User: knarf
Date: 2011/11/06 12:33 AM
Modified:
/
ET.tex
Log:
make sure lines are not broken before citations
File Changes:
Directory: /
============
File [modified]: ET.tex
Delta lines: +57 -58
===================================================================
--- ET.tex 2011-11-06 05:30:41 UTC (rev 162)
+++ ET.tex 2011-11-06 05:33:06 UTC (rev 163)
@@ -122,13 +122,13 @@
in the study of astrophysical systems containing black holes (BHs)
and neutron stars (NSs). While the first fully general relativistic (GR)
simulations of merging NS-NS binaries were reported in 1999, with further
-advances for the next few years \cite{Shibata:1999wm,Shibata:2002jb,
+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)
\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}
+(Baumgarte-Shapiro-Shibata-Nakamura) formalism~\cite{Shibata:1995we,Baumgarte:1998te}
that allowed for the first stable long-term evolutions of moving single
and multiple BH systems. These results quickly transformed the field
with the ability to effectively evolve the Einstein field equations
@@ -147,7 +147,7 @@
Ajith:2007kx} and references
therein), comparisons between numerical
waveforms~\cite{Baker:2006yw,Baker:2007fb}, determination of the spin of
-the remnant BH formed in BH-BH mergers~(e.g, \cite{Campanelli:2006uy,
+the remnant BH formed in BH-BH mergers~(e.g,~\cite{Campanelli:2006uy,
Campanelli:2006fg,Campanelli:2006fy,
Herrmann:2007ex,Rezzolla:2007rz,Berti:2007nw} and references therein),
and studies of eccentric BH-BH binaries
@@ -159,25 +159,25 @@
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,
-and \cite{Hawley2009apss} for a review of work on disk and jet models).
+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
dynamics in compact binary or single-star collapse scenarios, has
started to produce astrophysically interesting results only in the
past $\sim 3-5$ years, enabled primarily by the availability of the long-term
stable curvature evolution systems discussed above as well as improved GRMHD
-algorithms~(see \cite{Font:2008aa} for a review).
+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),
-including tabulated versions (e.g., \cite{Pandharipande:1989hn,
+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
+(e.g.,~\cite{Shen:1998by,Shen:1998gq,Lattimer:1991nc}). Some codes also
incorporate microphysical effects, such as neutrino cooling
\cite{Sekiguchi:2011zd}.
Many of the successful techniques used to
evolve BH-BH binaries have proven to be equally applicable to merging
-NS-NS and BH-NS binaries (see, e.g., \cite{Faber:2009zz,Duez:2009yz} for reviews), allowing for further investigations into the former
+NS-NS and BH-NS binaries (see, e.g.,~\cite{Faber:2009zz,Duez:2009yz} for reviews), allowing for further investigations into the former
and the first full GR simulations of the latter. All recent results use
either the GHG formalism (Caltech/Cornell, LSU/BYU/LIU, and Princeton) or
BSSN ``moving puncture'' gauge (or variants thereof; AEI/Sissa, Illinois,
@@ -185,27 +185,27 @@
refinement, since unigrid models cannot produce accurate long-term evolutions
without requiring exorbitant computational resources. Many groups' codes
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.
+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
-mergers using GRHD \cite{Baiotti:2008ra,Baiotti:2009gk,Baiotti:2010xh,
-Baiotti:2011am,Rezzolla:2010fd} and GRMHD \cite{Giacomazzo:2009mp,
+\item[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
-to simulate BH-NS mergers \cite{Duez:2008rb,Duez:2009yy,Foucart:2010eq}.
-\item[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
-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,
+to simulate BH-NS mergers~\cite{Duez:2008rb,Duez:2009yy,Foucart:2010eq}.
+\item[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
+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,
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}.
+most recently with the inclusion of neutrino cooling~\cite{Sekiguchi:2011zd}.
\todo{Check for updates to list before submission!}
\end{description}
@@ -214,10 +214,10 @@
in NSs. GRHD has been used to study, among many other applications,
massive stars collapsing to protoneutron stars
\cite{Ott:2006eu,Ott:2006eh,Shibata:2004kb}, the collapse of rotating,
-hypermassive NSs to BHs in 2D and 3D (see, e.g., \cite{Shibata:2006hr,
+hypermassive NSs to BHs in 2D and 3D (see, e.g.,~\cite{Shibata:2006hr,
Shibata:1999yx,Duez:2005sf,Duez:2005cj,Baiotti:2004wn,Baiotti:2005vi,
Baiotti:2006wn}), and non-axisymmetric instabilities in
-rapidly rotating polytropic NS models \cite{Shibata:1999yx,Baiotti:2006wn,
+rapidly rotating polytropic NS models~\cite{Shibata:1999yx,Baiotti:2006wn,
Manca:2007ca}.
In parallel to the advances in both our physical understanding of
@@ -226,22 +226,22 @@
aim of providing a computational core that can enable the 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
+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.
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
+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
+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.
@@ -281,9 +281,8 @@
\item {\bf Equation of state (EOS), microphysics, and radiation
transport}. Most presently published 3D GR(M)HD simulations, with the
- exceptions of recent work on massive star collapse
- \cite{???}\todo{Citation?} and binary mergers
- (see, e.g., \cite{Sekiguchi:2011zd}),
+ exceptions of recent work on massive star collapse~\cite{???}\todo{Citation?} and binary mergers
+ (see, e.g.,~\cite{Sekiguchi:2011zd}),
relied on a simple zero-temperature descriptions of
NS stellar structure, with many assuming simple polytropic forms.
Such EOSs are computationally
@@ -299,7 +298,7 @@
the cooling of NS-NS merger remnants and must not be left out when
attempting to accurately model such events. Only few studies have
incorporated neutrino and/or photon transport and interactions in
- approximate ways (see, e.g., \cite{Ott:2006eu,Farris:2008fe,Sekiguchi:2011zd}) \todo{Cite more}.
+ approximate ways (see, e.g.,~\cite{Ott:2006eu,Farris:2008fe,Sekiguchi:2011zd}) \todo{Cite more}.
\item {\bf High-order schemes and AMR\@}. Numerical accuracy is a
central issue in long-term GR(M)HD simulations and must be addressed
@@ -307,7 +306,7 @@
grid points on regions where finer resolution is needed, and (2)
high-order numerical techniques.
-Several AMR codes, including the {\tt Carpet} driver \cite{CarpetCode:web}
+Several AMR codes, including the {\tt Carpet} driver~\cite{CarpetCode:web}
included in the Einstein Toolkit,
are publicly available. An important task going forward is
to facilitate the coupling of existing and future GRMHD codes
@@ -462,8 +461,8 @@
The Einstein Toolkit offers two drivers, \codename{PUGH} and
{\tt Carpet}. \codename{PUGH} provides domains consisting of a uniform
grid with Cartesian topology, and is highly scalable (up to more than
-130,000 cores on a Blue Gene/P \cite{Cactuscode:BlueGene:web}.)
-{\tt Carpet} \cite{Schnetter:2003rb, Schnetter:2006pg,
+130,000 cores on a Blue Gene/P~\cite{Cactuscode:BlueGene:web}.)
+{\tt Carpet}~\cite{Schnetter:2003rb, Schnetter:2006pg,
CarpetCode:web} provides multi-block methods and adaptive mesh
refinement (AMR\@). Multi-block methods cover the domain with a set of
(possibly distorted) blocks that exchange boundary information via techniques such as
@@ -471,7 +470,7 @@
methods are supported by {\tt Carpet}, the Einstein Toolkit itself
does not yet
contain any multi-block coordinate systems.} The AMR capabilities
-employ the standard Berger-Oliger algorithm \cite{Berger:1984zza} with
+employ the standard Berger-Oliger algorithm~\cite{Berger:1984zza} with
subcycling in time.
AMR implies that resolution in the simulation
@@ -497,7 +496,7 @@
interpolation operations are implemented efficiently in {\tt Carpet}, and
are applied automatically as specified in the execution schedule,
i.e.\ without requiring function calls in user code.
-Figure \ref{fig:carpet-details} describes some details of the
+Figure~\ref{fig:carpet-details} describes some details of the
Berger-Oliger time stepping algorithm. More details are described in
\cite{Schnetter:2003rb}.
@@ -540,7 +539,7 @@
simulations lies in menial tasks that require no physical or numerical
insight.
-The Simulation Factory \cite{Thomas:2010aa, SimFactory:web} offers a
+The Simulation Factory~\cite{Thomas:2010aa, SimFactory:web} offers a
set of abstractions for the tasks necessary to set up and successfully
finish numerical simulations based on the {\tt Cactus} framework. These
abstractions hide tedious low-level management operations, they
@@ -551,7 +550,7 @@
supercomputers to be used in a uniform manner.
Using the Simulation Factory, we are able to offer a
-tutorial for the Einstein Toolkit \cite{EinsteinToolkit:web} that lets
+tutorial for the Einstein Toolkit~\cite{EinsteinToolkit:web} that lets
new users download, configure, build, and run full simulations of the
coupled Einstein/relativistic hydrodynamics equations on a
supercomputer with a few simple commands. Users need no prior
@@ -932,10 +931,10 @@
A substantial fraction of the published work on the components of the Einstein toolkit
involves the evolution of BH-BH binary systems.
The most widely used routine to generate initial data for these is the
-\codename{TwoPunctures} code, described originally in \cite{Ansorg:2004ds}, which solves
-the binary puncture equations for a pair of BHs \cite{Brandt:1997tf}.
+\codename{TwoPunctures} code, described originally in~\cite{Ansorg:2004ds}, which solves
+the binary puncture equations for a pair of BHs~\cite{Brandt:1997tf}.
To do so, one assumes the extrinsic curvature for each BH corresponds to
-the Bowen-York form \cite{Bowen:1980yu},
+the Bowen-York form~\cite{Bowen:1980yu},
\begin{eqnarray}
K_{(n)}^{ij}&=&\frac{3}{2r^2}(P^in^j+P^jn^i-(\gamma^{ij}-n^in^jP^kn_k))\nonumber\\
&&+\frac{3}{r^3}(\varepsilon^{ikl}S_kn_ln^j+\varepsilon^{jkl}S_kn_ln^i)
@@ -989,7 +988,7 @@
\subsubsection{Lorene-based binary data}
The ET contains three routines that can read in publicly available data generated
-by the {\tt Lorene} code \cite{Lorene:web,Gourgoulhon:2000nn}, though it does not
+by the {\tt Lorene} code~\cite{Lorene:web,Gourgoulhon:2000nn}, though it does not
currently include the capability of generating such data from scratch. For a
number of reasons, such functionality is not truly required; in particular,
{\tt Lorene} is a serial code and there is no time-savings at all to call it as
@@ -1027,9 +1026,9 @@
\end{figure}
\codename{Meudon\_Bin\_BH} can read in BH-BH binary initial data described
-in \cite{Grandclement:2001ed}, while \codename{Meudon\_Bin\_NS}
-handles binary NS data from \cite{Gourgoulhon:2000nn}. \codename{Meudon\_Mag\_NS}
-may be used to read in magnetized isolated NS data \cite{Lorene:web}.
+in~\cite{Grandclement:2001ed}, while \codename{Meudon\_Bin\_NS}
+handles binary NS data from~\cite{Gourgoulhon:2000nn}. \codename{Meudon\_Mag\_NS}
+may be used to read in magnetized isolated NS data~\cite{Lorene:web}.
\subsubsection{TOVSolver}
\label{sec:TOVSolver}
@@ -1197,7 +1196,7 @@
\\
K_0(x^\mu) & := & 0
\end{eqnarray}
-and $\Gamma$-driver shift condition \cite{Alcubierre:2002kk}:
+and $\Gamma$-driver shift condition~\cite{Alcubierre:2002kk}:
\begin{eqnarray}
G(\alpha,\phi,x^\mu) & := & (3/4)\, \alpha^{-2}
\\
@@ -1217,7 +1216,7 @@
$\beta^i$ 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, Schnetter:2010cz}, this
+As described, e.g., in~\cite{Muller:2009jx, Schnetter:2010cz}, 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.
@@ -1270,7 +1269,7 @@
During time evolution, a Sommerfeld-type radiative boundary condition
is applied to all components of the evolved BSSN variables as
-described in \cite{Alcubierre:2000xu}. The main feature of this boundary
+described in~\cite{Alcubierre:2000xu}. 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
@@ -1328,7 +1327,7 @@
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{Brown:2008sb}. Gauge changes
+inwards with the speed of light~\cite{Brown:2008sb}. Gauge changes
introduced by the boundary condition, which are physically not
observable, propagate faster, with a speed up to $\sqrt{2}$ for the
gauge conditions used in \codename{McLachlan}.
@@ -1348,7 +1347,7 @@
The primary hydrodynamics evolution routine in the Einstein Toolkit is
\codename{GRHydro}, a code derived from the public \codename{Whisky}
-code \cite{Baiotti:2004wn,Hawke:2005zw,Baiotti:2010zf,Whisky:web}
+code~\cite{Baiotti:2004wn,Hawke:2005zw,Baiotti:2010zf,Whisky:web}
designed primarily by researchers at AEI and their collaborators. It
includes a high resolution shock capturing (HRSC) scheme to evolve
hydrodynamic quantities, with several different reconstruction methods
@@ -1400,7 +1399,7 @@
We choose a definition of the 3-velocity that corresponds to the
velocity seen by an Eulerian observer at rest in the current spatial
-3-hypersurface \cite{},
+3-hypersurface~\cite{},
\begin{equation}
v^i = \frac{u^i}{W} + \frac{\beta^i}{\alpha}\,\,,
\label{eq:vel}
@@ -1480,7 +1479,7 @@
different forms of the slope limiter available. In practice, all
try to accomplish the same task of preserving monotonicity and removing
the possibility of spuriously creating local extrema. Implemented methods
-include minmod, superbee \cite{Roe:1986cb}, and monotonized central \cite{vanLeer:1977aa}.
+include minmod, superbee~\cite{Roe:1986cb}, and monotonized central~\cite{vanLeer:1977aa}.
The piecewise parabolic method (PPM) is a multi-step method based around
a quadratic fit to nearby points interpolated to cell faces
@@ -1513,7 +1512,7 @@
in question in space and time.
The simplest method implemented is the Harten-Lax-van Leer-Einfeldt
-solver \cite{Harten:1983on,Einfeldt:1988og} (HLL or HLLE, depending on the reference),
+solver~\cite{Harten:1983on,Einfeldt:1988og} (HLL or HLLE, depending on the reference),
which uses a two wave approximation to calculate the evolution along
the shock front. With $\xi_-$ and $\xi_+$ the most negative and
most positive wave speeds present on either side of the interface,
@@ -1546,7 +1545,7 @@
\end{equation}
It is these flux terms that are then used to evolve the hydrodynamic quantities.
-The Roe solver \cite{Roe:1981ar} involves linearizing the evolution system
+The Roe solver~\cite{Roe:1981ar} involves linearizing the evolution system
for the hydrodynamic evolution. Eq.~\ref{eq:Riemann}, defining
the Jacobian matrix $A\equiv \frac{\partial f}{\partial q}$, and
working out the eigenvalues $\lambda^i$ and left and right eigenvectors,
@@ -1572,7 +1571,7 @@
\subsubsection{Conservative to primitive conversion}
-In order to invert Eqs.~\ref{eq:p2c1} -- \ref{eq:p2c3}, solving for
+In order to invert Eqs.~\ref{eq:p2c1}~--~\ref{eq:p2c3}, solving for
the primitive variables based on the values of the conservative ones,
\codename{GRHydro} uses a 1-dimensional Newton-Raphson approach that
solves for a consistent value of the pressure. Defining the (known)
@@ -1656,7 +1655,7 @@
is encapsulated in the constant adiabatic index $\Gamma$. This EOS has been
used extensively in simulations of NS-NS and BH-NS mergers.
-The hybrid EOS, first introduced by \cite{Janka:1993da}, is a 2-piece
+The hybrid EOS, first introduced by~\cite{Janka:1993da}, is a 2-piece
piecewise polytropic with a thermal component designed for the
application in simple models of stellar collapse. At densities below
nuclear, a polytropic EOS with $\Gamma = \Gamma_1 \approx 4/3$ is
@@ -1878,7 +1877,7 @@
years~\cite{Szabados:2004ql}. Even though only a few rigorous proofs exist
that establish the properties of these latter quantities, they have
been demonstrated to be surprisingly helpful in numerical simulations
-(see, e.g., \cite{Lovelace:2009dg}), and are therefore
+(see, e.g.,~\cite{Lovelace:2009dg}), and are therefore
an indispensable tool in numerical relativity.
\codename{QuasiLocalMeasures} takes as input a horizon surface, or any
other surface that the user specifies, like a large coordinate
