 
 to the NS surface, minimizing Gibbs error there.  For BHs, excision 
@@ -1873,7 +1873,7 @@
 on a Schwarzschild background or the calculation of the Weyl scalar $\Psi_4$.
 
 The module \codename{Extract} uses the Moncrief formalism~\cite{
-Moncrief:1974am} to extract gauge-invariant wavefunctions $Q_{\ell m}^\times$ and $Q_{\ell
+Moncrief:1974am} to extract gauge-invariant wave functions $Q_{\ell m}^\times$ and $Q_{\ell
 m}^+$ given spherical surfaces of constant coordinate
 radius. The spatial metric is expressed as a perturbation on
 Schwarzschild and expanded into a tensor basis of
@@ -1951,8 +1951,8 @@
 While the waveforms generated by \codename{Extract} are 
 already decomposed on a convenient basis to separate modes, the 
 complex quantity $\Psi_4$ is provided by \codename{WeylScal4} as 
-a complex gridfunction.  For this quantity, and any other real or
-complex gridfunction, the module \codename{Multipole} interpolates 
+a complex grid function.  For this quantity, and any other real or
+complex grid function, the module \codename{Multipole} interpolates 
 the field $u(t,r,\theta,\phi)$ onto coordinate spheres of given radii
 and calculates the coefficients
 \begin{equation}
@@ -1979,7 +1979,7 @@
   \frac{d x^i}{d t} = -\beta^i, \label{eq:puncturetracking}
 \end{equation}
 where $x^i$ is the puncture location and $\beta^i$ is the shift. Since the
-puncture location usually does not coincide with gridpoints, the shift is
+puncture location usually does not coincide with grid points, the shift is
 interpolated to the location of the puncture.  
 Equation~(\eref{eq:puncturetracking}) is implemented with a simple first-order
 Euler scheme, accurate enough for controlling the location
@@ -2192,7 +2192,7 @@
 \section{Examples}
 \todo{Update if necessary}
 
-To demonstrate the properties of the code and its capabilities, we have used it to simulate common astrophysical configurations of interest.  Given the community-oriented direction of the project, the parameter files required to launch these simulations and a host of others are included and documented in the code releases, along with the datafiles produced by a representative set of simulation parameters to allow for code validation and confirmation of correct code performance on new platforms and architectures.  As part of the internal validation process, 
+To demonstrate the properties of the code and its capabilities, we have used it to simulate common astrophysical configurations of interest.  Given the community-oriented direction of the project, the parameter files required to launch these simulations and a host of others are included and documented in the code releases, along with the data files produced by a representative set of simulation parameters to allow for code validation and confirmation of correct code performance on new platforms and architectures.  As part of the internal validation process, 
 nightly builds are checked against a set of benchmarks to ensure that consistent results are generated with the inclusion of all new commits to the code.
 
 The performance of the Toolkit for vacuum configurations is demonstrated through evolutions of single, rotating BHs and the merger of binary black hole configurations (sections~\ref{sec:1bh-example} and \ref{sec:bbh-example}, respectively).   Linear oscillations about equilibrium for an isolated NS are discussed in section~\ref{sec:tov_oscillations}, and the collapse of a NS to a BH, including dynamical formation of a horizon, in section~\ref{sec:collapse_example}.  Finally, to show a less traditional application of the code, we show its ability to perform cosmological simulations by evolving a Kasner spacetime (see section~\ref{sec:cosmology}).
@@ -2871,7 +2871,7 @@
 by the Cauchy Characteristic Extraction (CCE) technique recently studied
 in~\cite{Babiuc:11,Reisswig:2010cd,Reisswig:2011a}.  The authors of one such
 CCE code~\cite{Babiuc:11} have agreed to make their work available to the
-whole community by integrating their CCE routines into the Einstein Tookit
+whole community by integrating their CCE routines into the Einstein Toolkit
 release 2011\_11 ``Maxwell,'' which will be described elsewhere.
 
 A second  much needed improvement of our existing methods