[Commits] [svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 186)

[knarf at cct.lsu.edu]

User: knarf
Date: 2011/11/11 10:18 AM

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  ET.tex

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--- ET.tex	2011-11-11 15:34:53 UTC (rev 185)
+++ ET.tex	2011-11-11 16:18:21 UTC (rev 186)
@@ -151,30 +151,28 @@
 been closely tied to the availability and ease-of-use of enabling
 software and computational infrastructure. This document describes
 the Einstein Toolkit, which provides such an infrastructure,
-developed openly and available freely with support from 
+developed openly and made available freely with grant support from 
 the National Science Foundation.
-%under the grant numbers 0903973/0903782/0904015 (CIGR).
 
 Now is a particularly exciting time for numerical relativity and
 relativistic astrophysics, with major advances having been achieved 
 in the study of astrophysical systems containing black holes (BHs) 
-and neutron stars (NSs).  While the first fully general relativistic (GR) 
+and neutron stars (NSs).  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,
-Shibata:2003ga,Shibata:2005ss,Shibata:2006nm}, systems containing BHs proved 
-much more numerically intractable until 2005.  That year, computational 
-breakthroughs were made using a generalized harmonic gauge (GHG) 
-\cite{Pretorius:2005gq} and then a ``moving puncture'' approach 
+Shibata:2003ga,Shibata:2005ss,Shibata:2006nm}. However, systems containing BHs proved 
+much more difficult to track numerically until 2005.  That year, computational 
+breakthroughs were made using a generalized harmonic formulation~\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} 
 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 
+which was now able to effectively evolve the Einstein field equations 
 for coalescing BH-BH binaries and other systems containing moving 
 BHs, including merging BH-NS binaries.
 
-These breakthroughs have led to many advancements with direct relevance 
-to astrophysics, including exciting new results on recoil velocities 
+These breakthroughs had direct relevance 
+to astrophysics, and enabled exciting new results on recoil velocities 
 from BH-BH mergers~(e.g,
 \cite{Baker:2006vn,Campanelli:2007ew,HolleyBockelmann:2007eh,
   Pollney:2007ss,Lousto:2007db,Lousto:2008dn} and references therein),
@@ -193,37 +191,42 @@
 Pfeiffer:2007yz,Stephens:2011as}. 
 
 Meanwhile, general relativistic magneto-hydrodynamics (GRMHD) 
-on fixed background spacetimes has been implemented in multi-dimensional
+on fixed background spacetimes has been successful in multi-dimensional
 settings since the mid-1990s, focusing on BH accretion processes and 
 relativistic jet production and evolution
 (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
-dynamics in compact binary or single-star collapse scenarios, has
+dynamics in compact binary star coalescence 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
+past $\sim 3-5$ years, enabled primarily by the availability of long-term
+stable curvature evolution systems as well as improved GRMHD
 algorithms~(see~\cite{Font:2008aa} for a review). 
 In addition to these developments, substantial progress has been made 
-using physically motivated equations of state (EOS), 
+in importing more 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 
-incorporate microphysical effects, such as neutrino cooling 
-\cite{Sekiguchi:2011zd}.
+(e.g.,~\cite{Shen:1998by,Shen:1998gq,Lattimer:1991nc}).  Some codes
+have also begun to incorporate microphysical effects of neutrino emission
+and deleptonization~\cite{Sekiguchi:2011zd,O'Connor:2009vw}.
 
 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
 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, 
-Jena, and Tokyo/Kyoto).  Nearly all include some form of adaptive mesh 
+either the general harmonic formalism or the
+BSSN formalism in the ``moving puncture'' gauge.  Nearly all include some form of adaptive mesh 
 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~(e.g.,\cite{Duez:2009yy,Sekiguchi:2011zd}).
+\todo{CDO: I think we should
+get completely rid of this; it's impossible to get it right and
+misleading. For example, there is the spec guys and me at Caltech;
+there is Burrows and Pretorius at Princeton, there is now CITA and
+WSU etc. Not at all a good idea to put this in writing.}
 The groups that have reported simulations of NS-NS or BH-NS mergers include:
 \begin{itemize}
 \item {\bf AEI/Sissa}:  BH-NS mergers using GRHD~\cite{Loffler:2006nu} and NS-NS