From c6eee0bab612c5586d906090941d51efef5a2370 Mon Sep 17 00:00:00 2001
From: allen <allen@6a3ddf76-46e1-4315-99d9-bc56cac1ef84>
Date: Tue, 4 Jun 2002 18:59:59 +0000
Subject: Fixing name clashes in citations

git-svn-id: http://svn.einsteintoolkit.org/cactus/EinsteinInitialData/IDAnalyticBH/trunk@118 6a3ddf76-46e1-4315-99d9-bc56cac1ef84
---
 doc/documentation.tex | 20 ++++++++++----------
 1 file changed, 10 insertions(+), 10 deletions(-)

diff --git a/doc/documentation.tex b/doc/documentation.tex
index 2a47bdf..d9ea1f4 100644
--- a/doc/documentation.tex
+++ b/doc/documentation.tex
@@ -82,7 +82,7 @@ associated parameters in turn.
 The Schwarzschild metric corresponds to a single, static, black hole.
 If the Cactus metric is specified as a conformal metric (by setting
 \texttt{admbase::metric\_type="yes"}), then the metric is
-set using isotropic coordinates \cite{mtw-isotropic}:
+set using isotropic coordinates \cite{CactusEinstein_IDAnalytic_mtw-isotropic}:
 \begin{equation}
   ds^2 = -\left(\frac{2r - M}{2r + M}\right)^2
   + \left(1 + \frac{M}{2r}\right)^4 \left(dr^2 + r^2(d\theta^2
@@ -150,7 +150,7 @@ could modify your parameter file as follows:
 \section{Kerr}
 
 Kerr initial data for an isolated rotating black hole is specified
-using the ``quasi-isotropic'' coordinates \cite{brandt-seidel:1996}:
+using the ``quasi-isotropic'' coordinates \cite{CactusEinstein_IDAnalytic_brandt-seidel:1996}:
 \begin{equation}
   ds^2 = \psi^4 (dr^2 + r^2(d\theta^2 + \chi^2\sin^2\theta d\phi^2)),
 \end{equation}
@@ -213,12 +213,12 @@ intial data with mass $M=1$ and angular momentum $a=0.3$ are:
 
 The earliest suggestion for initial data that might be said to
 corresponding to multiple black holes was given by Misner in 1960
-\cite{misner:1960}. He provided a prescription for writing a metric
+\cite{CactusEinstein_IDAnalytic_misner:1960}. He provided a prescription for writing a metric
 connecting a pair of massive bodies, instaneously at rest, whose
 throats are connected by a wormhole. Using the method of images, this
 solution was generalised to describe any number of black holes whose
 throats connect two identical asymptotically flat spacetimes
-\cite{misner:1963}.
+\cite{CactusEinstein_IDAnalytic_misner:1963}.
 \begin{figure}
   \centering
   \ifpdf
@@ -346,7 +346,7 @@ data which differs from the Misner data mainly in its choice of
 spacetime topology. Whereas the Misner data presumes that the throats
 connect a pair of asymptotically flat spacetimes which are identical
 to each other, the Brill-Lindquist data connects each throat to a
-separate asymptotically flat region \cite{brill-lindquist:1963}.
+separate asymptotically flat region \cite{CactusEinstein_IDAnalytic_brill-lindquist:1963}.
 \begin{figure}
   \centering
   \ifpdf
@@ -396,24 +396,24 @@ parameters such as the following could be used:
 \end{verbatim}
 
 \begin{thebibliography}{9}
-  \bibitem{mtw-isotropic}
+  \bibitem{CactusEinstein_IDAnalyticBH_mtw-isotropic}
     See, for instance, p. 840 of:
     Misner, C. W., Thorne, K. S., and Wheeler, J. A. (1973)
     \emph{Gravitation}, W. H. Freeman, San Francisco.
-  \bibitem{brandt-seidel:1996}
+  \bibitem{CactusEinstein_IDAnalyticBH_brandt-seidel:1996}
     Brandt, Steven R. and Seidel, Edward (1996)
     \emph{Evolution of distorted rotating black holes. III. Initial
     data},
     Phys. Rev., \textbf{D54}, 1403--1416.
-  \bibitem{misner:1960}
+  \bibitem{CactusEinstein_IDAnalyticBH_misner:1960}
     Misner, Charles W. (1960)
     \emph{Wormhole Initial Conditions},
     Phys. Rev., \textbf{118}, 1110--1111.
-  \bibitem{misner:1963}
+  \bibitem{CactusEinstein_IDAnalyticBH_misner:1963}
     Misner, Charles W. (1963)
     \emph{The Method of Images in Geometrostatics},
     Ann. Phys., \textbf{24}, 102--117.
-  \bibitem{brill-lindquist:1963}
+  \bibitem{CactusEinstein_IDAnalyticBH_brill-lindquist:1963}
     Brill, Dieter R., and Lindquist, Richard W. (1963)
     \emph{Interaction Energy in Geometrostatics}
     Phys. Rev., \textbf{131}, 471--476.
-- 
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