Commits November 2011

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13 participants
183 discussions

[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 244)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 02:22 PM Added: / arXiv.tar.gz Modified: / make_arXiv.sh Log: archive tarball Directory Changes: Directory: /svn:mime-type/ ========================== + application/octet-stream File Changes: Directory: / ============ File [added]: arXiv.tar.gz Delta lines: +0 -0 =================================================================== (Binary files differ) Property changes on: arXiv.tar.gz ___________________________________________________________________ File [modified]: make_arXiv.sh Delta lines: +0 -1 =================================================================== --- make_arXiv.sh 2011-11-14 19:52:47 UTC (rev 243) +++ make_arXiv.sh 2011-11-14 20:22:04 UTC (rev 244) @@ -13,7 +13,6 @@ cp -a \ figures/*.pdf\ - figures/*.png\ cactus-benchmarks/results-best.pdf\ examples/kerr/figs/waves.pdf\ examples/kerr/figs/waves_conv.pdf\

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 243)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 01:52 PM Removed: /figures/ err.png, kasner.png Modified: / make_arXiv.sh Log: remove unused figures File Changes: Directory: / ============ File [modified]: make_arXiv.sh Delta lines: +4 -1 =================================================================== --- make_arXiv.sh 2011-11-14 19:44:19 UTC (rev 242) +++ make_arXiv.sh 2011-11-14 19:52:47 UTC (rev 243) @@ -12,7 +12,8 @@ arXiv/ cp -a \ - figures/*\ + figures/*.pdf\ + figures/*.png\ cactus-benchmarks/results-best.pdf\ examples/kerr/figs/waves.pdf\ examples/kerr/figs/waves_conv.pdf\ @@ -35,3 +36,5 @@ examples/cosmology/figs/err.pdf\ \ arXiv/figures/ + +tar -czf arXiv.tar.gz arXiv/ Directory: /figures/ ==================== File [removed]: err.png Delta lines: +0 -0 =================================================================== (Binary files differ) File [removed]: kasner.png Delta lines: +0 -0 =================================================================== (Binary files differ)

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 242)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 01:44 PM Modified: / make_arXiv.sh Log: fix script File Changes: Directory: / ============ File [modified]: make_arXiv.sh Delta lines: +6 -3 =================================================================== --- make_arXiv.sh 2011-11-14 19:37:18 UTC (rev 241) +++ make_arXiv.sh 2011-11-14 19:44:19 UTC (rev 242) @@ -1,6 +1,6 @@ #!/bin/bash rm -rf arXiv -mkdir arXiv +mkdir -p arXiv/figures cp -a \ ET.tex\ ET.bbl\ @@ -9,7 +9,10 @@ iopams.sty\ widetext.sty\ iopart-num-edit.bst\ - figures\ + arXiv/ + +cp -a \ + figures/*\ cactus-benchmarks/results-best.pdf\ examples/kerr/figs/waves.pdf\ examples/kerr/figs/waves_conv.pdf\ @@ -31,4 +34,4 @@ examples/cosmology/figs/kasner.pdf\ examples/cosmology/figs/err.pdf\ \ - arXiv/ + arXiv/figures/

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 241)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 01:37 PM Added: / make_arXiv.sh Log: add small script to select sources for the arXiv Directory Changes: Directory: /svn:executable/ =========================== + * File Changes: Directory: / ============ File [added]: make_arXiv.sh Delta lines: +34 -0 =================================================================== --- make_arXiv.sh (rev 0) +++ make_arXiv.sh 2011-11-14 19:37:18 UTC (rev 241) @@ -0,0 +1,34 @@ +#!/bin/bash +rm -rf arXiv +mkdir arXiv +cp -a \ + ET.tex\ + ET.bbl\ + iopart.cls\ + iopart12.clo\ + iopams.sty\ + widetext.sty\ + iopart-num-edit.bst\ + figures\ + cactus-benchmarks/results-best.pdf\ + examples/kerr/figs/waves.pdf\ + examples/kerr/figs/waves_conv.pdf\ + examples/kerr/figs/waves_l4.pdf\ + examples/kerr/figs/waves_l4_conv.pdf\ + examples/kerr/figs/ah_mass.pdf\ + examples/kerr/figs/ah_mass_conv.pdf\ + examples/kerr/figs/qlm_mass.pdf\ + examples/kerr/figs/qlm_spin.pdf\ + examples/bbh/figs/tracks.pdf\ + examples/bbh/figs/mp_psi4_l2_m2_r60.pdf\ + examples/bbh/figs/amp_convergence_all_8th.pdf\ + examples/bbh/figs/phase_convergence_all_8th.pdf\ + examples/tov/rho_max.pdf\ + examples/tov/mode_spectrum.pdf\ + examples/tov/ham_conv.pdf\ + examples/collapse/radii.pdf\ + examples/collapse/H_convergence_at0.pdf\ + examples/cosmology/figs/kasner.pdf\ + examples/cosmology/figs/err.pdf\ + \ + arXiv/ Property changes on: make_arXiv.sh ___________________________________________________________________

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 240)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 01:34 PM Modified: / ET.tex Log: don't specify paths to figures in \includegraphics File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +30 -23 =================================================================== --- ET.tex 2011-11-14 19:05:49 UTC (rev 239) +++ ET.tex 2011-11-14 19:34:05 UTC (rev 240) @@ -30,7 +30,14 @@ \usepackage[sort&compress,numbers]{natbib} \renewcommand{\bibfont}{\footnotesize} -\graphicspath{{figures/}} +\graphicspath{{figures/} +{cactus-benchmarks/} +{examples/kerr/figs/} +{examples/bbh/figs/} +{examples/tov/} +{examples/collapse/} +{examples/cosmology/figs/} +} \setcounter{secnumdepth}{5} @@ -457,9 +464,9 @@ \begin{figure} \centering - \includegraphics[width=0.3\textwidth]{figures/carpet-timestepping} + \includegraphics[width=0.3\textwidth]{carpet-timestepping} \hspace{3em} - \includegraphics[width=0.3\textwidth]{figures/carpet-interpolation} + \includegraphics[width=0.3\textwidth]{carpet-interpolation} \caption{Berger-Oliger time stepping details, showing a coarse and a fine grid, with time advancing upwards. \textbf{Left:} Time stepping algorithm. First the coarse grid takes a large time step, then the @@ -476,7 +483,7 @@ used in production on up to several thousand cores~\cite{Reisswig:2010cd,Lousto:2010ut}. \begin{figure} \centering - \includegraphics[width=0.85\textwidth]{cactus-benchmarks/results-best} + \includegraphics[width=0.85\textwidth]{results-best} \caption{Results from weak scaling tests evolving the Einstein equations on a mesh refinement grid structure with nine levels. This shows the time required per grid point, @@ -2214,8 +2221,8 @@ Figure~\ref{fig:kerr_waves} shows the $\ell =2, m=0$ mode of $r\Psi_4$ extracted at $R=30M$, and its numerical convergence. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/waves} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/waves_conv} + \includegraphics[width=0.9\textwidth]{waves} + \includegraphics[width=0.9\textwidth]{waves_conv} \caption{The extracted $\ell =2, m=0$ mode of $\Psi_4$ as function of time from the high resolution run (top plot). The extraction was done at $R=30M$. Shown is both the real (solid black curve) and the @@ -2242,8 +2249,8 @@ Figure~\ref{fig:kerr_waves_l4} shows similar plots for the $\ell =4, m=0$ mode of $r\Psi_4$, again extracted at $R=30 M$. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/waves_l4} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/waves_l4_conv} + \includegraphics[width=0.9\textwidth]{waves_l4} + \includegraphics[width=0.9\textwidth]{waves_l4_conv} \caption{Real part of the extracted $\ell =4, m=0$ mode of $\Psi_4$ as function of time (top plot) for the high (solid black curve), medium (dashed blue curve) and low (dotted red @@ -2279,8 +2286,8 @@ \codename{AHFinderDirect} as a function of time at the high (black solid curve), medium (blue dashed curve) and low (red dotted curve) resolutions. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/ah_mass} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/ah_mass_conv} + \includegraphics[width=0.9\textwidth]{ah_mass} + \includegraphics[width=0.9\textwidth]{ah_mass_conv} \caption{The top plot shows the irreducible mass of the apparent horizon as a function of time at low (black solid curve), medium (blue dashed curve) and high (red dotted curve) resolutions. The inset is a zoom in on the @@ -2311,8 +2318,8 @@ mass (top plot) and the change in the spin, $\Delta S = S(t) - S(t=0)$, as calculated by \codename{QuasiLocalMeasures}. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/qlm_mass} - \includegraphics[width=0.9\textwidth]{examples/kerr/figs/qlm_spin} + \includegraphics[width=0.9\textwidth]{qlm_mass} + \includegraphics[width=0.9\textwidth]{qlm_spin} \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 bottom plot the green (dash-dotted) @@ -2502,8 +2509,8 @@ templates. \begin{figure} - \includegraphics[width=0.45\textwidth]{examples/bbh/figs/tracks} - \includegraphics[width=0.45\textwidth]{examples/bbh/figs/mp_psi4_l2_m2_r60} + \includegraphics[width=0.45\textwidth]{tracks} + \includegraphics[width=0.45\textwidth]{mp_psi4_l2_m2_r60} \caption{In the left panel, we plot the tracks corresponding to the evolution of two punctures initially located on the $x$-axis at $x=\pm 3$. The solid blue line represents puncture 1, and the dashed red line @@ -2517,8 +2524,8 @@ \end{figure} \begin{figure} - \includegraphics[width=0.45\textwidth]{examples/bbh/figs/amp_convergence_all_8th} - \includegraphics[width=0.45\textwidth]{examples/bbh/figs/phase_convergence_all_8th} + \includegraphics[width=0.45\textwidth]{amp_convergence_all_8th} + \includegraphics[width=0.45\textwidth]{phase_convergence_all_8th} \caption{Weyl scalar amplitude (left panel) and phase (right panel) convergence. The long dashed red curves represent the difference between the medium and low-resolution runs. The short dashed orange curves show @@ -2574,7 +2581,7 @@ \begin{figure} \label{fig:tov_rho_max} - \includegraphics[width=0.9\textwidth]{examples/tov/rho_max} + \includegraphics[width=0.9\textwidth]{rho_max} \caption{Evolution of the central density for the TOV star. Clearly visible is an initial spike, produced by the interpolation of the one-dimensional equilibrium solution onto the three-dimensional evolution grid. The remainder of the evolution @@ -2598,7 +2605,7 @@ \begin{figure} \label{fig:tov_mode_spectrum} - \includegraphics[width=0.9\textwidth]{examples/tov/mode_spectrum} + \includegraphics[width=0.9\textwidth]{mode_spectrum} \caption{Eigenfrequency mode spectrum of a TOV star. Shown is the power spectral density of the central matter density, computed from a full 3D relativistic hydrodynamics simulation and compared to the values obtained by @@ -2627,7 +2634,7 @@ \begin{figure} \label{fig:tov_ham_conv} - \includegraphics[width=0.9\textwidth]{examples/tov/ham_conv} + \includegraphics[width=0.9\textwidth]{ham_conv} \caption{Convergence factor of Hamiltonian constraint violation at $r=0\mathrm{M}$ and $r=5\mathrm{M}$. The observed convergence order of about $1.5$ at the center of the star is lower then the general @@ -2686,7 +2693,7 @@ than second order, but higher than first order. \begin{figure} \label{fig:tov_collapse_radii} - \includegraphics[width=0.9\textwidth]{examples/collapse/radii} + \includegraphics[width=0.9\textwidth]{radii} \caption{Coordinate radius of the surface of the collapsing star and radius of the forming apparent horizon. The stellar surface is defined as the point where $\rho$ is @@ -2700,7 +2707,7 @@ \end{figure} \begin{figure} \label{fig:tov_collapse_H_convergence_at0} - \includegraphics[width=0.9\textwidth]{examples/collapse/H_convergence_at0} + \includegraphics[width=0.9\textwidth]{H_convergence_at0} \caption{Convergence factor for the Hamiltonian constraint violation at the center of the collapsing star. We plot convergence factors computed using a set of 4 runs covering the diameter of the star @@ -2773,8 +2780,8 @@ time resolutions. \begin{figure} - \includegraphics[width=0.9\textwidth]{examples/cosmology/figs/kasner.pdf} - \includegraphics[width=0.9\textwidth]{examples/cosmology/figs/err.pdf} + \includegraphics[width=0.9\textwidth]{kasner.pdf} + \includegraphics[width=0.9\textwidth]{err.pdf} \caption{Top: the evolution of a vacuum spacetime of the type~\eref{eq:gowdyT3}, with $P=Q=\lambda=0$; the initial data are chosen as $\gamma_{ij}=\delta_{ij}$ and $K_{ij}={\rm diag}(-2/3,-2/3,1/3)$.

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 135)
by roland.haas＠physics.gatech.edu 14 Nov '11

14 Nov '11

User: rhaas Date: 2011/11/14 01:29 PM Modified: /trunk/ einsteintoolkit.bib Log: fix minor issues wrt author names and paper titles File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.bib Delta lines: +15 -22 =================================================================== --- trunk/einsteintoolkit.bib 2011-11-14 18:15:19 UTC (rev 134) +++ trunk/einsteintoolkit.bib 2011-11-14 19:29:42 UTC (rev 135) @@ -141,7 +141,7 @@ Stergioulas and Ryoji Takahashi", title = "{Towards a stable numerical evolution of strongly gravitating systems in general relativity: The - Conformal treatments}", + Conformal Treatments}", journal = "Phys. Rev. D", volume = 62, pages = 044034, @@ -187,9 +187,7 @@ } @article{Anderson:2007kz, - author = "Anderson, Matthew and Hirschmann, Eric W. and - Lehner, Luis and Liebling, Steven L. and Motl, - Patrick M. and others", + author = "Matthew Anderson and Eric W. Hirschmann and Luis Lehner and Steven L. Liebling and Patrick M. Motl and David Neilsen and Carlos Palenzuela and Joel E. Tohline", title = "{Simulating binary neutron stars: Dynamics and gravitational waves}", journal = "Phys. Rev. D", @@ -197,15 +195,13 @@ pages = 024006, doi = "10.1103/PhysRevD.77.024006", year = 2008, - eprint = "arXiv:0708.2720 [gr-qc]", + eprint = "arXiv:0708.2720", adsurl = {http://www.slac.stanford.edu/spires/find/hep/www?rawcmd=find+doi+10.1103/PhysRevD.77.024006}, } @article{Anderson:2008zp, - author = "Anderson, Matthew and Hirschmann, Eric W. and - Lehner, Luis and Liebling, Steven L. and Motl, - Patrick M. and others", + author = "Matthew Anderson and Eric W. Hirschmann and Luis Lehner and Steven L. Liebling and Patrick M. Motl and David Neilsen and Carlos Palenzuela and Joel E. Tohline", title = "{Magnetized Neutron Star Mergers and Gravitational Wave Signals}", journal = "Phys. Rev. Lett.", @@ -213,7 +209,7 @@ pages = 191101, doi = "10.1103/PhysRevLett.100.191101", year = 2008, - eprint = "arXiv:0801.4387 [gr-qc]", + eprint = "arXiv:0801.4387", adsurl = {http://www.slac.stanford.edu/spires/find/hep/www?rawcmd=find+doi+10.1103/PhysRevLett.100.191101}, } @@ -248,7 +244,7 @@ @Article{Anninos:1996ez, author = {Peter Anninos and Karen Camarda and Joseph Libson - and Joan Mass{'o} and Edward Seidel and Wai-Mo Suen}, + and Joan Mass{\'o} and Edward Seidel and Wai-Mo Suen}, title = {Finding apparent horizons in dynamic 3-D numerical space-times}, journal = {Phys. Rev. D}, @@ -1068,7 +1064,7 @@ pages = 114002, doi = "10.1088/0264-9381/27/11/114002", year = 2010, - eprint = "arXiv:0912.3529 [astro-ph.HE]", + eprint = "arXiv:0912.3529", } ##E ############################################################################ @@ -1101,7 +1097,7 @@ Yuk Tung and Shapiro, Stuart L. and Taniguchi, Keisuke and Baumgarte, Thomas W.", title = "{Fully General Relativistic Simulations of Black - Hole- Neutron Star Mergers}", + Hole-Neutron Star Mergers}", journal = "Phys. Rev. D", volume = 77, year = 2008, @@ -1207,9 +1203,7 @@ } @article{Foucart:2011mz, - author = "Foucart, Francois and Duez, Matthew D. and Kidder, - Lawrence E. and Scheel, Mark A. and Szilagyi, Bela and - others", + author = "Francois Foucart and Matthew D. Duez and Lawrence E. Kidder and Mark A. Scheel and Bela Szilagyi and Saul A. Teukolsky", title = "{Black hole-neutron star mergers for 10 solar mass black holes}", year = "2011", @@ -1434,7 +1428,7 @@ @Article{Harten:1983on, author = {Amiram Harten and Peter D. Lax and Bram van Leer}, - title = {On Upstream Differencing and Godunov-Type Schemes for Hyperbolic Conservation Laws}, + title = {On Upstream Differencing and {G}odunov-Type Schemes for Hyperbolic Conservation Laws}, journal = {SIAM review}, volume = {25}, number = {1}, @@ -1781,7 +1775,7 @@ @Article{Lousto:2008dn, author = {{Lousto}, Carlos O. and {Zlochower}, Yosef}, title = "{Modeling gravitational recoil from precessing - highly- spinning unequal-mass black-hole binaries}", + highly-spinning unequal-mass black-hole binaries}", year = 2009, journal = "Phys. Rev. D", volume = 79, @@ -1804,8 +1798,7 @@ } @article{Lovelace:2009dg, - author = "Lovelace, Geoffrey and Chen, Yanbei and Cohen, Michael - and Kaplan, Jeffrey D. and Keppel, Drew and others", + author = "Geoffrey Lovelace and Yanbei Chen and Michael Cohen and Jeffrey D. Kaplan and Drew Keppel and Keith D. Matthews and David A. Nichols and Mark A. Scheel and Ulrich Sperhake", title = "{Momentum flow in black-hole binaries. II. Numerical simulations of equal-mass, head-on mergers with antiparallel spins}", @@ -1876,7 +1869,7 @@ } @article{Muller:2009jx, - author = "Muller, Doreen and Bruegmann, Bernd", + author = "M{\"u}ller, Doreen and Br{"u}gmann, Bernd", title = "{Toward a dynamical shift condition for unequal mass black hole binary simulations}", journal = "Class. Quant. Grav.", @@ -1930,7 +1923,7 @@ @Article{Oppenheimer:1939ne, author = "Oppenheimer, J. R. and Volkoff, G. M.", - title = "{On Massive neutron cores}", + title = "{On Massive Neutron Cores}", journal = "Phys. Rev.", volume = 55, year = 1939, @@ -2529,7 +2522,7 @@ editor = {Barth, Timothy J. and Deconinck, H. Array}, keywords = {Fluid dynamics Differential equations Mathematical physics.}, title = {High Order {ENO} and {WENO} Schemes for Computational Fluid Dynamics}, - booktitle = {High order methods for computational physics /}, + booktitle = {High order methods for computational physics}, year = {1999}, publisher = {Springer}, address = {New York},

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 239)
by schnetter＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: eschnett Date: 2011/11/14 01:05 PM Modified: / ET.tex Log: Small whitespace corrections File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +2 -2 =================================================================== --- ET.tex 2011-11-14 18:11:02 UTC (rev 238) +++ ET.tex 2011-11-14 19:05:49 UTC (rev 239) @@ -225,7 +225,7 @@ without requiring exorbitant computational resources, though some BH-NS simulations have been performed with a pseudospectral code \cite{Duez:2008rb,Duez:2009yy,Foucart:2010eq,Foucart:2011mz}. Many groups' codes now include GRMHD (used widely for NS-NS mergers, and for BH-NS mergers in~\cite{Chawla:2010sw}, and some include microphysical effects as -well~(e.g.,\cite{Duez:2009yy,Sekiguchi:2011zd,Sekiguchi:2011mc}). +well~(e.g.,~\cite{Duez:2009yy,Sekiguchi:2011zd,Sekiguchi:2011mc}). In addition to studying binary mergers, numerical relativity is a necessary element for understanding stellar collapse and dynamical instabilities @@ -916,7 +916,7 @@ \end{eqnarray} where the sub/superscript $(m)$ refers to the contribution from BH $m=1,2$; the 3-momentum is $p^i$; the BH spin angular momentum is $S_i$; the conformal 3-metric -$\gamma^{ij}$ is assumed to be flat, i.e. $\gamma_{ij}=\eta_{ij}$, and $\hat{N}^i=x^i/r$ +$\gamma^{ij}$ is assumed to be flat, i.e.\ $\gamma_{ij}=\eta_{ij}$, and $\hat{N}^i=x^i/r$ is the Cartesian normal vector relative to the position of each BH in turn. This solution automatically satisfies the momentum constraint, and the Hamiltonian constraint may be written as an elliptic equation for the conformal factor, defined by the condition $g_{ij}=\psi^4\gamma_{ij}$ or equivalently $\psi\equiv (\det|g_{ij}|)^{1/12}$:

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 134)
by jfaber＠einsteintoolkit.org 14 Nov '11

14 Nov '11

User: jfaber Date: 2011/11/14 12:15 PM Modified: /trunk/ einsteintoolkit.bib Log: Update a few refs for consistency File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.bib Delta lines: +7 -11 =================================================================== --- trunk/einsteintoolkit.bib 2011-11-14 16:50:30 UTC (rev 133) +++ trunk/einsteintoolkit.bib 2011-11-14 18:15:19 UTC (rev 134) @@ -109,7 +109,7 @@ hydrodynamics}", journal = "Astrophys. J. Suppl.", volume = "122", - pages = "151", + pages = "151-166", doi = "10.1086/313214", year = "1999", eprint = "astro-ph/9903352", @@ -852,13 +852,12 @@ and van Meter, James R.", title = "{Black-hole binaries, gravitational waves, and numerical relativity}", - journal = "Rev.Mod.Phys.", + journal = "Rev. Mod. Phys.", volume = "82", doi = "10.1103/RevModPhys.82.3069", year = "2010", - eprint = "1010.5260", - archivePrefix = "arXiv", - primaryClass = "gr-qc", + pages = "3069-3119", + eprint = "arXiv:1010.5260", } @article{Chawla:2010sw, @@ -1083,7 +1082,6 @@ YEAR = {1988}, NUMBER = {2}, PAGES = {294--318}, - ISSN = {0036-1429}, CODEN = {SJNAAM}, MRCLASS = {65M05 (76-08 76N15)}, MRNUMBER = {933726 (89e:65086)}, @@ -1442,7 +1440,6 @@ number = {1}, year = {1983}, pages = {35}, - issn = {0036-1445}, } @ARTICLE{Harten:1983hr, @@ -2536,8 +2533,7 @@ year = {1999}, publisher = {Springer}, address = {New York}, - issn = {3540658939 (pbk. : acid-free pap}, - pages = {439--582}, + pages = {439--582}, snote = {A related online version can be found under {\em Essentially {N}on-{O}scillatory and {W}eighted {E}ssentially {N}on-{O}scillatory {S}chemes for {H}yperbolic {C}onservation @@ -2636,7 +2632,7 @@ title = {{Simulation} {Factory}: Taming Application Configuration and Workflow on High-End Resources}, year = 2010, - eprint = {arXiv:1008.4571 [cs.DC]}, + eprint = {arXiv:1008.457}, } #Comment point to http://compframe.org/cbhpc2010/proceedings/ once they exist @@ -2839,7 +2835,7 @@ relativity}", journal = "Mon. Not. Roy. Astron. Soc.", volume = "322", - pages = "389", + pages = "389-396", doi = "10.1046/j.1365-8711.2001.04115.x", year = "2001", eprint = "astro-ph/9908359",

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 238)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 12:11 PM Modified: / ET.tex Log: two of gabs suggestions File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +2 -6 =================================================================== --- ET.tex 2011-11-14 17:52:21 UTC (rev 237) +++ ET.tex 2011-11-14 18:11:02 UTC (rev 238) @@ -295,19 +295,15 @@ of the goals of the Einstein Toolkit. 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 +However, many 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 otherwise necessary burden of creating such an infrastructure, while at the same time increasing the amount of code review and thus, code quality. - In addition, the Einstein Toolkit provides computer scientists an ideal platform to perform state-of-the-art research, which directly benefits research in other areas of science and provides an -immediate application of their research. One of the most prominent -examples within the Einstein Toolkit is the {\tt Cactus} computational toolkit, -a framework developed by computer scientists now used by researchers -in many other fields. +immediate application of their research. \section{Design and Strategy}

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/examples/kerr/figs/ (Rev. 237)
by knarf＠cct.lsu.edu 14 Nov '11

14 Nov '11

User: knarf Date: 2011/11/14 11:52 AM Modified: /examples/kerr/figs/ ah_mass.pdf, ah_mass_conv.pdf, kerr.py, qlm_mass.pdf, qlm_spin.pdf, waves.pdf, waves_conv.pdf, waves_l4.pdf, waves_l4_conv.pdf Log: fix figure 12 File Changes: Directory: /examples/kerr/figs/ =============================== File [modified]: ah_mass.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [modified]: ah_mass_conv.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [modified]: kerr.py Delta lines: +4 -0 =================================================================== --- examples/kerr/figs/kerr.py 2011-11-14 17:52:10 UTC (rev 236) +++ examples/kerr/figs/kerr.py 2011-11-14 17:52:21 UTC (rev 237) @@ -157,6 +157,8 @@ ax.set_xlabel(r'$t [M]$') ax.set_ylabel(r'$M_{\rm IH} [M]$') +ax.yaxis.set_major_formatter(mticker.ScalarFormatter(useOffset=False)) + handles, labels = ax.get_legend_handles_labels() ax.legend(handles, labels, loc='best') @@ -166,7 +168,9 @@ axs.plot(t, ord1m, linestyle='--', color='blue') axs.plot(t, ord1l, linestyle=':', color='red') axs.set_ylim(ylim) +axs.yaxis.set_major_formatter(mticker.ScalarFormatter(useOffset=False)) + plt.savefig('qlm_mass.pdf') fig = plt.figure(figsize=(6, 3)) File [modified]: qlm_mass.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [modified]: qlm_spin.pdf Delta lines: +1 -1 =================================================================== --- examples/kerr/figs/qlm_spin.pdf 2011-11-14 17:52:10 UTC (rev 236) +++ examples/kerr/figs/qlm_spin.pdf 2011-11-14 17:52:21 UTC (rev 237) @@ -4,7 +4,7 @@ << /Type /Catalog /Pages 3 0 R >> endobj 2 0 obj -<< /CreationDate (D:20111113220623-07'00') +<< /CreationDate (D:20111114095145-07'00') /Producer (matplotlib pdf backend) /Creator (matplotlib 0.99.3, http://matplotlib.sf.net) >> endobj File [modified]: waves.pdf Delta lines: +1 -1 =================================================================== --- examples/kerr/figs/waves.pdf 2011-11-14 17:52:10 UTC (rev 236) +++ examples/kerr/figs/waves.pdf 2011-11-14 17:52:21 UTC (rev 237) @@ -4,7 +4,7 @@ << /Type /Catalog /Pages 3 0 R >> endobj 2 0 obj -<< /CreationDate (D:20111113220612-07'00') +<< /CreationDate (D:20111114095138-07'00') /Producer (matplotlib pdf backend) /Creator (matplotlib 0.99.3, http://matplotlib.sf.net) >> endobj File [modified]: waves_conv.pdf Delta lines: +2 -2 =================================================================== --- examples/kerr/figs/waves_conv.pdf 2011-11-14 17:52:10 UTC (rev 236) +++ examples/kerr/figs/waves_conv.pdf 2011-11-14 17:52:21 UTC (rev 237) @@ -4,7 +4,7 @@ << /Type /Catalog /Pages 3 0 R >> endobj 2 0 obj -<< /CreationDate (D:20111113220614-07'00') +<< /CreationDate (D:20111114095139-07'00') /Producer (matplotlib pdf backend) /Creator (matplotlib 0.99.3, http://matplotlib.sf.net) >> endobj @@ -1590,7 +1590,7 @@ /FontDescriptor 30 0 R /Widths 28 0 R /LastChar 255 /FirstChar 0 >> endobj 4 0 obj -<< /F4 13 0 R /F1 17 0 R /F5 25 0 R /F3 21 0 R /F2 29 0 R >> +<< /F4 13 0 R /F1 17 0 R /F3 21 0 R /F2 29 0 R /F5 25 0 R >> endobj 5 0 obj << >> File [modified]: waves_l4.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [modified]: waves_l4_conv.pdf Delta lines: +0 -0 =================================================================== (Binary files differ)

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Commits November 2011