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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 234)
by gallen＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: gallen Date: 2011/11/14 11:22 AM Modified: / ET.tex Log: affiliation and word changes in intro File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +15 -14 =================================================================== --- ET.tex 2011-11-14 17:14:47 UTC (rev 233) +++ ET.tex 2011-11-14 17:22:34 UTC (rev 234) @@ -88,7 +88,7 @@ Bruno C. Mundim $^2$, Christian D. Ott $^{5,1,6}$, Erik Schnetter $^{7,8,1}$, -Gabrielle Allen $^1$, +Gabrielle Allen $^{1,9,10}$, Manuela Campanelli $^2$ and Pablo Laguna $^4$} @@ -103,6 +103,8 @@ ON, Canada} \address{$^8$ Department of Physics, University of Guelph, Guelph, ON, Canada} +\address{$^9$ Department of Computer Science, Louisiana State University, Baton Rouge, LA, USA} +\address{$^{10}$ National Science Foundation, USA} \ead{knarf(a)cct.lsu.edu} %\thanks{{}$^{(1)}$ Department of Computer Science, @@ -122,10 +124,10 @@ We describe the Einstein Toolkit, a community-driven, freely accessible computational infrastructure intended for use in numerical relativity, relativistic astrophysics, and other applications. The Toolkit, developed by a -collaboration involving researchers from several institutions around the world, +collaboration involving researchers from multiple institutions around the world, combines a core set of components needed to simulate astrophysical objects such as black holes, compact objects, and collapsing stars, as well as a full suite -of analysis tools. The Einstein Toolkit is based on the Cactus Framework for +of analysis tools. The Einstein Toolkit is currently based on the Cactus Framework for high-performance computing and the Carpet adaptive mesh refinement driver. It implements spacetime evolution via the BSSN evolution system and general-relativistic hydrodynamics in a finite-volume discretization. The @@ -157,13 +159,13 @@ in the study of astrophysical systems containing black holes (BHs) 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, +advances over the next few years~\cite{Shibata:1999wm,Shibata:2002jb, 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 +much more difficult to evolve numerically until 2005. That year, computational +breakthroughs were made following the development of 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 +that lead to the first stable long-term evolutions of moving single and multiple BH systems. These results quickly transformed the field which was now able to effectively evolve the Einstein field equations for coalescing BH-BH binaries and other systems containing moving @@ -238,15 +240,14 @@ Simultaneously with the advances in both our physical understanding of relativistic dynamics and the numerical techniques required to study them, -a set of computational tools and libraries has been developed with the +a set of general computational tools and libraries has been developed with the aim of providing a computational core that can enable new science, -broaden the community, facilitate interdisciplinary research and take +broaden the community, facilitate collaborative and interdisciplinary research, promote software reuse and take advantage of emerging petascale computers and advanced cyberinfrastructure: -the Cactus computational toolkit~\cite{Cactuscode:web}. While it was -developed in large part by computer scientists, its development was driven by -direct input from other fields, especially numerical relativity, and has -succeeded in applying expertise in computer science directly to problems in -numerical relativity. +the Cactus computational toolkit~\cite{Cactuscode:web}. +Although the development of Cactus was driven directly from the numerical relativity community, it was developed in collaboration +with computer scientists and other computational fields to facilitate the incorporation of innovations in computational +theory and technology. This success prompted usage of the {\tt Cactus} computational toolkit in other areas, such as ocean forecast models~\cite{Djikstra2005} and chemical reaction

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 233)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 11:14 AM Modified: / ET.tex Log: spellcheck File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +14 -14 =================================================================== --- ET.tex 2011-11-14 17:03:30 UTC (rev 232) +++ ET.tex 2011-11-14 17:14:47 UTC (rev 233) @@ -293,7 +293,7 @@ attacked directly with fewer potential infrastructure problems, one of the goals of the Einstein Toolkit. -While the Einstein Toolkit does have a large group of users, many of themdo not directly collaborate on science problems, and some compete. +While the Einstein Toolkit does have a large group of users, many of them do not directly collaborate on science problems, and some compete. However, all groups agree that sharing the development of the underlying infrastructure is mutually beneficial for every group and the wider community as well. This is achieved by lifting off the research groups' shoulders much of the @@ -347,7 +347,7 @@ starting with code generation all to way to archiving of simulation results: (i) the {\tt Cactus} framework ``flesh'' provides the underlying infrastructure to build complex simulation codes out of independently -developed modules and facillates communication between these modules. (ii) the +developed modules and facilities communication between these modules. (ii) the adaptive mesh refinement driver, {\tt Carpet}, is build on top of {\tt Cactus} and provides problem independent adaptive mesh refinement support for simulations that need to resolve physics on length scales differing by many @@ -355,7 +355,7 @@ internal details of the mesh refinement driver. (iii) {\tt Kranc}, which generates code in a computer language from a high-level description in Mathematica and (iv) the Simulation Factory, which provides a uniform, high-level interface to -common operations, such submisson and restart of jobs, for a large number of +common operations, such as submission and restart of jobs, for a large number of compute clusters. \subsection{Cactus Framework} @@ -395,13 +395,13 @@ group continues to be comprised of numerical relativists. It is not surprising therefore, that one of the science modules provided in the Einstein Toolkit is a set of state of the art modules to simulate binary -black hole mergers. All modules to simulate and analyse the data are provided +black hole mergers. All modules to simulate and analyze the data are provided out of the box. This set of modules also provides a way of testing the Einstein Toolkit modules in a production type simulation rather than synthetic test cases. Some of these modules have been developed specifically for the Einstein Toolkit while others are modules used in previous publications and have been contributed to the toolkit. In these cases the Einstein Toolkit -provides documenation and best practise guidelines for the contributed modules. +provides documentation and best practice guidelines for the contributed modules. \subsection{Adaptive Mesh Refinement} @@ -485,7 +485,7 @@ This shows the time required per grid point, where smaller numbers are better (the ideal scaling is a horizontal line). This - demonstrates excellect scalability to up to more than 10,000 + demonstrates excellent scalability to up to more than 10,000 cores. Including hydrodynamics approximately doubles calculation times without negatively influencing scalability.} \label{fig:weak-scaling} @@ -509,7 +509,7 @@ Today's supercomputers differ significantly in their hardware configuration, available software, directory structure, -queueing system, queuing policy, and many other user-visible +queuing system, queuing policy, and many other user-visible properties. In addition, the system architectures and user interfaces offered by supercomputers are very different from those offered by laptops or workstations. This makes performing large, @@ -988,7 +988,7 @@ it to extend to spatial infinity. Within each of the nested sub-domains, fields are decomposed into Chebyshev modes radially and into spherical harmonics in the angular directions, with elliptic equation solving reduced to a matrix -problem. The nested sub-domains ineen not be perfectly spherical, and +problem. The nested sub-domains need not be perfectly spherical, and indeed one may modify the outer boundaries of each to cover any convex shape. For NSs, this allows one to map the surface of a particular sub-domain to the NS surface, minimizing Gibbs error there. For BHs, excision @@ -1873,7 +1873,7 @@ on a Schwarzschild background or the calculation of the Weyl scalar $\Psi_4$. The module \codename{Extract} uses the Moncrief formalism~\cite{ -Moncrief:1974am} to extract gauge-invariant wavefunctions $Q_{\ell m}^\times$ and $Q_{\ell +Moncrief:1974am} to extract gauge-invariant wave functions $Q_{\ell m}^\times$ and $Q_{\ell m}^+$ given spherical surfaces of constant coordinate radius. The spatial metric is expressed as a perturbation on Schwarzschild and expanded into a tensor basis of @@ -1951,8 +1951,8 @@ While the waveforms generated by \codename{Extract} are already decomposed on a convenient basis to separate modes, the complex quantity $\Psi_4$ is provided by \codename{WeylScal4} as -a complex gridfunction. For this quantity, and any other real or -complex gridfunction, the module \codename{Multipole} interpolates +a complex grid function. For this quantity, and any other real or +complex grid function, the module \codename{Multipole} interpolates the field $u(t,r,\theta,\phi)$ onto coordinate spheres of given radii and calculates the coefficients \begin{equation} @@ -1979,7 +1979,7 @@ \frac{d x^i}{d t} = -\beta^i, \label{eq:puncturetracking} \end{equation} where $x^i$ is the puncture location and $\beta^i$ is the shift. Since the -puncture location usually does not coincide with gridpoints, the shift is +puncture location usually does not coincide with grid points, the shift is interpolated to the location of the puncture. Equation~(\eref{eq:puncturetracking}) is implemented with a simple first-order Euler scheme, accurate enough for controlling the location @@ -2192,7 +2192,7 @@ \section{Examples} \todo{Update if necessary} -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 datafiles 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, +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. 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}). @@ -2871,7 +2871,7 @@ by the Cauchy Characteristic Extraction (CCE) technique recently studied in~\cite{Babiuc:11,Reisswig:2010cd,Reisswig:2011a}. The authors of one such CCE code~\cite{Babiuc:11} have agreed to make their work available to the -whole community by integrating their CCE routines into the Einstein Tookit +whole community by integrating their CCE routines into the Einstein Toolkit release 2011\_11 ``Maxwell,'' which will be described elsewhere. A second much needed improvement of our existing methods

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 232)
by diener＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: diener Date: 2011/11/14 11:03 AM Modified: / ET.tex Log: Fix the caption to figure 12. File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +5 -4 =================================================================== --- ET.tex 2011-11-14 16:57:34 UTC (rev 231) +++ ET.tex 2011-11-14 17:03:30 UTC (rev 232) @@ -2322,11 +2322,12 @@ \begin{figure} \includegraphics[width=0.9\textwidth]{examples/kerr/figs/qlm_mass} \includegraphics[width=0.9\textwidth]{examples/kerr/figs/qlm_spin} - \caption{The top plot shows the total mass and the right plot shows the changing spin (i.e.\ $\Delta S=S(t)-S(t=0)$ of the BH as a function of time. + \caption{The top plot shows the total mass and the bottom plot shows the change in spin (i.e.\ $\Delta S=S(t)-S(t=0)$ of the BH as a function of time. In both plots the black (solid) curve is for high, blue (dashed) for medium -and red (dotted) for low resolution. In the right plot the green (dash-dotted) -curve shows the high resolution result scaled for second-order convergence with -the medium resolution.} +and red (dotted) for low resolution. In the bottom plot the green (dash-dotted) +curve shows the high resolution result scaled for second-order convergence. The +agreement with the medium resolution curve shows that the change in spin +converges to zero as expected.} \label{fig:ah_mass_spin} \end{figure} In both cases the black (solid) curve is for high, blue (dashed) for medium and

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 231)
by diener＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: diener Date: 2011/11/14 10:57 AM Modified: / ET.tex Log: Fix equation 28. File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +3 -2 =================================================================== --- ET.tex 2011-11-14 16:54:11 UTC (rev 230) +++ ET.tex 2011-11-14 16:57:34 UTC (rev 231) @@ -1124,8 +1124,9 @@ \nonumber\\ & & {} - 2\tilde{A}^{ij}\partial_j\alpha + 2\alpha\left[ (m-1)\partial_k\tilde{A}^{ki} - \frac{2m}{3}\tilde{D}^i K - + m(\tilde{\Gamma}^i_{\; kl}\tilde{A}^{kl} + 6\tilde{A}^{ij}\partial_j\phi) - \right] - S^i, + \right. \nonumber \\ + & & {} + m(\tilde{\Gamma}^i_{\; kl}\tilde{A}^{kl} + + 6\tilde{A}^{ij}\partial_j\phi) \Bigg] - S^i, \end{eqnarray} \end{widetext} with the momentum constraint damping constant set to $m=1$. The stress

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 230)
by jfaber＠einsteintoolkit.org 14 Nov '11

14 Nov '11

User: jfaber Date: 2011/11/14 10:54 AM Modified: / iopart-num-edit.bst Log: Print proceedings titles in the refs File Changes: Directory: / ============ File [modified]: iopart-num-edit.bst Delta lines: +3 -1 =================================================================== --- iopart-num-edit.bst 2011-11-14 16:47:53 UTC (rev 229) +++ iopart-num-edit.bst 2011-11-14 16:54:11 UTC (rev 230) @@ -75,7 +75,8 @@ % cited in the text, or that in the database. %--------------------------------------------------------------------- % - % Hacked so that titles are printed for Journal articles and so that + % Hacked so that titles are printed for Journal articles, so that + % article titles show up in conferences procs., and so that % we print eprint information only if the journal field is empty % % The latter is accomplished by the following commands: @@ -1464,6 +1465,7 @@ format.authors "author" output.check format.date "year" output.check date.block + format.title "title" output.check crossref missing$ {

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 133)
by jfaber＠einsteintoolkit.org 14 Nov '11

14 Nov '11

User: jfaber Date: 2011/11/14 10:50 AM Modified: /trunk/ einsteintoolkit.bib Log: Deleting duplicate ref File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.bib Delta lines: +0 -15 =================================================================== --- trunk/einsteintoolkit.bib 2011-11-14 16:44:00 UTC (rev 132) +++ trunk/einsteintoolkit.bib 2011-11-14 16:50:30 UTC (rev 133) @@ -1822,21 +1822,6 @@ primaryClass = "gr-qc", } -@Article{Lousto:2010ut, - author = "Lousto, Carlos O. and Zlochower, Yosef", - title = "{Orbital Evolution of Extreme-Mass-Ratio Black-Hole - Binaries with Numerical Relativity}", - journal = "Phys. Rev. Lett.", - volume = "106", - year = "2011", - pages = "041101", - eprint = "1009.0292", - archivePrefix = "arXiv", - primaryClass = "gr-qc", - doi = "10.1103/PhysRevLett.106.041101", - SLACcitation = "%%CITATION = 1009.0292;%%" -} - ##M ############################################################################ @article{Manca:2007ca,

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 229)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 10:47 AM Modified: / ET.tex Log: reorder affiliations File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +5 -5 =================================================================== --- ET.tex 2011-11-14 16:44:55 UTC (rev 228) +++ ET.tex 2011-11-14 16:47:53 UTC (rev 229) @@ -86,8 +86,8 @@ Roland Haas $^{5,4}$, Ian Hinder $^3$, Bruno C. Mundim $^2$, -Christian D. Ott $^{5,1,8}$, -Erik Schnetter $^{6,7,1}$, +Christian D. Ott $^{5,1,6}$, +Erik Schnetter $^{7,8,1}$, Gabrielle Allen $^1$, Manuela Campanelli $^2$ and Pablo Laguna $^4$} @@ -98,11 +98,11 @@ \address{$^3$ Max-Planck-Institut f\"{u}r Gravitationsphysik, Albert-Einstein-Institut, Golm, Germany} \address{$^4$ Center for Relativistic Astrophysics, School of Physics, Georgia Institute of Technology, Atlanta, GA, USA} \address{$^5$ TAPIR, California Institute of Technology, Pasadena, CA, USA} -\address{$^6$ Perimeter Institute for Theoretical Physics, Waterloo, +\address{$^6$ Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Japan} +\address{$^7$ Perimeter Institute for Theoretical Physics, Waterloo, ON, Canada} -\address{$^7$ Department of Physics, University of Guelph, Guelph, ON, +\address{$^8$ Department of Physics, University of Guelph, Guelph, ON, Canada} -\address{$^8$ Institute for the Physics and Mathematics of the Universe, University of Tokyo, Kashiwa, Japan} \ead{knarf(a)cct.lsu.edu} %\thanks{{}$^{(1)}$ Department of Computer Science,

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 228)
by jfaber＠einsteintoolkit.org 14 Nov '11

14 Nov '11

User: jfaber Date: 2011/11/14 10:44 AM Modified: / iopart-num-edit.bst Log: Fix journal vs. preprint formatting in reference list see the file header for the changes from iopart-num.bst as available online File Changes: Directory: / ============ File [modified]: iopart-num-edit.bst Delta lines: +21 -4 =================================================================== --- iopart-num-edit.bst 2011-11-14 16:40:05 UTC (rev 227) +++ iopart-num-edit.bst 2011-11-14 16:44:55 UTC (rev 228) @@ -74,7 +74,16 @@ % The order in the reference list is that by which the works were originally % cited in the text, or that in the database. %--------------------------------------------------------------------- - + % + % Hacked so that titles are printed for Journal articles and so that + % we print eprint information only if the journal field is empty + % + % The latter is accomplished by the following commands: + % journal empty$ + % { format.eprint output } + % { skip$ } + % if$ + % ENTRY { address archive @@ -1303,7 +1312,7 @@ %mc emphasize %mc "journal" output.check %mc add.blank - journal + journal "journal" bibinfo.check section field.or.null strip.trailing trim emphasize @@ -1313,6 +1322,7 @@ { skip$ } { section * add.blank} if$ + %mc end format.vol.num.pages output } @@ -1322,8 +1332,15 @@ if$ format.issn output format.note output -% format.eprint output +%% format.eprint output format.url output + + journal empty$ + { format.eprint output } + { skip$ } + if$ + + fin.entry } FUNCTION {book} @@ -1354,7 +1371,7 @@ %% format.edition output format.isbn output format.note output - format.eprint output +%% format.eprint output format.url output fin.entry }

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 132)
by jfaber＠einsteintoolkit.org 14 Nov '11

14 Nov '11

User: jfaber Date: 2011/11/14 10:44 AM Modified: /trunk/ einsteintoolkit.bib Log: Added four refs File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.bib Delta lines: +81 -19 =================================================================== --- trunk/einsteintoolkit.bib 2011-11-14 16:12:37 UTC (rev 131) +++ trunk/einsteintoolkit.bib 2011-11-14 16:44:00 UTC (rev 132) @@ -51,8 +51,17 @@ "key" entry that specifies where this entry should appear in an alphabetically sorted list. - - +The following BST file hack works nicely for getting eprints +into a paper when the "journal" field is empty: +# journal empty$ +# { format.eprint output} +# { skip$ } +# if$ +In short, noting that a stack-based language is used, we first +put the journal name, if any, onto the stack, and query if it is empty -- +note that if commands occur after the "then" and "else" blocks, not before +If there is no journal entry, we print the eprint according to the format +If there is a journal entry, we skip over the branch and suppress the eprint info ##A ############################################################################ @Article{Ajith:2007kx, @@ -209,6 +218,34 @@ {http://www.slac.stanford.edu/spires/find/hep/www?rawcmd=find+doi+10.1103/PhysRevLett.100.191101}, } +@Article{Anninos:1995am, + author = "Anninos, Peter and others", + title = "{Three-dimensional numerical relativity: The Evolution of + black holes}", + journal = "Phys. Rev. D", + volume = "52", + year = "1995", + pages = "2059-2082", + eprint = "gr-qc/9503025", + doi = "10.1103/PhysRevD.52.2059", + SLACcitation = "%%CITATION = GR-QC/9503025;%%" +} + +@Article{Anninos:1996ai, + author = "Anninos, Peter and Masso, Joan and Seidel, Edward and Suen, + Wai-Mo and Tobias, Malcolm", + title = "{Dynamics of gravitational waves in 3D: Formulations, + methods, and tests}", + journal = "Phys. Rev. D", + volume = "56", + year = "1997", + pages = "842-858", + eprint = "gr-qc/9610057", + doi = "10.1103/PhysRevD.56.842", + SLACcitation = "%%CITATION = GR-QC/9610057;%%" +} + + @Article{Anninos:1996ez, author = {Peter Anninos and Karen Camarda and Joseph Libson and Joan Mass{'o} and Edward Seidel and Wai-Mo Suen}, @@ -553,7 +590,7 @@ year = 1984, } -@misc{Bernuzzi:2011aq, +@article{Bernuzzi:2011aq, author = "Bernuzzi, Sebastiano and Thierfelder, Marcus and Bruegmann, Bernd", title = "{Accuracy of numerical relativity waveforms from binary @@ -1171,7 +1208,7 @@ eprint = "arXiv:1007.4203 [astro-ph.HE]", } -@misc{Foucart:2011mz, +@article{Foucart:2011mz, author = "Foucart, Francois and Duez, Matthew D. and Kidder, Lawrence E. and Scheel, Mark A. and Szilagyi, Bela and others", @@ -1257,7 +1294,7 @@ url = {http://edoc.mpg.de/3341}, } -@misc{Gold:2011df, +@article{Gold:2011df, author = "Gold, Roman and Bernuzzi, Sebastiano and Thierfelder, Marcus and Bruegmann, Bernd and Pretorius, Frans", title = "{Eccentric binary neutron star mergers}", @@ -1670,7 +1707,7 @@ } ##L ############################################################################ -@misc{Lackey:2011vz, +@article{Lackey:2011vz, author = "Lackey, Benjamin D. and Kyutoku, Koutarou and Shibata, Masaru and Brady, Patrick R. and Friedman, John L.", title = "{Extracting equation of state parameters from black @@ -1690,7 +1727,7 @@ year = 1991, } -@misc{Lechner:2004cs, +@article{Lechner:2004cs, author = {{Lechner}, C. and {Alic}, D. and {Husa}, S.}, title = "{From Tensor Equations to Numerical Code -- Computer Algebra Tools for Numerical Relativity}", eprint = {arXiv:cs/0411063}, @@ -1757,6 +1794,18 @@ SLACcitation = "%%CITATION = 0805.0159;%%" } +@article{Lousto:2010ut, + author = "Lousto, Carlos O. and Zlochower, Yosef", + title = "{Orbital Evolution of Extreme-Mass-Ratio Black-Hole + Binaries with Numerical Relativity}", + journal = "Phys. Rev. Lett.", + volume = "106", + pages = "041101", + doi = "10.1103/PhysRevLett.106.041101", + year = "2011", + eprint = "1009.0292", + } + @article{Lovelace:2009dg, author = "Lovelace, Geoffrey and Chen, Yanbei and Cohen, Michael and Kaplan, Jeffrey D. and Keppel, Drew and others", @@ -2224,6 +2273,19 @@ eprint = "arXiv:1003.0859 [gr-qc]", } +@Article{Seidel:1999ey, + author = "Seidel, Edward and Suen, Wai-Mo", + title = "{Numerical Relativity As A Tool For Computational + Astrophysics}", + journal = "J. Comput. Appl. Math", + volume = 109, + pages = "493-525", + doi = "10.1016/S0377-0427(99)00169-7", + year = "1999", + eprint = "gr-qc/9904014", + SLACcitation = "%%CITATION = GR-QC/9904014;%%" +} + @article{Sekiguchi:2011zd, author = "Sekiguchi, Yuichiro and Kiuchi, Kenta and Kyutoku, Koutarou and Shibata, Masaru", @@ -2239,7 +2301,7 @@ doi = {10.1103/PhysRevLett.107.051102}, } -@misc{Sekiguchi:2011mc, +@article{Sekiguchi:2011mc, author = "Sekiguchi, Yuichiro and Kiuchi, Kenta and Kyutoku, Koutarou and Shibata, Masaru", title = "{Effects of hyperons in binary neutron star mergers}", @@ -2247,17 +2309,6 @@ eprint = "arXiv:1110.4442", } -@article{Shibata:1995we, - author = "Shibata, Masaru and Nakamura, Takashi", - title = "{Evolution of three-dimensional gravitational waves: - Harmonic slicing case}", - journal = "Phys. Rev. D", - volume = "52", - pages = "5428-5444", - doi = "10.1103/PhysRevD.52.5428", - year = "1995", -} - @Article{Shen:1998by, author = "Shen, H. and Toki, H. and Oyamatsu, K. and Sumiyoshi, K.", @@ -2284,6 +2335,17 @@ eprint = "arXiv:nucl-th/9805035", } +@article{Shibata:1995we, + author = "Shibata, Masaru and Nakamura, Takashi", + title = "{Evolution of three-dimensional gravitational waves: + Harmonic slicing case}", + journal = "Phys. Rev. D", + volume = "52", + pages = "5428-5444", + doi = "10.1103/PhysRevD.52.5428", + year = "1995", +} + @article{Shibata:1998sg, author = "Shibata, Masaru and Baumgarte, Thomas W. and Shapiro, Stuart L.",

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/examples/cosmology/figs/ (Rev. 227)
by eloisa.bentivegna＠aei.mpg.de 14 Nov '11

14 Nov '11

User: bentivegna Date: 2011/11/14 10:40 AM Modified: /examples/cosmology/figs/ err.pdf, kasner.pdf, kasner.py Log: Corrected factors in convergence study of Kasner. File Changes: Directory: /examples/cosmology/figs/ ==================================== File [modified]: err.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [modified]: kasner.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [modified]: kasner.py Delta lines: +3 -3 =================================================================== --- examples/cosmology/figs/kasner.py 2011-11-14 16:36:17 UTC (rev 226) +++ examples/cosmology/figs/kasner.py 2011-11-14 16:40:05 UTC (rev 227) @@ -38,10 +38,10 @@ axb = figb.add_subplot(1,1,1) # plot -axb.plot(t, (ord1-exa1)/16**3, linestyle='-', color='black', label='$\gamma_{xx}^n-\gamma_{xx}^e$') -axb.plot(t, (ord1m[::2]-exa1)/16**2, linestyle='--', color='blue', label='$\gamma_{xx}^n-\gamma_{xx}^e$') -axb.plot(t, (ord1h[::4]-exa1)/16, linestyle='-.', color='black', label='$\gamma_{xx}^n-\gamma_{xx}^e$') axb.plot(t, (ord1hh[::8]-exa1), linestyle=':', color='blue', label='$\gamma_{xx}^n-\gamma_{xx}^e$') +axb.plot(t, (ord1h[::4]-exa1)/16, linestyle='-.', color='black', label='$(\gamma_{xx}^n-\gamma_{xx}^e)/16$') +axb.plot(t, (ord1m[::2]-exa1)/16**2, linestyle='--', color='blue', label='$(\gamma_{xx}^n-\gamma_{xx}^e)/16^2$') +axb.plot(t, (ord1-exa1)/16**3, linestyle='-', color='black', label='$(\gamma_{xx}^n-\gamma_{xx}^e)/16^3$') axb.set_xlabel(r'$t$')

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