[Commits] [svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 19)

[bcmsma at astro.rit.edu]

User: bmundim
Date: 2011/01/24 12:01 PM

Modified:
 /
  ET.tex

Log:
 Following Frank's suggestion of breaking lines around
 column 80.

File Changes:

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

File [modified]: ET.tex
Delta lines: +55 -41
===================================================================
--- ET.tex	2011-01-24 17:52:33 UTC (rev 18)
+++ ET.tex	2011-01-24 18:01:31 UTC (rev 19)
@@ -414,48 +414,58 @@
 \subsection{Initial Data}
 \todo{1/2 page Josh, Bruno}
 
-The Einstein Toolkit contains many modules used to generate initial data for GR simulations,
-including both vacuum and hydrodynamical configurations.  These include modules used primarily
-for testing out various components of the evolution scheme as well as physically motivated
-configurations that describe single of binary blacks and/or neutron stars.  Many of the modules
-are self-contained, consisting of either all the code to generate exact initial solutions or
-the numerical tools required to construct solutions known semi-analytically. Others, though,
-require the installation of other numerical software packages that are included in the toolkit
-as External libraries.  The {\tt twopunctures} module \cite{Ansorg:2004ds}, commonly used in numerical
-relativity to generate binary black hole data, invokes the GNU Scientific Library [GSL; \cite{Galassi:2009}].
-Several modules  have also been implemented to read in datafiles generated by the
-{\tt Lorene code} \cite{Lorene:web,GGTMB}, including the BHBH, BHNS, and NSNS data made publicly
-available through the Lorene website.
+The Einstein Toolkit contains many modules used to generate initial data for 
+GR simulations, including both vacuum and hydrodynamical configurations.  
+These include modules used primarily for testing out various components of 
+the evolution scheme as well as physically motivated configurations that 
+describe single of binary blacks and/or neutron stars.  Many of the modules
+are self-contained, consisting of either all the code to generate exact 
+initial solutions or the numerical tools required to construct solutions 
+known semi-analytically. Others, though, require the installation of other 
+numerical software packages that are included in the toolkit as External 
+libraries.  The {\tt twopunctures} module \cite{Ansorg:2004ds}, commonly 
+used in numerical relativity to generate binary black hole data, invokes 
+the GNU Scientific Library [GSL; \cite{Galassi:2009}].  Several modules  
+have also been implemented to read in datafiles generated by the {\tt Lorene 
+code} \cite{Lorene:web,GGTMB}, including the BHBH, BHNS, and NSNS data 
+made publicly available through the Lorene website.
 
-Scheduling of initial data routines generally follows a standard format.  User-defined parameters
-are run through a parameter check designed to catch obvious internal inconsistencies, in addition to
-any known incompatibilities with other modules of the toolkit.  Initial data is then generated
-at the proper stage within the Cactus framework, determined primarily by whether the configuration
-in question represents vacuum or a hydrodynamical configuration.  Finally, any necessary cleanup
-is typically performed at the end of the initial step, prior to the iterations forward in time.
+Scheduling of initial data routines generally follows a standard format.  
+User-defined parameters are run through a parameter check designed to catch 
+obvious internal inconsistencies, in addition to any known incompatibilities 
+with other modules of the toolkit.  Initial data is then generated at the proper 
+stage within the Cactus framework, determined primarily by whether the 
+configuration in question represents vacuum or a hydrodynamical configuration.  
+Finally, any necessary cleanup is typically performed at the end of the initial 
+step, prior to the iterations forward in time.
 
-For vacuum initial data configurations, an initial data module must supply $g_{ij}$, the spatial 3-metric,
-and $K_{ij}$, the extrinsic curvature.  While the evolution scheme typically makes use of the BSSN formalism,
-the conversion between the physical and conformal metric and extrinsic curvature is handled solely within
-evolution modules, and is not referenced by initial data ones.  Optionally, many initial data modules also
-supply values for the lapse and shift vector, and in some cases time derivatives as well, though these
-may be supplied by other routines depending on the freedom to choose gauge conditions envisioned for a
-specific configuration.
+For vacuum initial data configurations, an initial data module must supply 
+$g_{ij}$, the spatial 3-metric, and $K_{ij}$, the extrinsic curvature.  
+While the evolution scheme typically makes use of the BSSN formalism,
+the conversion between the physical and conformal metric and extrinsic 
+curvature is handled solely within evolution modules, and is not referenced 
+by initial data ones.  Optionally, many initial data modules also supply values 
+for the lapse and shift vector, and in some cases time derivatives as well, 
+though these may be supplied by other routines depending on the freedom 
+to choose gauge conditions envisioned for a specific configuration.
 
-For hydrodynamic configurations, assuming that an equation of state has been specified, the user must also
-supply the values of hydrodynamic variables at all grid locations, in particular the primitive variables
-$\rho$, $v_i$ and the energy variable $\epsilon$ for all cases where we don't have a polytype EOS in the
-form $P=P(\rho)$ (see Sec.~\ref{???} for a discussion of the use of EOS in the ET).  For an MHD configuration,
-one must supply all of these along with the initial magnetic field $B^i$ as well.
+For hydrodynamic configurations, assuming that an equation of state has been 
+specified, the user must also supply the values of hydrodynamic variables 
+at all grid locations, in particular the primitive variables $\rho$, $v_i$ and 
+the energy variable $\epsilon$ for all cases where we don't have a polytype EOS 
+in the form $P=P(\rho)$ (see Sec.~\ref{???} for a discussion of the use of EOS 
+in the ET).  For an MHD configuration, one must supply all of these along with 
+the initial magnetic field $B^i$ as well.
 
 The initial data routines currently implemented include the following:
 \begin{itemize}
 \item Vacuum spacetime tests:
 \begin{enumerate}
-\item {\tt IDConstraintViolate}: A vacuum spacetime in which the diagonal terms in the spatial metric are
-modified by a spatial deformation to explicitly violate the Hamiltonian constraint.
-\item {\tt Exact}: A set of exact spacetimes in various coordinates, along with tools to Lorentz boost
-those configurations.
+\item {\tt IDConstraintViolate}: A vacuum spacetime in which the diagonal terms 
+in the spatial metric are modified by a spatial deformation to explicitly 
+violate the Hamiltonian constraint.
+\item {\tt Exact}: A set of exact spacetimes in various coordinates, along with 
+tools to Lorentz boost those configurations.
 \end{enumerate}
 \item Vacuum gravitational wave configurations:
 \begin{enumerate}
@@ -464,13 +474,17 @@
 \end{enumerate}
 \item Black Hole configurations:
 \begin{enumerate}
-\item {\tt IDAnalyticBH}: This module can generate Schwarzchild black holes, as well as the Misner solution
-for multiple BHs and the brill-Lindquist binary BH solution.
-\item {\tt IDAxibrillBH,~IDAxiOddBrillBH}: These modules generate single black holes deformed by even and
-odd parity axisymmetric perturbations, respectively.
-\item {\tt DistortedBHIVP,~RotatingDBHIVP}: These modules generate single black holes distorted by even
-and odd-parity non-axisymmetric perturbation, respectivey.
-\item {\tt TwoPunctures}: This module generates accurate binary black-hole initial data.
+\item {\tt IDAnalyticBH}: This module can generate Schwarzchild black holes, 
+as well as the Misner solution for multiple BHs and the brill-Lindquist binary 
+BH solution.
+\item {\tt IDAxibrillBH,~IDAxiOddBrillBH}: These modules generate single 
+black holes deformed by even and odd parity axisymmetric perturbations, 
+respectively.
+\item {\tt DistortedBHIVP,~RotatingDBHIVP}: These modules generate single 
+black holes distorted by even and odd-parity non-axisymmetric perturbation, 
+respectivey.
+\item {\tt TwoPunctures}: This module generates accurate binary black-hole 
+initial data.
 \end{enumerate}
 \end{itemize}