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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 286)
by ian.hinder＠aei.mpg.de 12 Mar '12

12 Mar '12

User: hinder Date: 2012/03/12 10:57 AM Modified: / ET.tex Log: ET.tex: Rework discussion of NRAR error criteria according to referee comments File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +16 -12 =================================================================== --- ET.tex 2012-03-12 15:56:23 UTC (rev 285) +++ ET.tex 2012-03-12 15:57:39 UTC (rev 286) @@ -2728,18 +2728,22 @@ %seems to be the one corresponding to an $8$-th order accurate finite %difference approximation. We also indicate on both plots the time at which the gravitational -wave frequency reaches $\omega=0.2/\mathrm{M}$. We follow a community standard, agreed -to over the course of the NRAR\cite{NRAR:web} collaboration, that constrains -the numerical resolution so that the accumulated phase error is not -larger than $0.05$ radians at a gravitational wave frequency of -$\omega=0.2/\mathrm{M}$. From the plot, we assert that the phase error between the -higher and high resolutions and the one between high and medium-high -resolutions satisfies this criterion, while the phase error between -the medium-high and medium resolutions barely satisfies the criterion; and the -one between medium and low resolutions does not. We conclude then -that the three highest resolution runs do have sufficient resolution -to extract waveforms for use in the construction of analytic waveform -templates. +wave frequency reaches $\omega=0.2/\mathrm{M}$. This reference time +has been suggested, for example in the NRAR\cite{NRAR:web} +collaboration, as a useful point at which errors can be compared +between codes. The suggestion is that the accumulated phase error +should not be larger than $0.05$ radians at this reference time, and +that this is roughly the scale of accuracy which might be useful for +comparisons with analytic approximation methods. From the plot, we +assert that the phase difference between the higher and high +resolutions and the one between high and medium-high resolutions +satisfies this criterion, while the phase difference between the +medium-high and medium resolutions barely satisfies the criterion; and +the one between medium and low resolutions does not. We conclude then +that the three highest resolution runs do have the suggested accuracy. +While the waveform shown here is too short for comparison with +analytic methods, we illustrate here that these sorts of comparisons +can be made using the toolkit. \begin{figure} \includegraphics[width=0.45\textwidth]{tracks}

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 285)
by roland.haas＠physics.gatech.edu 12 Mar '12

12 Mar '12

User: rhaas Date: 2012/03/12 10:56 AM Modified: / ET.tex Log: re-word explanation of why point-wise convergence at origin fails. File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +4 -6 =================================================================== --- ET.tex 2012-03-12 15:55:18 UTC (rev 284) +++ ET.tex 2012-03-12 15:56:23 UTC (rev 285) @@ -2982,12 +2982,10 @@ violation~\eref{eqn:analysis_hamiltonian_constraint} at the center of the collapsing star. Up to the time when the apparent horizon forms, the convergence order is -an expected $\approx 1.5$. At later times, the collapse of the lapse -function at the -center of the collapsing star renders a pointwise measurement of the -convergence factor at the center impossible. Similarly the $\Gamma$-driver -shift condition used, pushes the infalling matter beyond the -innermost grid point~\cite{Thierfelder:2010dv}. Eventually the shock +an expected $\approx 1.5$. At later times the $\Gamma$-driver +shift condition used pushes the infalling matter beyond the +innermost grid point~\cite{Thierfelder:2010dv}, which prevents a clean +measurement of a convergence factor. Eventually the shock capturing scheme is unable to resolve the steep gradients and becomes dissipative, which leads to a loss of rest mass inside of the apparent horizon. The observed horizon mass on the other hand stays constant.

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 284)
by schnetter＠cct.lsu.edu 12 Mar '12

12 Mar '12

User: eschnett Date: 2012/03/12 10:55 AM Modified: / ET.tex Log: Beautify table 1 File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +2 -3 =================================================================== --- ET.tex 2012-03-12 15:52:06 UTC (rev 283) +++ ET.tex 2012-03-12 15:55:18 UTC (rev 284) @@ -537,9 +537,8 @@ \small \centering \begin{tabular}{lll|rrr} - Name & Architecture (CPU) & Interconnect & nodes & cores/ & CPU - freq. \\ - & & & & node & \\\hline + Name & Architecture (CPU) & Interconnect & nodes & cores/node & CPU + freq. \\\hline Franklin (NERSC) & Cray XT4 (AMD) & SeaStar2 & 8502 & 4 & 2.3 GHz \\ HLRB II (LRZ Munich) & SGI Altix (Itanium) & NUMAlink & 1 & 9728

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 283)
by schnetter＠cct.lsu.edu 12 Mar '12

12 Mar '12

User: eschnett Date: 2012/03/12 10:52 AM Modified: / ET.tex Log: Describe where to download the examples File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +16 -2 =================================================================== --- ET.tex 2012-03-12 15:38:08 UTC (rev 282) +++ ET.tex 2012-03-12 15:52:06 UTC (rev 283) @@ -2403,8 +2403,22 @@ \section{Examples}% \label{sec:examples} -To demonstrate the properties of the code and its capabilities, we have used it to simulate common astrophysical configurations of interest. Given the community-oriented direction of the project, the parameter files required to launch these simulations and a host of others are included and documented in the code releases, along with the data files produced by a representative set of simulation parameters to allow for code validation and confirmation of correct code performance on new platforms and architectures. As part of the internal validation process, -nightly builds are checked against a set of benchmarks to ensure that consistent results are generated with the inclusion of all new commits to the code. +To demonstrate the properties of the code and its capabilities, we +have used it to simulate common astrophysical configurations of +interest. Given the community-oriented direction of the project, the +parameter files required to launch these simulations and a host of +others are included and documented in the code releases\footnote{The + examples shown in this paper are located in a subdirectory + \codename{par/arXiv:1111.3344} of the examples obtained when + downloading the Einstein Toolkit. The current version of these + examples can also be directly accessed via \codename{svn checkout + \url{https://svn.einsteintoolkit.org/cactus/EinsteinExamples/trunk/par/arXiv:1111.3344}}}, +along with the data files produced by a representative set of +simulation parameters to allow for code validation and confirmation of +correct code performance on new platforms and architectures. As part +of the internal validation process, nightly builds are checked against +a set of benchmarks to ensure that consistent results are generated +with the inclusion of all new commits to the code. The performance of the Toolkit for vacuum configurations is demonstrated through evolutions of single, rotating BHs and the merger of binary black hole configurations (sections~\ref{sec:1bh-example} and \ref{sec:bbh-example}, respectively). Linear oscillations about equilibrium for an isolated NS are discussed in section~\ref{sec:tov_oscillations}, and the collapse of a NS to a BH, including dynamical formation of a horizon, in section~\ref{sec:collapse_example}. Finally, to show a less traditional application of the code, we show its ability to perform cosmological simulations by evolving a Kasner spacetime (see section~\ref{sec:cosmology}).

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[svn:einsteintoolkit] EinsteinExamples/branches/ET_2011_10/par/arXiv:1111.3344/ (Rev. 31)
by schnetter＠cct.lsu.edu 12 Mar '12

12 Mar '12

User: eschnett Date: 2012/03/12 10:51 AM Added: /branches/ET_2011_10/par/arXiv:1111.3344/ /branches/ET_2011_10/par/arXiv:1111.3344/bbh/ BBHHighRes.par, BBHHigherRes.par, BBHLowRes.par, BBHMedHRes.par, BBHMedRes.par, bbh.par /branches/ET_2011_10/par/arXiv:1111.3344/collapse/ tov_collapse_vc_l3.par /branches/ET_2011_10/par/arXiv:1111.3344/cosmology/ gowdy.par, kasner-hi.par, kasner-med.par, kasner-vhi.par, kasner.par /branches/ET_2011_10/par/arXiv:1111.3344/kerr/ by-a0.7-hi.par, by-a0.7-med.par, by-a0.7.par /branches/ET_2011_10/par/arXiv:1111.3344/tov/ tov.rpar Log: Backport parameter files used in the ET paper from trunk File Changes: Directory: /branches/ET_2011_10/par/arXiv:1111.3344/bbh/ ======================================================== File [added]: BBHHighRes.par Delta lines: <Unavailable> File [added]: BBHHigherRes.par Delta lines: <Unavailable> File [added]: BBHLowRes.par Delta lines: <Unavailable> File [added]: BBHMedHRes.par Delta lines: <Unavailable> File [added]: BBHMedRes.par Delta lines: <Unavailable> File [added]: bbh.par Delta lines: <Unavailable> Directory: /branches/ET_2011_10/par/arXiv:1111.3344/collapse/ ============================================================= File [added]: tov_collapse_vc_l3.par Delta lines: <Unavailable> Directory: /branches/ET_2011_10/par/arXiv:1111.3344/cosmology/ ============================================================== File [added]: gowdy.par Delta lines: <Unavailable> File [added]: kasner-hi.par Delta lines: <Unavailable> File [added]: kasner-med.par Delta lines: <Unavailable> File [added]: kasner-vhi.par Delta lines: <Unavailable> File [added]: kasner.par Delta lines: <Unavailable> Directory: /branches/ET_2011_10/par/arXiv:1111.3344/kerr/ ========================================================= File [added]: by-a0.7-hi.par Delta lines: <Unavailable> File [added]: by-a0.7-med.par Delta lines: <Unavailable> File [added]: by-a0.7.par Delta lines: <Unavailable> Directory: /branches/ET_2011_10/par/arXiv:1111.3344/tov/ ======================================================== File [added]: tov.rpar Delta lines: <Unavailable>

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[svn:einsteintoolkit] EinsteinExamples/trunk/par/arXiv:1111.3344/collapse/tov_1/ (Rev. 30)
by schnetter＠cct.lsu.edu 12 Mar '12

12 Mar '12

User: eschnett Date: 2012/03/12 10:50 AM Removed: /trunk/par/arXiv:1111.3344/collapse/tov_1/ Log: Remove empty directory

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 282)
by roland.haas＠physics.gatech.edu 12 Mar '12

12 Mar '12

User: rhaas Date: 2012/03/12 10:38 AM Modified: / ET.tex Log: remove offending sentence below Equ. 15 wrt to origin handling in TOV solver File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +2 -3 =================================================================== --- ET.tex 2012-03-12 15:37:20 UTC (rev 281) +++ ET.tex 2012-03-12 15:38:08 UTC (rev 282) @@ -1112,7 +1112,7 @@ The routine also supplies the analytically known solution in the exterior, \begin{eqnarray} - P & = & P({\tt TOV\_atmosphere}),\nonumber \\ + P & = & P(\mbox{\tt TOV\_atmosphere}),\nonumber \\ M_e & = & M, \nonumber\\ \Phi & = &\dfrac{1}{2} \log(1-2M / \hat{r}) \label{eq:TOVexterior} @@ -1129,9 +1129,8 @@ subject to the boundary condition that in the exterior, \begin{eqnarray} r &=& \dfrac{1}{2}\left(\sqrt{\hat{r}^2-2Mr}+\hat{r} -M\right)\nonumber \\ -\hat{r}&=&r\left(1+\dfrac{M}{2r}\right)^2 \ , +\hat{r}&=&r\left(1+\dfrac{M}{2r}\right)^2 \ . \end{eqnarray} -handling with some care the potentially singular terms that appear at the origin. In converting the solution into the variables required for a dynamical evolution, one may assume that the metric is conformally flat, with a conformal factor given by $\psi = \sqrt{\hat{r}/r}$, or equivalently, a logarithmic conformal factor $\phi = \frac{1}{2}\log(\hat{r}/r)$. To facilitate the construction of stars in more complicated dynamical configurations,

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 281)
by ian.hinder＠aei.mpg.de 12 Mar '12

12 Mar '12

User: hinder Date: 2012/03/12 10:37 AM Modified: / ET.tex Log: ET.tex: Add statement saying that the ADM linear momentum is not computed File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +1 -1 =================================================================== --- ET.tex 2012-03-12 15:06:41 UTC (rev 280) +++ ET.tex 2012-03-12 15:37:20 UTC (rev 281) @@ -2011,7 +2011,7 @@ \end{eqnarray} on a specified spherical surface, preferably one far from the center of the domain since these quantities are only properly defined when -calculated at infinity. +calculated at infinity. The ADM linear momentum is not computed. There are also the quasi-local measures of mass and angular momentum, from any \ahz{s} found during the spacetime. Both

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[svn:einsteintoolkit] EinsteinExamples/trunk/par/arXiv:1111.3344/ (Rev. 29)
by schnetter＠cct.lsu.edu 12 Mar '12

12 Mar '12

User: eschnett Date: 2012/03/12 10:37 AM Removed: /trunk/par/arXiv:1111.3344/bbh/BBHHighRes/ /trunk/par/arXiv:1111.3344/bbh/BBHHigherRes/ /trunk/par/arXiv:1111.3344/bbh/BBHLowRes/ /trunk/par/arXiv:1111.3344/bbh/BBHMedHRes/ /trunk/par/arXiv:1111.3344/bbh/BBHMedRes/ /trunk/par/arXiv:1111.3344/bbh/figs/ /trunk/par/arXiv:1111.3344/bbh/py_scripts/ /trunk/par/arXiv:1111.3344/bbh/sm_scripts/ /trunk/par/arXiv:1111.3344/collapse/ plot_defaults.py /trunk/par/arXiv:1111.3344/collapse/tov_15/ /trunk/par/arXiv:1111.3344/collapse/tov_2/ /trunk/par/arXiv:1111.3344/collapse/tov_3/ /trunk/par/arXiv:1111.3344/cosmology/figs/ /trunk/par/arXiv:1111.3344/cosmology/kasner-hi/ /trunk/par/arXiv:1111.3344/cosmology/kasner-med/ /trunk/par/arXiv:1111.3344/cosmology/kasner-vhi/ /trunk/par/arXiv:1111.3344/cosmology/kasner/ /trunk/par/arXiv:1111.3344/kerr/by-a0.7-hi/ /trunk/par/arXiv:1111.3344/kerr/by-a0.7-med/ /trunk/par/arXiv:1111.3344/kerr/by-a0.7/ /trunk/par/arXiv:1111.3344/kerr/figs/ /trunk/par/arXiv:1111.3344/tov/ plot_defaults.py /trunk/par/arXiv:1111.3344/tov/tov_2/ /trunk/par/arXiv:1111.3344/tov/tov_4/ /trunk/par/arXiv:1111.3344/tov/tov_8/ Log: Remove empty directories File Changes: Directory: /trunk/par/arXiv:1111.3344/collapse/ =============================================== File [removed]: plot_defaults.py Delta lines: +0 -1 =================================================================== --- trunk/par/arXiv:1111.3344/collapse/plot_defaults.py 2012-03-12 15:34:13 UTC (rev 28) +++ trunk/par/arXiv:1111.3344/collapse/plot_defaults.py 2012-03-12 15:37:03 UTC (rev 29) @@ -1 +0,0 @@ -link ../../plot_defaults.py \ No newline at end of file Directory: /trunk/par/arXiv:1111.3344/tov/ ========================================== File [removed]: plot_defaults.py Delta lines: +0 -1 =================================================================== --- trunk/par/arXiv:1111.3344/tov/plot_defaults.py 2012-03-12 15:34:13 UTC (rev 28) +++ trunk/par/arXiv:1111.3344/tov/plot_defaults.py 2012-03-12 15:37:03 UTC (rev 29) @@ -1 +0,0 @@ -link ../../plot_defaults.py \ No newline at end of file

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[svn:einsteintoolkit] EinsteinExamples/trunk/par/arXiv:1111.3344/ (Rev. 28)
by schnetter＠cct.lsu.edu 12 Mar '12

12 Mar '12

User: eschnett Date: 2012/03/12 10:34 AM Added: /trunk/par/arXiv:1111.3344/ /trunk/par/arXiv:1111.3344/bbh/ BBHHighRes.par, BBHHigherRes.par, BBHLowRes.par, BBHMedHRes.par, BBHMedRes.par, bbh.par /trunk/par/arXiv:1111.3344/bbh/BBHHighRes/ /trunk/par/arXiv:1111.3344/bbh/BBHHigherRes/ /trunk/par/arXiv:1111.3344/bbh/BBHLowRes/ /trunk/par/arXiv:1111.3344/bbh/BBHMedHRes/ /trunk/par/arXiv:1111.3344/bbh/BBHMedRes/ /trunk/par/arXiv:1111.3344/bbh/figs/ /trunk/par/arXiv:1111.3344/bbh/py_scripts/ plot_defaults.py /trunk/par/arXiv:1111.3344/bbh/sm_scripts/ /trunk/par/arXiv:1111.3344/collapse/ plot_defaults.py, tov_collapse_vc_l3.par /trunk/par/arXiv:1111.3344/collapse/tov_1/ /trunk/par/arXiv:1111.3344/collapse/tov_15/ /trunk/par/arXiv:1111.3344/collapse/tov_2/ /trunk/par/arXiv:1111.3344/collapse/tov_3/ /trunk/par/arXiv:1111.3344/cosmology/ gowdy.par, kasner-hi.par, kasner-med.par, kasner-vhi.par, kasner.par /trunk/par/arXiv:1111.3344/cosmology/figs/ plot_defaults.py /trunk/par/arXiv:1111.3344/cosmology/kasner-hi/ /trunk/par/arXiv:1111.3344/cosmology/kasner-med/ /trunk/par/arXiv:1111.3344/cosmology/kasner-vhi/ /trunk/par/arXiv:1111.3344/cosmology/kasner/ /trunk/par/arXiv:1111.3344/kerr/ by-a0.7-hi.par, by-a0.7-med.par, by-a0.7.par /trunk/par/arXiv:1111.3344/kerr/by-a0.7-hi/ /trunk/par/arXiv:1111.3344/kerr/by-a0.7-med/ /trunk/par/arXiv:1111.3344/kerr/by-a0.7/ /trunk/par/arXiv:1111.3344/kerr/figs/ plot_defaults.py /trunk/par/arXiv:1111.3344/tov/ plot_defaults.py, tov.rpar /trunk/par/arXiv:1111.3344/tov/tov_2/ /trunk/par/arXiv:1111.3344/tov/tov_4/ /trunk/par/arXiv:1111.3344/tov/tov_8/ Log: Add examples from our Einstein Toolkit paper File Changes: Directory: /trunk/par/arXiv:1111.3344/bbh/ ========================================== File [added]: BBHHighRes.par Delta lines: <Unavailable> File [added]: BBHHigherRes.par Delta lines: <Unavailable> File [added]: BBHLowRes.par Delta lines: <Unavailable> File [added]: BBHMedHRes.par Delta lines: <Unavailable> File [added]: BBHMedRes.par Delta lines: <Unavailable> File [added]: bbh.par Delta lines: <Unavailable> Directory: /trunk/par/arXiv:1111.3344/collapse/ =============================================== File [added]: plot_defaults.py Delta lines: <Unavailable> File [added]: tov_collapse_vc_l3.par Delta lines: <Unavailable> Directory: /trunk/par/arXiv:1111.3344/cosmology/ ================================================ File [added]: gowdy.par Delta lines: <Unavailable> File [added]: kasner-hi.par Delta lines: <Unavailable> File [added]: kasner-med.par Delta lines: <Unavailable> File [added]: kasner-vhi.par Delta lines: <Unavailable> File [added]: kasner.par Delta lines: <Unavailable> Directory: /trunk/par/arXiv:1111.3344/cosmology/figs/ ===================================================== File [added]: plot_defaults.py Delta lines: <Unavailable> Directory: /trunk/par/arXiv:1111.3344/kerr/figs/ ================================================ File [added]: plot_defaults.py Delta lines: <Unavailable> Directory: /trunk/par/arXiv:1111.3344/kerr/ =========================================== File [added]: by-a0.7-hi.par Delta lines: <Unavailable> File [added]: by-a0.7-med.par Delta lines: <Unavailable> File [added]: by-a0.7.par Delta lines: <Unavailable> Directory: /trunk/par/arXiv:1111.3344/bbh/py_scripts/ ===================================================== File [added]: plot_defaults.py Delta lines: <Unavailable> Directory: /trunk/par/arXiv:1111.3344/tov/ ========================================== File [added]: plot_defaults.py Delta lines: <Unavailable> File [added]: tov.rpar Delta lines: <Unavailable>

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