User: knarf Date: 2011/11/11 09:34 AM

Modified: / ET.tex

Log: start on small issues in section 2

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File [modified]: ET.tex Delta lines: +12 -12 =================================================================== --- ET.tex 2011-11-11 15:27:00 UTC (rev 184) +++ ET.tex 2011-11-11 15:34:53 UTC (rev 185) @@ -287,10 +287,10 @@

\subsection{Scientific}

-While the list of studies mentioned in the introduction collectively represent +While the aforementioned studies collectively represent breakthrough simulations that have significantly advanced the modeling of relativistic astrophysical systems, all simulations are presently -missing one or more critical physical ingredients, as well as lacking the +missing one or more critical physical ingredients and are lacking the numerical precision to accurately and realistically model the large-scale and small-scale dynamics of their target systems simultaneously.

@@ -301,27 +301,27 @@

\begin{itemize} \item{\bf MHD}. Many studies, in particular those concerned with - massive star collapse, NS-NS or BH-NS binaries, and rotational + massive star collapse, NS-NS or BH-NS binaries and rotational non-axisymmetric instabilities, are still performed in pure GRHD@. Without a doubt, these systems must be simulated with GRMHD to capture - the effects of magnetic fields that in many cases will + the effects of magnetic fields which in many cases will alter the simulation outcome on a qualitative level and may be the driving mechanisms behind much of the observable EM signature from GRBs (e.g.,~\cite{Woosley:2006fn}) and magneto-rotationally exploding core-collapse supernovae (e.g.,~\cite{Burrows:2007yx}). In addition, all simulations that have - taken into account magnetic fields are still limited to the + taken magnetic fields into account are still limited to the ideal MHD approximation, which assumes perfect conductivity. Non-ideal GRMHD schemes are just becoming available~(see, e.g.,~\cite{Palenzuela:2008sf,DelZanna:2007pk}), - but yet to be implemented widely in many branches of numerical relativity. + but have yet to be implemented widely in many branches of numerical relativity.

\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 + exception of recent work on massive star collapse (see, e.g.,~\cite{Ott:2006eu}) and binary mergers (see, e.g.,~\cite{Sekiguchi:2011zd}), - relied on a simple zero-temperature descriptions of + relied on simple zero-temperature descriptions of NS stellar structure, with many assuming simple polytropic forms. Such EOSs are computationally efficient, but are not necessarily a good description for matter in @@ -329,12 +329,12 @@ finite-temperature EOSs, derived from the microphysical descriptions of high-density matter, will lead to qualitatively different and much more astrophysically reliable results (see, e.g.,~\cite{Ott:2006eu}). - In addition, most GR(M)HD studies are - neglecting transport of neutrinos and photons + In addition, most GR(M)HD studies + neglect transport of neutrinos and photons and their interactions with matter. Neutrinos in particular play a crucial role in core-collapse supernovae and in - the cooling of NS-NS merger remnants and must not be left out when - attempting to accurately model such events. Only few studies have + the cooling of NS-NS merger remnants, thus they must not be left out when + attempting to accurately model such events. Few studies have incorporated neutrino and/or photon transport and interactions in approximate ways (see, e.g.,~\cite{Ott:2006eu,Farris:2008fe,Sekiguchi:2011zd}).