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[svn:einsteintoolkit] GRHydro/trunk/src/ (Rev. 287)
by bcmsma＠astro.rit.edu 01 Nov '11

01 Nov '11

User: bmundim Date: 2011/11/01 05:19 PM Modified: /trunk/src/ GRHydro_SourceM.F90, GRHydro_TmunuM.F90 Log: RIT dev: Implement comoving contravariant magnetic 4-vector. File Changes: Directory: /trunk/src/ ====================== File [modified]: GRHydro_SourceM.F90 Delta lines: +1 -1 =================================================================== --- trunk/src/GRHydro_SourceM.F90 2011-10-25 18:45:10 UTC (rev 286) +++ trunk/src/GRHydro_SourceM.F90 2011-11-01 22:19:55 UTC (rev 287) @@ -252,7 +252,7 @@ rhohstarW2 = (rho(i,j,k)*(one + eps(i,j,k)) + press(i,j,k)+ b2)*& w_lorentz(i,j,k)**2 - pstar = press(i,j,k)+b2/2.d0 + pstar = press(i,j,k)+0.5d0*b2 !!$ For a change, these are T^{ij} File [modified]: GRHydro_TmunuM.F90 Delta lines: +13 -1 =================================================================== --- trunk/src/GRHydro_TmunuM.F90 2011-10-25 18:45:10 UTC (rev 286) +++ trunk/src/GRHydro_TmunuM.F90 2011-11-01 22:19:55 UTC (rev 287) @@ -67,12 +67,16 @@ #define Bvecx(i,j,k) Bvec(i,j,k,1) #define Bvecy(i,j,k) Bvec(i,j,k,2) #define Bvecz(i,j,k) Bvec(i,j,k,3) +#define bcomx(i,j,k) bcom(i,j,k,1) +#define bcomy(i,j,k) bcom(i,j,k,2) +#define bcomz(i,j,k) bcom(i,j,k,3) subroutine GRHydro_TmunuM(CCTK_ARGUMENTS) implicit none DECLARE_CCTK_ARGUMENTS + DECLARE_CCTK_PARAMETERS CCTK_REAL :: velxlow, velylow, velzlow CCTK_REAL :: betaxlow, betaylow, betazlow, beta2 @@ -119,7 +123,7 @@ !!$ square of the lorentz factor. rhohstarw2 = w_lorentz(i,j,k)**2*(rho(i,j,k)*(1.0D0 + eps(i,j,k)) + press(i,j,k) + b2) - pstar = press(i,j,k)+b2/2.d0 + pstar = press(i,j,k)+0.5d0*b2 !!$ Calculate lower components of 4-velocity (without the Lorent factor). !!$ uxlow = velxlow @@ -142,6 +146,14 @@ eTxz(i,j,k) = eTxz(i,j,k) + rhohstarw2*velxlow*velzlow + pstar*gxz(i,j,k) - bxlow*bzlow eTyz(i,j,k) = eTyz(i,j,k) + rhohstarw2*velylow*velzlow + pstar*gyz(i,j,k) - bylow*bzlow + if(calculate_bcom .ne. 0) then + bcom_sq(i,j,k) = b2 + bcom0(i,j,k) = w_lorentz(i,j,k)*bdotv/alp(i,j,k) + bcomx(i,j,k) = Bvecx(i,j,k)/w_lorentz(i,j,k) + bcom0(i,j,k)*(alp(i,j,k)*velx(i,j,k)-betax(i,j,k)) + bcomy(i,j,k) = Bvecy(i,j,k)/w_lorentz(i,j,k) + bcom0(i,j,k)*(alp(i,j,k)*vely(i,j,k)-betay(i,j,k)) + bcomz(i,j,k) = Bvecz(i,j,k)/w_lorentz(i,j,k) + bcom0(i,j,k)*(alp(i,j,k)*velz(i,j,k)-betaz(i,j,k)) + endif + end do end do end do

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 157)
by roland.haas＠physics.gatech.edu 27 Oct '11

27 Oct '11

User: rhaas Date: 2011/10/27 08:52 PM Modified: / ET.tex /examples/collapse/ H_convergence_at0.pdf, H_convergence_at0.py Log: work on text for tov collapse section update tov collpase plot with nicer tick marks remove some todos of Roland's point out conflict in usage of \\rho File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +60 -33 =================================================================== --- ET.tex 2011-10-24 19:14:38 UTC (rev 156) +++ ET.tex 2011-10-28 01:52:58 UTC (rev 157) @@ -1352,6 +1352,10 @@ \subsection{Hydrodynamics Evolution} \label{sec:GRHydro} +\todo{RH: there is a conflict of notation between the rest mass density $\rho$ +as used by GRHydro and the $T_{nn}$ component used by the spacetime codes +(McLachlan, TOVSolver, TwoPunctures if we described it). Ways around it would +be $\rho_0$ and $\rho_{ADM}$ for examples.} Hydrodynamic evolution in the Einstein Toolkit is designed so that it interacts with the metric curvature evolution through a small set of variables, allowing for maximum modularity in implementing, editing, @@ -2011,7 +2015,7 @@ base modules described in Sec.~\ref{sec:base_modules}, explicitly written as: \begin{eqnarray} - H &=& R - K^i{}_j K^j{}_i + K^2 - 16 \pi \rho \\ + H &=& R - K^i{}_j K^j{}_i + K^2 - 16 \pi \rho \label{eqn:analysis_hamiltonian_constraint}\\ M_i &=& \nabla_j K_i{}^j - \nabla_i K - 8 \pi S_i \end{eqnarray} where $S_i=-\frac{1}{\alpha} \left( T_{i0} - \beta^j T_{ij} \right)$. @@ -2121,7 +2125,7 @@ \end{center} \caption{Grid layout of a simulation using \codename{Cartoon2D}. The $z$-axis is the axis of rotational symmetry. Image courtesy of - Denis Pollney.\todo{RH: ask Denis if we can use his figure}} + Denis Pollney.} \label{fig:cartoon-plane} \end{figure} @@ -2141,7 +2145,7 @@ point $x''$ for which there is actual data stored. In this example, two reflection symmetries along the horizontal and vertical axis are present. Notice how the vector components change in - transformations $A$ and $B$. Image courtesy of Steve White.} + transformations $A$ and $B$.} % Image courtesy of Steve White.} \label{fig:faces} \end{figure} @@ -2687,33 +2691,49 @@ $2$.} \end{figure} -\subsection{Collapse\pages{2 Christian}} -Show TOV collapse and BH formation -\todo{RH: there are three runs for this for convergence testing. All three will be -used eventually. These plots~\ref{fig:tov_collapse_rho_central}, \ref{fig:tov_collapse_radii} -currently only use data from the highest resolution run to show what happens.} +\subsection{Collapse\pages{2 Christian, Roland}} The previous examples dealt either with a preexisting black hole (BBH) or -with a smooth singularity free spacetime (TOV oscillations). The ET however is +with a smooth singularity free spacetime (TOV oscillations). The evolution +codes in the toolkit however are also able to handle the dynamic formation of a singularity as a star collapses into a black hole. As a simple example of this process we study the collapse -of a non-rotating TOV solution into a black hole. We create initial data as in +of a non-rotating TOV star into a black hole. We create initial data as in section~\ref{sec:tov_oscilations} using $\rho_c=3.154e-3$ and $K_{ID} = 100$, -$\Gamma = 2$ yielding a star of mass $1.67\,M_\odot$. As is common in these -situations we trigger collapse by reducing the pressure during the evolution -by reducing the polytropic constant $K_{ID}$ from its initial data value to $K -= 0.98 \, K_{ID} = 98$. \todo{RH: cite some papers, eg. Whisky and ref -therein} -Doing so speeds up the collapse and provides a -physical trigger for the collapse rather than random numerical fluctuations +$\Gamma = 2$ yielding a star of mass $1.67\,M_\odot$. As is +common in these situations~\cite{Baiotti:2005vi} we trigger collapse by +reducing the pressure support after initial data has been constructed +by lowering the polytropic constant +$K_{ID}$ from its initial data value to $K = 0.98 \, K_{ID} = 98$. To ensure +that the pressure depleted configuration remains a solution of the +constraints~\cite{eqn:analysis_hamiltonian_constraint} in the presence of +matter we rescale the rest mass density +$\rho$ such that the total energy density $T_{nn}$ \todo{RH: unify notation of +$\rho$} does not change +\begin{equation} + \rho' + K (\rho')^2 = \rho + K_{ID} \rho^2. + \label{eqn:collapse_rho_rescaled} +\end{equation} +Compared to the initial configuration, this rescaled star posseses a higher +central density and lower pressure. +This change in $K$ speeds up the collapse and provides a +physical trigger for the collapse rather relying on random numerical +fluctuations which would not be guaranteed to converge to a unique value with higher resolution. In order to resolve the star as well as push the outer boundary far enough away so that the star and the numerical outer boundary are not in causal contact during the simulation we employ a fixed mesh refinement scheme. The outermost box has a radius of $R_0 = 204.8\,M_\odot$ and a resolution of -$3.2\,M_\odot$ ($1.6\,M_\odot$, $0.6\,M_\odot$ for higher convergence levels). +$3.2\,M_\odot$ ($2.4\,M_\odot$, $1.6\,M_\odot$, $0.6\,M_\odot$ for higher +convergence levels). Around the star which is centered on the origin we stack $5$ extra boxes of -size $4\times2^\ell$, $0 \le \ell \le 4$ where the resolution on each finer -level is twice that of the surrounding level. We use the PPM +approximate size $8\times2^\ell\,M_\odot$ for $0 \le \ell \le 4$, where the +resolution on each finer +% RH: there is a likely typo in the paramter file which creates boxes of +% radii: 2M,4M,8M,13.6M(!),32M,64M respectively. Changing it to 16M +% doesn't really do any good or harm. +level is twice that of the surrounding level. In order to resolve the large +density gradients developping during the collapse, two more levels with radii +$4\,M_\odot$ and $2\,M_\odot$ are present inside of the star. We use the PPM reconstruction method and the HLLE Riemann solver to obtain second order convergent results in smooth regions. Due to the presence of the density maximum at the center of the star and the non-smooth atmosphere at the @@ -2722,30 +2742,37 @@ \begin{figure} \label{fig:tov_collapse_radii} \includegraphics[width=0.9\textwidth]{examples/collapse/radii} - \caption{Location on x axis where $\rho = 100\,\mathtt{whisky\_rho\_min}$ and - the areal radius of the apparent horizon ($R_g = 2\,M_\star = - 2\,1.63\,M_{\mathord\odot}$).} + \caption{Stellar radius of the collapsing star and radius of the forming + apparent horizon. The stellar surface is defined as the point where $\rho$ is + $100$ time the atmosphere density. $R$ is the circumferential radius of the + apparent horizon and $R_g = 2\,M_\star = 2\times1.63\,M_{\mathord\odot}$. An + apparent horizon forms at a time roughly equal to when the mass of the star + is enclosed in its gravitational radius, forming black hole and causally + disconnecting the evolution in the interior from the outside spacetime.} \end{figure} \begin{figure} \label{fig:tov_collapse_H_convergence_at0.pdf} \includegraphics[width=0.9\textwidth]{examples/collapse/H_convergence_at0} \caption{Convergence factor for the Hamiltonian constraint evaluated at the - center of the collapsing star.} + center of the collapsing star. We plot convergence factors computed using + a set of 5 runs covering the diameter of the star with $\approx 60, 80, + 120, 240$ grid points. + % initial star radius is: 6M, resolutions are 0.2,0.15,0.1,0.05 on the box + % (radius 8M) covering the star + } \end{figure} In Figure~\ref{fig:tov_collapse_radii} we plot on the same graph the -approximate location of the edge of star and the areal radius of the apparent +approximate location of the star surface and the circumferential radius of the +apparent horizon once a horizon is found in the simulation. Clearly the apparent horizon is found at approximately the same time as the star's size approaches -its Schwarzschild radius.\todo{RH:replace AH radius with coordinate radius} In +its Schwarzschild radius. In Figure~\ref{fig:tov_collapse_H_convergence_at0} we display the convergence factor for the Hamiltonian constraint at the center of the collapsing star. -Hopefully we -see that the convergence order is between $1$ and $2$. Just before the -apparent horizon forms the density at the center of the star increases rapidly -and we are unable to properly resolve the small central region with the -available computational resources. For this reason the maximum of the -Hamiltonian constraint rises rapidly just before the the interior of the star -is encapsulated in the horizon. +Up to the time when the apparent horizon forms the convergence order is +$\approx 1.5$ as expected. After that the singularity which forms at the +center of the black hole prevents a clear measurement of the convergence +factor. \subsection{Cosmology\pagesdone{1}} Directory: /examples/collapse/ ============================== File [modified]: H_convergence_at0.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [modified]: H_convergence_at0.py Delta lines: +2 -2 =================================================================== --- examples/collapse/H_convergence_at0.py 2011-10-24 19:14:38 UTC (rev 156) +++ examples/collapse/H_convergence_at0.py 2011-10-28 01:52:58 UTC (rev 157) @@ -27,13 +27,13 @@ ax.set_xlabel(r't [M]') ax.xaxis.set_major_locator(mticker.MaxNLocator(7)) -ax.xaxis.set_minor_locator(mticker.MaxNLocator(14)) +ax.xaxis.set_minor_locator(mticker.AutoMinorLocator(2)) ax.xaxis.grid(False) ax2 = ax.twiny() ax2.set_xlabel(r't [ms]') ax2.set_xlim((ax.get_xlim()[0]/M_to_ms, ax.get_xlim()[1]/M_to_ms)) ax2.xaxis.set_major_locator(mticker.MaxNLocator(7)) -ax2.xaxis.set_minor_locator(mticker.MaxNLocator(14)) +ax2.xaxis.set_minor_locator(mticker.AutoMinorLocator(2)) ax.set_ylabel(r'$C(H)$') ax.yaxis.set_major_locator(mticker.MaxNLocator(5)) ax.yaxis.set_minor_locator(mticker.MaxNLocator(10))

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[svn:einsteintoolkit] IDAnalyticBH/trunk/src/ (Rev. 183)
by schnetter＠cct.lsu.edu 27 Oct '11

27 Oct '11

User: eschnett Date: 2011/10/27 10:30 AM Modified: /trunk/src/ BrillLindquist.c Log: Use "epsilon" also for Brill-Lindquist IDAnalyticBH has an "epsilon" parameter to smooth out singularites. This parameter should also be used in Brill-Lindquist initial data. Otherwise, moving puncture evolution of these data is not possible without an explicit smoothing step. File Changes: Directory: /trunk/src/ ====================== File [modified]: BrillLindquist.c Delta lines: +1 -1 =================================================================== --- trunk/src/BrillLindquist.c 2011-10-25 18:45:16 UTC (rev 182) +++ trunk/src/BrillLindquist.c 2011-10-27 15:30:44 UTC (rev 183) @@ -143,7 +143,7 @@ tmp1 = sqrt(SQR(xval+hole_x0[n]) +SQR(yval+hole_y0[n]) +SQR(zval+hole_z0[n]) - +1.0e-20); + +SQR(epsilon)); psi[i] += hole_mass[n]/tmp1*0.5;

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[svn:einsteintoolkit] NullNews/trunk/src/ (Rev. 6)
by schnetter＠cct.lsu.edu 27 Oct '11

27 Oct '11

User: eschnett Date: 2011/10/27 09:37 AM Modified: /trunk/src/ set_pointers.h Log: PITTNullCode/NullNews does not build on BlueGene/P; the C++ STL reports an error. The reason seems to be that NULL is interpreted as integer constant instead of a pointer. An explicit case solves this problem there. File Changes: Directory: /trunk/src/ ====================== File [modified]: set_pointers.h Delta lines: +4 -4 =================================================================== --- trunk/src/set_pointers.h 2011-10-25 18:45:30 UTC (rev 5) +++ trunk/src/set_pointers.h 2011-10-27 14:37:05 UTC (rev 6) @@ -1,9 +1,9 @@ // define pointer array for past timelevels! - vector<CCTK_REAL*> uBondiP(max_timelevels, NULL); - vector<CCTK_COMPLEX*> Psi4P(max_timelevels, NULL); - vector<CCTK_COMPLEX*> NewsP(max_timelevels, NULL); - vector<CCTK_COMPLEX*> NewsBP(max_timelevels, NULL); + vector<CCTK_REAL*> uBondiP(max_timelevels, (CCTK_REAL*)NULL); + vector<CCTK_COMPLEX*> Psi4P(max_timelevels, (CCTK_COMPLEX*)NULL); + vector<CCTK_COMPLEX*> NewsP(max_timelevels, (CCTK_COMPLEX*)NULL); + vector<CCTK_COMPLEX*> NewsBP(max_timelevels, (CCTK_COMPLEX*)NULL); // Get current timelevel... // We assume here that the two vars uBondi[0] amd uBondi[1] are right next to each

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[svn:einsteintoolkit] www/about/releases/ (Rev. 742)
by schnetter＠cct.lsu.edu 25 Oct '11

25 Oct '11

User: eschnett Date: 2011/10/25 04:00 PM Modified: /about/releases/ ET_2011_10_announcement.php Log: Reword release notes File Changes: Directory: /about/releases/ =========================== File [modified]: ET_2011_10_announcement.php Delta lines: +84 -39 =================================================================== --- about/releases/ET_2011_10_announcement.php 2011-10-25 20:57:05 UTC (rev 741) +++ about/releases/ET_2011_10_announcement.php 2011-10-25 21:00:57 UTC (rev 742) @@ -1,19 +1,58 @@ <?php $title='Release Announcement'; include_once($_SERVER['DOCUMENT_ROOT'].'/global/header.php');?> -We are pleased to announce the fourth release (code name "<a href="http://en.wikipedia.org/wiki/James_Clerk_Maxwell">Maxwell</a>") of the Einstein Toolkit, an open, community developed software infrastructure for relativistic astrophysics. This release includes substantial changes to the underlying AMR infrastructure Carpet and the simfactory tool. GRHydro is now officially released with support for magnetohydrodynamics. In addition, bug fixes accumulated since the previous release in April 2011 have been included. +We are pleased to announce the fourth release (code name +"<a href="http://en.wikipedia.org/wiki/James_Clerk_Maxwell">Maxwell</a>") +of the Einstein Toolkit, an open, community developed software +infrastructure for relativistic astrophysics. This release includes +substantial changes to the underlying AMR infrastructure Carpet and +the Simfactory tool. GRHydro now officially supports +magnetohydrodynamics. In addition, many errors have been corrected +since the previous release in April 2011. -The Einstein Toolkit is a collection of software components and tools for simulating and analyzing general relativistic astrophysical systems that builds on numerous software efforts in the numerical relativity community including CactusEinstein, the Carpet AMR infrastructure and the relativistic hydrodynamics code GRHydro (an updated and extended version of the public release of the Whisky code). The Cactus Framework is used as the underlying computational infrastructure providing large-scale parallelization, general computational components, and a model for collaborative, portable code development. The toolkit includes modules to build complete codes for simulating black hole spacetimes as well as systems governed by relativistic hydrodynamics. +The Einstein Toolkit is a collection of software components and +tools for simulating and analyzing general relativistic astrophysical +systems. It builds on numerous software efforts in the numerical +relativity community including CactusEinstein, the Carpet AMR +infrastructure, and the relativistic hydrodynamics code GRHydro. The +Cactus Framework is used as the underlying computational +infrastructure providing large-scale parallelization, general +computational components, and a model for collaborative, portable code +development. The toolkit includes modules to build complete codes for +simulating black hole spacetimes as well as systems governed by +relativistic hydrodynamics. -The Einstein Toolkit uses a distributed software model and its different modules are developed, distributed, and supported either by the core team of Einstein Toolkit Maintainers, or by individual groups. Where modules are provided by external groups, the Einstein Toolkit Maintainers provide quality control for modules for inclusion in the toolkit and help coordinate support. The Einstein Toolkit Maintainers currently involve postdocs and faculty from five different institutions, and host weekly meetings that are open for anyone to join in. +The Einstein Toolkit uses a distributed software model, and its +different modules are developed, distributed, and supported either by +the core team of Einstein Toolkit Maintainers, or by individual +research groups. Where modules are provided by external groups, the +Einstein Toolkit Maintainers provide quality control for modules for +inclusion in the toolkit and help coordinate support. The Einstein +Toolkit Maintainers currently involve postdocs and faculty from five +different institutions, and host weekly meetings that are open for +anyone to join. -Guiding principles for the design and implementation of the toolkit include: open, community-driven software development; well thought out and stable interfaces; separation of physics software from computational science infrastructure; provision of complete working production code; training and education for a new generation of researchers. +Guiding principles for the design and implementation of the toolkit +include: open, community-driven software development; well thought-out +and stable interfaces; separation of physics software from +computational science infrastructure; provision of a complete working +production code; and training and education for a new generation of +researchers. -For more information about using or contributing to the Einstein Toolkit, or to join the Einstein Toolkit Consortium, please visit our web pages at <<a href="http://einsteintoolkit.org">http://einsteintoolkit.org</a>>. +For more information about using or contributing to the Einstein +Toolkit, or to join the Einstein Toolkit Consortium, please visit our +web pages at +<<a href="http://einsteintoolkit.org">http://einsteintoolkit.org</a>>. -The Einstein Toolkit is primarily supported by NSF 0903973/0903782/0904015 (CIGR), and also by NSF 0701566/0855892 (XiRel), 0721915 (Alpaca), 0905046/0941653 (PetaCactus) and 0710874 (LONI Grid). +The Einstein Toolkit is primarily supported by NSF +0903973/0903782/0904015 (CIGR), and also by NSF 0701566/0855892 +(XiRel), 0721915 (Alpaca), 0905046/0941653 (PetaCactus), and 0710874 +(LONI). -The Einstein Toolkit thorns contain over 130 regression test cases. On a large portion of the tested machines, all of these testsuites <a href="http://einsteintoolkit.org/release-info/parse_testsuite_results.php">pass</a>, using both MPI and OpenMP. +The Einstein Toolkit thorns contain over 130 regression test cases. +On a large portion of the tested machines, all of these +testsuites <a href="http://einsteintoolkit.org/release-info/parse_testsuite_results.php">pass</a>, +using both MPI and OpenMP parallelisation. The changes between this and the previous release include: <ul> @@ -22,65 +61,71 @@ <ul> <li> Significant internal development <li> Grid structure is handled in a more efficient manner, leading to improved parallel scalability - <li> Grid structure output now supports multipatch + <li> Grid structure output supports multipatch <li> Improvements to OpenMP parallelism in Carpet <li> Support for cell-centering - <li> Timers are now hierarchical - use parameter output_timer_tree_every to output the timer tree to standard output. This makes it much easier to see where the time is spent in a simulation - <li> A backtrace file is now written to the output directory when the simulation code crashes. Note that you probably need to add the -rdynamic option to CFLAGS and CXXFLAGS for the backtrace symbols to be interpreted correctly. + <li> Timers are hierarchical, which makes it much easier to see where the time is spent in a simulation. (Use the parameter output_timer_tree_every to output the timer tree to standard output.) + <li> A backtrace file is written to the output directory when the simulation code crashes. (Note that you probably need to add the -rdynamic option to CFLAGS and CXXFLAGS for the backtrace symbols to be interpreted correctly.) </ul> - <li> CarpetIOHDF5: There are now parameters which select whether symmetry, boundary and buffer points are output for sliced output. - <li> CarpetRegrid2: Now supports "true" AMR based on a regridding criterion + <li> CarpetIOHDF5: There are now parameters to select whether + symmetry, boundary, or buffer points should be output. + <li> CarpetRegrid2: Supports full AMR based on a regridding criterion <li> SimFactory <ul> - <li> Completely new rewrite, new repository. - <li> Machine database and optionlists updated due to system changes on HPC resources - <li> Can now run the Cactus test suites as part of a job in a queuing system - <li> TODO: List of new machines supported by SimFactory? - <li> Optionlists now enable instruction vectorisation by default - this affects those thorns that explicitly use this vectorisation, including McLachlan and Carpet - <li> Now supports parameter file scripts <name>.rpar - these should be scripts which write a parameter file to <name>.par. This is useful for performing simple calculations on parameters in python or perl - <li> Now uses the Intel compiler by default on Kraken and Hopper + <li> Internally completely rewritten + <li> Machine database and optionlists updated + <li> Can run the Cactus test suites as part of a job in a queuing system +  + <li> Optionlists enable instruction vectorization by default, + which can significantly improve performance. (This affects those thorns that explicitly use vectorisation, including McLachlan and Carpet.) + <li> Supports parameter file scripts <name>.rpar, written e.g. + in Perl or Python. + <li> Uses the Intel compiler by default on Kraken and Hopper </ul> <li> Cactus <ul> <li> CUDA support added for GPU computing - <li> Parameters can now be used in STORAGE specifications in schedule.ccl files - <li> Multi-line parameter values can now contain comments - this makes it easier to comment out entries - <li> Mac OS 10.7 (Lion) is now supported - <li> CCTK_GFINDEX3D now checks index against array bounds when CCTK_DEBUG is defined - <li> Standard output of Cactus build process is now much more compact + <li> Parameters can be used in STORAGE specifications in schedule.ccl files + <li> Multi-line parameter values can contain comments - this makes it easier to comment out entries + <li> Mac OS 10.7 (Lion) is supported + <li> CCTK_GFINDEX3D checks index against array bounds in debug configurations + <li> Standard output of Cactus build process is much more compact </ul> <li> McLachlan <ul> - <li> Performance improvements + <li> Various performance improvements <li> BSSN has instruction vectorisation enabled by default for improved speed </ul> <li> GRHydro <ul> - <li> Support for MHD was added, but is by default disabled. + <li> Supports GR-MHD </ul> - <li> WeylScal4: OpenMP support enabled in WeylScal4 - <li> TimerReport: "top timers" now given as min/max/mean across all processes instead of just from the root process + <li> WeylScal4: parallelised via OpenMP + <li> TimerReport: "top timers" given as min/max/mean across all processes (instead of just from the root process) <li> ADMBase <ul> - <li> Variables now have flat boundary condition applied - <li> Default value of ADMBase::initial_shift is now zero rather than none + <li> ADM variables have flat boundary condition applied + <li> Shift vector has storage by default </ul> - <li> TwoPunctures: Now outputs a BBH metadata file, as used by NINJA / NRAR projects - <li> Vectors: New thorn which supports instruction vectorization to improve performance of codes that use it - <li> Cauchy Characteristic Extraction and the PITT Null Code are now included. + <li> TwoPunctures: Outputs a BBH metadata file, as used by NINJA / NRAR projects + <li> Vectors: New thorn for vectorizing code, can significantly + improve performance of codes that use it + <li> Cauchy Characteristic Extraction and the PITT Null Code are included. <ul> <li> The Pitt code implements a robust fully nonlinear characteristic evolution scheme for the Einstein equations for asymptotically flat spacetimes. <li> Included in the code is the gauge invariant calculation of the Bondi News function at future null infinity. - <li> Include in the code are thorns that implement Cauchy Characteristic extraction, where Cauchy evolutions (McLachlan) provide boundary data for a characteristic evolution. This allows for the unambiguous calculation of the gravitational waveform from merging BBH spacetimes. + <li> Included in the code are thorns that implement Cauchy Characteristic extraction, where Cauchy evolutions (McLachlan) provide boundary data for a characteristic evolution. This allows for the unambiguous calculation of the gravitational waveform from merging BBH spacetimes. </ul> <li> FFTW3 library has been added to the ET <li> Kranc <ul> - <li> thorns can now be generated including a Jacobian transformation of all derivatives - this means they can be used with multi-patch - <li> improvements to instruction vectorization - <li> can now perform finite differences using either function calls or macros; control using VECTORISE_INLINE = yes/no in optionlist; using functions can make the code fit in the instruction cache where it didn't before, resulting in large speed increases, using macros can cause compilers to run out of memory for complicated codes - <li> Generated thorns now check that there are sufficient ghost and boundary points for the finite differencing stencil used - <li> error detection has been improved + <li>Thorns can be generated including a Jacobian transformation of + all derivatives - this means they can be used with multi-patch grids + <li> Improvements to instruction vectorization + <li> Reduced instruction cache usage, selected via VECTORISE_INLINE + = yes/no in the optionlist. This can result in large speed increases. + <li> Generated thorns check that there are sufficient ghost and boundary points for the finite differencing stencils + <li> Improved error detection </ul> </ul>

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[svn:einsteintoolkit] www/about/releases/ (Rev. 741)
by knarf＠cct.lsu.edu 25 Oct '11

25 Oct '11

User: knarf Date: 2011/10/25 03:57 PM Modified: /about/releases/ ET_2011_10_announcement.php Log: fix typo File Changes: Directory: /about/releases/ =========================== File [modified]: ET_2011_10_announcement.php Delta lines: +1 -1 =================================================================== --- about/releases/ET_2011_10_announcement.php 2011-10-25 20:49:10 UTC (rev 740) +++ about/releases/ET_2011_10_announcement.php 2011-10-25 20:57:05 UTC (rev 741) @@ -1,7 +1,7 @@ <?php $title='Release Announcement'; include_once($_SERVER['DOCUMENT_ROOT'].'/global/header.php');?> -We are pleased to announce the forth release (code name "<a href="http://en.wikipedia.org/wiki/James_Clerk_Maxwell">Maxwell</a>") of the Einstein Toolkit, an open, community developed software infrastructure for relativistic astrophysics. This release includes substantial changes to the underlying AMR infrastructure Carpet and the simfactory tool. GRHydro is now officially released with support for magnetohydrodynamics. In addition, bug fixes accumulated since the previous release in April 2011 have been included. +We are pleased to announce the fourth release (code name "<a href="http://en.wikipedia.org/wiki/James_Clerk_Maxwell">Maxwell</a>") of the Einstein Toolkit, an open, community developed software infrastructure for relativistic astrophysics. This release includes substantial changes to the underlying AMR infrastructure Carpet and the simfactory tool. GRHydro is now officially released with support for magnetohydrodynamics. In addition, bug fixes accumulated since the previous release in April 2011 have been included. The Einstein Toolkit is a collection of software components and tools for simulating and analyzing general relativistic astrophysical systems that builds on numerous software efforts in the numerical relativity community including CactusEinstein, the Carpet AMR infrastructure and the relativistic hydrodynamics code GRHydro (an updated and extended version of the public release of the Whisky code). The Cactus Framework is used as the underlying computational infrastructure providing large-scale parallelization, general computational components, and a model for collaborative, portable code development. The toolkit includes modules to build complete codes for simulating black hole spacetimes as well as systems governed by relativistic hydrodynamics.

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[svn:einsteintoolkit] www/about/ (Rev. 740)
by knarf＠cct.lsu.edu 25 Oct '11

25 Oct '11

User: knarf Date: 2011/10/25 03:49 PM Modified: /about/ index.php Log: point to new release File Changes: Directory: /about/ ================== File [modified]: index.php Delta lines: +5 -5 =================================================================== --- about/index.php 2011-10-25 20:48:11 UTC (rev 739) +++ about/index.php 2011-10-25 20:49:10 UTC (rev 740) @@ -30,7 +30,7 @@ The tools and thorns comprising the Einstein Toolkit are provided in a standard Cactus - thornlist: <a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2011_05/einsteintoolki…">Einstein + thornlist: <a href="https://svn.einsteintoolkit.org/manifest/branches/ET_2011_10/einsteintoolki…">Einstein Toolkit Thornlist</a>. A <a href="http://docs.einsteintoolkit.org/et-docs/Tutorial_for_New_Users">tutorial</a> describes in easy steps how to download, compile, and run the @@ -62,9 +62,9 @@ the source code and associated tools for simulations, including Cactus thorns. The component list is written using the Component Retrieval Language and can be checked out using - the <a href="https://github.com/gridaphobe/CRL/raw/ET_2011_05/GetComponents" + the <a href="https://github.com/gridaphobe/CRL/raw/ET_2011_10/GetComponents" class="nostyle">GetComponents</a> tools. -Distribution: <a href="https://github.com/gridaphobe/CRL/raw/ET_2011_05/GetComponents">https://github.com/gridaphobe/CRL/raw/ET_2011_05/GetComponents</a> +Distribution: <a href="https://github.com/gridaphobe/CRL/raw/ET_2011_10/GetComponents">https://github.com/gridaphobe/CRL/raw/ET_2011_10/GetComponents</a> </td> </tr> @@ -82,7 +82,7 @@ resources. Distribution: CCT SVN -repository: <a href="https://svn.cct.lsu.edu/repos/numrel/simfactory/branches/ET_2011_05">https://svn.cct.lsu.edu/repos/numrel/simfactory/branches/ET_2011_05</a></td> +repository: <a href="https://svn.cct.lsu.edu/repos/numrel/simfactory2/branches/ET_2011_10">https://svn.cct.lsu.edu/repos/numrel/simfactory2/branches/ET_2011_10</a></td> </tr> <tr> @@ -104,7 +104,7 @@ the documentation for information on how to run these on the QueenBee machine. -Distribution: <a href="https://svn.einsteintoolkit.org/cactus/EinsteinExamples/branches/ET_2011_05…">https://svn.einsteintoolkit.org/cactus/EinsteinExamples/branches/ET_2011_05…</a> +Distribution: <a href="https://svn.einsteintoolkit.org/cactus/EinsteinExamples/branches/ET_2011_10…">https://svn.einsteintoolkit.org/cactus/EinsteinExamples/branches/ET_2011_10…</a> </td> </tr> </table>

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[svn:einsteintoolkit] www/about/ (Rev. 739)
by knarf＠cct.lsu.edu 25 Oct '11

25 Oct '11

User: knarf Date: 2011/10/25 03:48 PM Modified: /about/ index.php Log: remove old and outdated info File Changes: Directory: /about/ ================== File [modified]: index.php Delta lines: +0 -81 =================================================================== --- about/index.php 2011-10-25 20:46:36 UTC (rev 738) +++ about/index.php 2011-10-25 20:48:11 UTC (rev 739) @@ -109,85 +109,4 @@ </tr> </table> -<h2>Thorns moving</h2> - -A lot of components moved from one place to another in the recent - past. The following table gives an overview of the moved - components. Please note that only components are mentioned here - which either moved to the Einstein Toolkit or into Cactus. Many - other Cactus repositories moved from CVS to Subversion as well, but - stayed within Cactus itself. Those are not mentioned here. - -<h3>Cactus thorns</h3> -<table border="0"> -<tr><th>Old arrangement</th><th>Old thorn name </th><th>New arrangement </th><th>New name (if changed)</th></tr> -<tr><td>AEIThorns </td><td>AHFinderDirect </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>AEIThorns </td><td>CalcK </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>AEIThorns </td><td>Constants </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>AEIThorns </td><td>Dissipation </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>AEIThorns </td><td>EHFinder </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>AEIThorns </td><td>Exact </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>AEIThorns </td><td>Formaline </td><td>CactusUtils </td><td> </td></tr> -<tr><td>AEIThorns </td><td>Fortran </td><td>CactusBase </td><td> </td></tr> -<tr><td>AEIThorns </td><td>IDConstraintViolate</td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>AEIThorns </td><td>IDFileADM </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>AEIThorns </td><td>Nice </td><td>CactusUtils </td><td> </td></tr> -<tr><td>AEIThorns </td><td>NoExcision </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>AEIThorns </td><td>Noise </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>AEIThorns </td><td>Norms </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>AEIThorns </td><td>ReflectionSymmetry </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>AEIThorns </td><td>RotatingSymmetry180</td><td>CactusNumerical </td><td> </td></tr> -<tr><td>AEIThorns </td><td>RotatingSymmetry90 </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>AEIThorns </td><td>SphericalSurface </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>AEIThorns </td><td>TwoPunctures </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>Excision </td><td>LegoExcision </td><td>EinsteinEvolve </td><td> </td></tr> -<tr><td>PerturbedBH </td><td>DistortedBHIVP </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>PerturbedBH </td><td>IDAxiOddBrillBH </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>PerturbedBH </td><td>RotatingDBHIVP </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>BetaThorns </td><td>Cartoon2D </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>CactusBase </td><td>MoL </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>ADMAnalysis </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>ADMBase </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>ADMConstraints </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>ADMCoupling </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>ADMMacros </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>AHFinder </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>CoordGauge </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>Extract </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>HydroBase </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>IDAnalyticBH </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>CactusEinstein </td><td>IDAxiBrillBH </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>CactusEinstein </td><td>IDBrillData </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>CactusEinstein </td><td>IDLinearWaves </td><td>EinsteinInitialData</td><td> </td></tr> -<tr><td>CactusEinstein </td><td>StaticConformal </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEinstein </td><td>TmunuBase </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEOS </td><td>EOS_Base </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEOS </td><td>EOSG_Base </td><td>EinsteinBase </td><td> </td></tr> -<tr><td>CactusEOS </td><td>EOSG_Hybrid </td><td>EinsteinEOS </td><td> </td></tr> -<tr><td>CactusEOS </td><td>EOSG_IdealFluid </td><td>EinsteinEOS </td><td> </td></tr> -<tr><td>CactusEOS </td><td>EOSG_Polytrope </td><td>EinsteinEOS </td><td> </td></tr> -<tr><td>CactusEOS </td><td>EOS_Hybrid </td><td>EinsteinEOS </td><td> </td></tr> -<tr><td>CactusEOS </td><td>EOS_Ideal_Fluid </td><td>EinsteinEOS </td><td>EOS_IdealFluid</td></tr> -<tr><td>CactusEOS </td><td>EOS_Polytrope </td><td>EinsteinEOS </td><td> </td></tr> -<tr><td>CIGR_tmp </td><td>Hydro_Analysis </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>CIGR_tmp </td><td>Whisky </td><td>EinsteinEvolve </td><td>GRHydro</td></tr> -<tr><td>CIGR_tmp </td><td>Whisky_Init_Data </td><td>EinsteinInitialData</td><td>GRHydro_InitData</td></tr> -<tr><td>CIGR_tmp </td><td>Whisky_TOVSolverC </td><td>EinsteinInitialData</td><td>TOVSolver</td></tr> -<tr><td>LSUThorns </td><td>ID_Bin_BH </td><td>EinsteinInitialData</td><td>Meudon_Bin_BH</td></tr> -<tr><td>LSUThorns </td><td>ID_Bin_NS </td><td>EinsteinInitialData</td><td>Meudon_Bin_NS</td></tr> -<tr><td>LSUThorns </td><td>ID_Mag_NS </td><td>EinsteinInitialData</td><td>Meudon_Mag_NS</td></tr> -<tr><td>LSUThorns </td><td>NewRad </td><td>EinsteinEvolve </td><td> </td></tr> -<tr><td>TAT </td><td>Periodic </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>TAT </td><td>Slab </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>TAT </td><td>SlabTest </td><td>CactusNumerical </td><td> </td></tr> -<tr><td>TAT </td><td>TGRtensor </td><td>EinsteinUtils </td><td> </td></tr> -<tr><td>Waves </td><td>Multipole </td><td>EinsteinAnalysis </td><td> </td></tr> -<tr><td>Waves </td><td>WeylScal4 </td><td>EinsteinAnalysis </td><td> </td></tr> -</table> - -New arrangements within the EinteinToolkit have URLs of the form -<pre>https://svn.einsteintoolkit.org/cactus/ARRANGEMENT/THORN</pre> -and thorns within Cactus can be found using -<pre>https://svn.cactuscode.org/arrangements/ARRANGEMENT/THORN</pre>. - <?php include_once($_SERVER['DOCUMENT_ROOT'].'/global/footer.php');?>

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[svn:einsteintoolkit] www/about/releases/ (Rev. 738)
by knarf＠cct.lsu.edu 25 Oct '11

25 Oct '11

User: knarf Date: 2011/10/25 03:46 PM Modified: /about/releases/ ET_2011_10_announcement.php Log: fix date File Changes: Directory: /about/releases/ =========================== File [modified]: ET_2011_10_announcement.php Delta lines: +1 -1 =================================================================== --- about/releases/ET_2011_10_announcement.php 2011-10-25 20:45:39 UTC (rev 737) +++ about/releases/ET_2011_10_announcement.php 2011-10-25 20:46:36 UTC (rev 738) @@ -137,6 +137,6 @@    Eric Seidel -April 21, 2011 +October 25, 2011 <?php include_once($_SERVER['DOCUMENT_ROOT'].'/global/footer.php');?>

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[svn:einsteintoolkit] www/ (Rev. 737)
by knarf＠cct.lsu.edu 25 Oct '11

25 Oct '11

User: knarf Date: 2011/10/25 03:45 PM Modified: / index.php Log: mention new release on main page File Changes: Directory: / ============ File [modified]: index.php Delta lines: +4 -4 =================================================================== --- index.php 2011-10-25 20:44:03 UTC (rev 736) +++ index.php 2011-10-25 20:45:39 UTC (rev 737) @@ -13,10 +13,10 @@ <a class = "downloadbutton" href = "download/">Download</a> -April 2011: We are pleased to -<a href="about/releases/ET_2011_05_announcement.php">announce the -third release</a> (code name -"<a href="http://en.wikipedia.org/wiki/Marie_Curie">Curie</a>") +October 2011: We are pleased to +<a href="about/releases/ET_2011_10_announcement.php">announce the +forth release</a> (code name +"<a href="http://en.wikipedia.org/wiki/James_Clerk_Maxwell">Maxwell</a>") of the Einstein Toolkit, an open, community developed software infrastructure for relativistic astrophysics.

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