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[svn:einsteintoolkit] GRHydro/trunk/ (Rev. 266)
by roland.haas＠physics.gatech.edu 15 Sep '11

15 Sep '11

User: rhaas Date: 2011/09/15 11:42 AM Modified: /trunk/ param.ccl /trunk/src/ GRHydro_ParamCheck.F90, GRHydro_Tmunu.F90 Log: add option to smoothly dampen Tmunu to vacuum outside of a given radius File Changes: Directory: /trunk/src/ ====================== File [modified]: GRHydro_ParamCheck.F90 Delta lines: +4 -0 =================================================================== --- trunk/src/GRHydro_ParamCheck.F90 2011-08-19 23:58:27 UTC (rev 265) +++ trunk/src/GRHydro_ParamCheck.F90 2011-09-15 16:42:47 UTC (rev 266) @@ -125,5 +125,9 @@ end if end if + if (Tmunu_damping_radius_min .gt. Tmunu_damping_radius_max) then + call CCTK_WARN(0, "Minimum damping radius is greater than maximum damping radius!") + end if + end subroutine GRHydro_ParamCheck File [modified]: GRHydro_Tmunu.F90 Delta lines: +31 -11 =================================================================== --- trunk/src/GRHydro_Tmunu.F90 2011-08-19 23:58:27 UTC (rev 265) +++ trunk/src/GRHydro_Tmunu.F90 2011-09-15 16:42:47 UTC (rev 266) @@ -70,18 +70,22 @@ implicit none DECLARE_CCTK_ARGUMENTS + DECLARE_CCTK_PARAMETERS CCTK_REAL velxlow, velylow, velzlow CCTK_REAL betaxlow, betaylow, betazlow, beta2 CCTK_REAL utlow, uxlow, uylow, uzlow CCTK_REAL rhoenthalpy CCTK_REAL ut,ux,uy,uz,bst,bsx,bsy,bsz,bs2 + CCTK_REAL dampfac CCTK_INT i,j,k +!!$ Damping factor + dampfac = 1.0 !$OMP PARALLEL DO PRIVATE(i,j,k,velxlow, velylow, velzlow,& !$OMP betaxlow, betaylow, betazlow, beta2, utlow, uxlow, uylow, uzlow,& - !$OMP rhoenthalpy, ut,ux,uy,uz,bst,bsx,bsy,bsz,bs2) + !$OMP rhoenthalpy, ut,ux,uy,uz,bst,bsx,bsy,bsz,bs2,dampfac) do k = 1, cctk_lsh(3) do j = 1, cctk_lsh(2) do i = 1, cctk_lsh(1) @@ -111,21 +115,37 @@ uylow = velylow uzlow = velzlow + +!!$ Initialize damping factor + dampfac = 1.0 +!!$ Apply tanh blending for Tmunu. + if ((Tmunu_damping_radius_min .gt. 0) .and. (r(i,j,k) .gt. Tmunu_damping_radius_min)) then + ! 0.5 * (1.0 - tanh(4.0*(x-x0)/sigma0)) + if (r(i,j,k) .lt. Tmunu_damping_radius_max) then + dampfac = 0.5 * (1.0 - tanh(4.0*(r(i,j,k)-0.5*(Tmunu_damping_radius_max+Tmunu_damping_radius_min))/(Tmunu_damping_radius_max-Tmunu_damping_radius_min))) + else + dampfac = 0.0 + continue ! no need to add anything to Tmunu at the current point (it's zero anyway!) + endif + else + dampfac = 1.0 + endif + !!$ Calculate Tmunu (the lower components!). - eTtt(i,j,k) = eTtt(i,j,k) + rhoenthalpy*utlow**2 + press(i,j,k)*(beta2 - alp(i,j,k)**2) + eTtt(i,j,k) = eTtt(i,j,k) + dampfac * (rhoenthalpy*utlow**2 + press(i,j,k)*(beta2 - alp(i,j,k)**2)) - eTtx(i,j,k) = eTtx(i,j,k) + rhoenthalpy*utlow*uxlow + press(i,j,k)*betaxlow - eTty(i,j,k) = eTty(i,j,k) + rhoenthalpy*utlow*uylow + press(i,j,k)*betaylow - eTtz(i,j,k) = eTtz(i,j,k) + rhoenthalpy*utlow*uzlow + press(i,j,k)*betazlow + eTtx(i,j,k) = eTtx(i,j,k) + dampfac * (rhoenthalpy*utlow*uxlow + press(i,j,k)*betaxlow) + eTty(i,j,k) = eTty(i,j,k) + dampfac * (rhoenthalpy*utlow*uylow + press(i,j,k)*betaylow) + eTtz(i,j,k) = eTtz(i,j,k) + dampfac * (rhoenthalpy*utlow*uzlow + press(i,j,k)*betazlow) - eTxx(i,j,k) = eTxx(i,j,k) + rhoenthalpy*uxlow**2 + press(i,j,k)*gxx(i,j,k) - eTyy(i,j,k) = eTyy(i,j,k) + rhoenthalpy*uylow**2 + press(i,j,k)*gyy(i,j,k) - eTzz(i,j,k) = eTzz(i,j,k) + rhoenthalpy*uzlow**2 + press(i,j,k)*gzz(i,j,k) + eTxx(i,j,k) = eTxx(i,j,k) + dampfac * (rhoenthalpy*uxlow**2 + press(i,j,k)*gxx(i,j,k)) + eTyy(i,j,k) = eTyy(i,j,k) + dampfac * (rhoenthalpy*uylow**2 + press(i,j,k)*gyy(i,j,k)) + eTzz(i,j,k) = eTzz(i,j,k) + dampfac * (rhoenthalpy*uzlow**2 + press(i,j,k)*gzz(i,j,k)) - eTxy(i,j,k) = eTxy(i,j,k) + rhoenthalpy*uxlow*uylow + press(i,j,k)*gxy(i,j,k) - eTxz(i,j,k) = eTxz(i,j,k) + rhoenthalpy*uxlow*uzlow + press(i,j,k)*gxz(i,j,k) - eTyz(i,j,k) = eTyz(i,j,k) + rhoenthalpy*uylow*uzlow + press(i,j,k)*gyz(i,j,k) + eTxy(i,j,k) = eTxy(i,j,k) + dampfac * (rhoenthalpy*uxlow*uylow + press(i,j,k)*gxy(i,j,k)) + eTxz(i,j,k) = eTxz(i,j,k) + dampfac * (rhoenthalpy*uxlow*uzlow + press(i,j,k)*gxz(i,j,k)) + eTyz(i,j,k) = eTyz(i,j,k) + dampfac * (rhoenthalpy*uylow*uzlow + press(i,j,k)*gyz(i,j,k)) end do end do Directory: /trunk/ ================== File [modified]: param.ccl Delta lines: +16 -0 =================================================================== --- trunk/param.ccl 2011-08-19 23:58:27 UTC (rev 265) +++ trunk/param.ccl 2011-09-15 16:42:47 UTC (rev 266) @@ -532,6 +532,22 @@ { } "no" +############### Parameters for Tmunu damping (useful in atmosphere) ##################### + +CCTK_REAL Tmunu_damping_radius_min "damping radius at which we start to damp with a tanh function" +{ + -1 :: "damping switched off" + 0:* :: "damping radius at which we start to damp" +} -1 + + +CCTK_REAL Tmunu_damping_radius_max "damping radius at which Tmunu becomes 0" +{ + -1 :: "damping switched off" + 0:* :: "greater than minimum radius above" +} -1 + + ############### temporary parameters to be removed once connected issues are fixed. boolean con2prim_oct_hack "Disregard c2p failures in oct/rotsym90 boundary cells with xyz < 0" STEERABLE=ALWAYS

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[svn:einsteintoolkit] www/publications/ (Rev. 610)
by bcmsma＠astro.rit.edu 14 Sep '11

14 Sep '11

User: bmundim Date: 2011/09/14 11:03 AM Modified: /publications/ index.php Log: Sort publication list by year. File Changes: Directory: /publications/ ========================= File [modified]: index.php Delta lines: <Unavailable>

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 133)
by knarf＠cct.lsu.edu 13 Sep '11

13 Sep '11

User: knarf Date: 2011/09/13 02:01 PM Added: /examples/tov/ plot_defaults.py, rho_max.py Removed: /examples/tov/ rho_max.plot, rho_max.svg /examples/tov/tov_2/ hydrobase::rho.maximum.asc.spectrum.bz2 Modified: / ET.tex /examples/tov/ make_plots.sh, mode_spectrum.pdf, mode_spectrum.py, rho_max.pdf Log: more on tov oscillations File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: <Unavailable> Directory: /examples/tov/ ========================= File [modified]: make_plots.sh Delta lines: <Unavailable> File [modified]: mode_spectrum.pdf Delta lines: <Unavailable> File [modified]: mode_spectrum.py Delta lines: <Unavailable> File [added]: plot_defaults.py Delta lines: <Unavailable> File [modified]: rho_max.pdf Delta lines: <Unavailable> File [removed]: rho_max.plot Delta lines: <Unavailable> File [added]: rho_max.py Delta lines: <Unavailable> File [removed]: rho_max.svg Delta lines: <Unavailable> Directory: /examples/tov/tov_2/ =============================== File [removed]: hydrobase::rho.maximum.asc.spectrum.bz2 Delta lines: <Unavailable>

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 132)
by knarf＠cct.lsu.edu 13 Sep '11

13 Sep '11

User: knarf Date: 2011/09/13 12:04 AM Modified: / ET.tex /examples/tov/ mode_spectrum.pdf, mode_spectrum.py Log: add tov text, improve psd figure File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +34 -25 =================================================================== --- ET.tex 2011-09-13 04:29:02 UTC (rev 131) +++ ET.tex 2011-09-13 05:04:10 UTC (rev 132) @@ -2554,10 +2554,11 @@ \end{figure} \subsection{Linear oscillations of TOV stars\pages{2 Frank}} -The previous examples did not include the evolution of matter within a relativistic -spacetime. One interesting test of a coupled matter-spacetime evolution is -to measure the eigenfrequencies of a stable TOV star. These eigenfrequencies -can be compared to values known from linear perturbation theory. +The examples in the previous subsections did not include the evolution of +matter within a relativistic spacetime. One interesting test of a coupled +matter-spacetime evolution is to measure the eigenfrequencies of a stable TOV +star. These eigenfrequencies can be compared to values known from linear +perturbation theory. This test uses an equillibrium configuration of a self-gravitating fluid sphere, described by a polytropic equation of state. This one-dimensional @@ -2570,11 +2571,10 @@ Despite the system being in equilibrium, the solution experiences oscillations mainly due to perturbations from two sources, the interpolation of the initial data onto the evolution grid, and due to the interaction of the star and the -atmosphere. The former is damped out with time, and can be reduced by -increasing both the resolution of the one-dimensional solution and of the -evolution grid. For resolutions of tests presented here, this perturbation was -small compared to perturbations from the remaining source, the interaction with -the atmosphere. These perturbations are present during the whole evolution, +atmosphere. The former is damped quickly, and can be reduced by increasing the +resolution of the evolution grid. It can be seen as initial spike in the +evolution of the central density of the star. The remaining perturbations, +mainly from the atmosphere treatment, are present during the whole evolution, continuously exciting oscillations. Given enough evolution time, the frequencies of these oscillations can be measured with satisfactory accuracy. @@ -2583,39 +2583,48 @@ and an initial central density of $\varrho_0=1.28\times10^{-3}$. This model can be taken to represent a non-rotating neutron star with a mass of $M=1.4\mathrm{M}_\odot$. The computational domain is a cube of length -$640\mathrm{M}$ and a resolution of $2\mathrm{M}$ in each dimension. Four -additional grids refine the region around the star at the origin, each doubling -the resolution, with sizes of $120\mathrm{M}$, $60\mathrm{M}$, $30\mathrm{M}$ -and $15\mathrm{M}$, resulting in a resolution of $0.125\mathrm{M}$ across the -entire star. +$640\mathrm{M}$ and a base resolution of $2\mathrm{M}$ ($4\mathrm{M}$, +$8\mathrm{M}$) in each dimension. Four additional grids refine the region +around the star located at the origin, each doubling the resolution, with sizes +of $120\mathrm{M}$, $60\mathrm{M}$, $30\mathrm{M}$ and $15\mathrm{M}$, +resulting in a resolution of $0.125\mathrm{M}$ ($0.25\mathrm{M}$, +$0.5\mathrm{M}$) across the entire star. In figure~\ref{fig:tov_rho_max} we show the evolution of the central density of -the star, over an evolution time of~\todo{X}. +the star, over an evolution time of $1300\mathrm{M}$. The initial spike is due +to the perturbation of the solution resulting from the interpolation onto the +evolution grid. These oscillations are quickly damped. Most of the remaining +oscillations are due to perturbations resulting from the treatment of the +atmosphere. The mean of the central density shows a drift, which converges +to zero with increasing resolution.\todo{show} \begin{figure} \label{fig:tov_rho_max} - \includegraphics[width=0.8\textwidth]{examples/tov/rho_max} + \includegraphics[width=0.95\textwidth]{examples/tov/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 equillibirum solution onto the three-dimensional evolution grid. The remainder of the evolution however, the central density evolution is dominated by continuous excitations coming - from the interaction of the stellar surface with the artificial atmosphere.} + from the interaction of the stellar surface with the artificial atmosphere. Shown + are three different resolutions.} \end{figure} -In figure~\ref{fig:tov_mode_spectrum} we show the power spectrum of the central +In figure~\ref{fig:tov_mode_spectrum} we show the power spectral density (PSD) of the central density oscillations computed from a full 3D relativistic hydrodynamics simulation, compared to the coresponding frequencies as obtained with perturbative techniques, kindly provided to use by Kentaro Takami and computed -using the method described in~\cite{Yoshida01}. Clearly the 3D simulation can -correctly represent the fundamental mode frequency and the first three -overtones of the neutron star. +using the method described in~\cite{Yoshida01}. The PSD was computed using the entire +time series, removing the linear trend, averaging over Hanning windows overlapping half the +signal length after padding the signal to five time it's length. +The agreement of the frequencies of the fundamental mode and the first three overtones +is clearly visible. \begin{figure} \label{fig:tov_mode_spectrum} - \includegraphics[width=0.8\textwidth]{examples/tov/mode_spectrum} - \caption{Eigenfrequency mode spectrum of TOV star. Shown is the spectrum - computed from a full 3D relativistic hydrodynamics simulation compared - to the values obtained by perturbation theory.} + \includegraphics[width=0.95\textwidth]{examples/tov/mode_spectrum} + \caption{Eigenfrequency mode spectrum of a TOV star. Shown is the power spectral density + of the central density, computed from a full 3D relativistic hydrodynamics simulation compared + to the values obtained by perturbation theory.\todo{improve caption}} \end{figure} Directory: /examples/tov/ ========================= File [modified]: mode_spectrum.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [modified]: mode_spectrum.py Delta lines: +2 -2 =================================================================== --- examples/tov/mode_spectrum.py 2011-09-13 04:29:02 UTC (rev 131) +++ examples/tov/mode_spectrum.py 2011-09-13 05:04:10 UTC (rev 132) @@ -54,8 +54,8 @@ Fy = Fy[int(start*len(Fy)): int(end*len(Fy))] # Plot basics -fig = plt.figure() -fig.subplots_adjust(hspace=0.45, wspace=0.3, left=0.15, bottom=0.15) +fig = plt.figure(figsize=(15, 5)) +fig.subplots_adjust(top=0.9,bottom=0.18, left=0.08,right=0.98) ax = fig.add_subplot(1,1,1) # mode names and frequencies

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 131)
by knarf＠cct.lsu.edu 12 Sep '11

12 Sep '11

User: knarf Date: 2011/09/12 11:29 PM Added: /examples/tov/ mode_spectrum.py Removed: /examples/tov/ mode_labels.sh, mode_spectrum.plot, mode_spectrum.svg, modes.dat Modified: /examples/tov/ make_plots.sh, mode_spectrum.pdf Log: use matplotlib for mode plot, calculate psd on the fly, including overlap with Hanning window, padding and linear detrending Directory Changes: Directory: /svn:executable/ =========================== + * File Changes: Directory: /examples/tov/ ========================= File [modified]: make_plots.sh Delta lines: +1 -2 =================================================================== --- examples/tov/make_plots.sh 2011-09-09 18:23:23 UTC (rev 130) +++ examples/tov/make_plots.sh 2011-09-13 04:29:02 UTC (rev 131) @@ -1,4 +1,3 @@ -gnuplot < mode_spectrum.plot -inkscape -A mode_spectrum.pdf mode_spectrum.svg +./mode_spectrum.py gnuplot < rho_max.plot inkscape -A rho_max.pdf rho_max.svg File [removed]: mode_labels.sh Delta lines: +0 -1 =================================================================== --- examples/tov/mode_labels.sh 2011-09-09 18:23:23 UTC (rev 130) +++ examples/tov/mode_labels.sh 2011-09-13 04:29:02 UTC (rev 131) @@ -1 +0,0 @@ -perl -ane 'if ($F[2]) { print "set label \"$F[2]\" at ".($F[0]-0.15).",2.e-6\n"; }' modes.dat File [modified]: mode_spectrum.pdf Delta lines: +0 -0 =================================================================== (Binary files differ) File [removed]: mode_spectrum.plot Delta lines: +0 -13 =================================================================== --- examples/tov/mode_spectrum.plot 2011-09-09 18:23:23 UTC (rev 130) +++ examples/tov/mode_spectrum.plot 2011-09-13 04:29:02 UTC (rev 131) @@ -1,13 +0,0 @@ -set size ratio 0.3 -set term svg enhanced size 600,250 -set output 'mode_spectrum.svg' -set xlabel 'f/[kHz]' -set xtics 2 nomirror -set mxtics 2 -set x2tics scale 0 -set ylabel 'PSD' -set ytics 10 -#load '<./mode_labels.sh' -plot [:10][:-50] '<bzcat tov_2/hydrobase::rho.maximum.asc.spectrum.bz2' u ($1/1000):(10*log10($2)) w lp t '', \ -'<sed -e ''s/$.*$/\1 -80\n\1 -50\n/g'' modes.dat' u 1:3 w l t '', \ -'modes.dat' u 1:(0):x2ticlabels(2) w l t '' File [added]: mode_spectrum.py Delta lines: +105 -0 =================================================================== --- examples/tov/mode_spectrum.py (rev 0) +++ examples/tov/mode_spectrum.py 2011-09-13 04:29:02 UTC (rev 131) @@ -0,0 +1,105 @@ +#!/usr/bin/python + +# Compute power spectral density of given data +import numpy as np +import matplotlib.pyplot as plt +import matplotlib.ticker as mticker + +from matplotlib import rc +from matplotlib.mlab import detrend_linear + +# stuff +fontsize = 20 +xlim = (0,10) +ylim = (-140,-100) +rc('text', usetex=True) +rc('font', family='serif') +rc('font', serif='palatino') +rc('font', weight='bolder') +rc('mathtext', default='sf') +rc("lines", markeredgewidth=1) +rc("lines", linewidth=3) +rc('axes', labelsize=fontsize) +rc("axes", linewidth=2) +rc('xtick', labelsize=fontsize) +rc('ytick', labelsize=fontsize) +rc('legend', fontsize=fontsize) +rc('xtick.major', pad=8) +rc('ytick.major', pad=8) + +def set_tick_sizes(ax, major, minor): + for l in ax.get_xticklines() + ax.get_yticklines(): + l.set_markersize(major) + for tick in ax.xaxis.get_minor_ticks() + ax.yaxis.get_minor_ticks(): + tick.tick1line.set_markersize(minor) + tick.tick2line.set_markersize(minor) + ax.xaxis.LABELPAD=10. + ax.xaxis.OFFSETTEXTPAD=10. + +# constants +G = 6.673e-11 +c = 299792458 +M_sol = 1.98892e30 +# convertion factors +M_to_ms = 1./(1000*M_sol*G/(c*c*c)) + +# load data +Fx, Fy = np.loadtxt("tov_2/hydrobase::rho.maximum.asc.bz2", comments="#", usecols=(1,2), unpack=True) +dt = M_to_ms/(Fx[1]-Fx[0]) + +# slice data if wanted +start = 0.0 +end = 1. +Fx = Fx[int(start*len(Fx)): int(end*len(Fx))] +Fy = Fy[int(start*len(Fy)): int(end*len(Fy))] + +# Plot basics +fig = plt.figure() +fig.subplots_adjust(hspace=0.45, wspace=0.3, left=0.15, bottom=0.15) +ax = fig.add_subplot(1,1,1) + +# mode names and frequencies +modes = { +"F" : 1.44252691528028, +"H1": 3.95408396916149, +"H2": 5.91494894170517, +"H3": 7.77382493405710, +"H4": 9.58768293806276, +"H5": 11.3772129983097, +"H6": 13.1520241905666, +"H7": 14.9172321735655, +} + +# plot modes as vertical lines and label them +for mode, freq in modes.items(): + ax.plot((freq,freq), ylim, 'b--') + ax.text(freq-0.1, ylim[1]+1, mode, fontsize=fontsize) +#ax.plot((2*modes["F"], 2*modes["F"]), (-200,0), 'g--') +#ax.plot((3*modes["F"], 3*modes["F"]), (-200,0), 'g--') +#ax.plot((4*modes["F"], 4*modes["F"]), (-200,0), 'g--') + +# plot PSD +frac = 0.5 * len(Fy) +ax.psd(Fy, NFFT=int(frac), pad_to=5*int(frac), noverlap=int(frac*0.5), detrend=detrend_linear, Fs=dt, linestyle='-', color='black', scale_by_freq=False) +#ax.psd(Fy, NFFT=int(len(Fy)*frac), pad_to=10*int(len(Fy)*frac), noverlap=int(len(Fy)*frac*0.50), detrend=detrend_linear, Fs=M_to_ms/(Fx[1]-Fx[0]), linestyle='-', marker='x', color='red') + +# plot properties +ax.set_xlim(xlim) +ax.set_ylim(ylim) + +#plt.title('PSD', fontsize=fontsize) +ax.set_xlabel(r'$f$ [kHz]') +ax.set_ylabel(r'PSD [dB/Hz]') + +ax.xaxis.set_major_locator(mticker.MaxNLocator(10)) +ax.xaxis.set_minor_locator(mticker.MaxNLocator(20)) +ax.xaxis.grid(False) +ax.yaxis.set_major_locator(mticker.MaxNLocator(5)) +ax.yaxis.set_minor_locator(mticker.MaxNLocator(9)) +ax.yaxis.grid(False) +set_tick_sizes(ax, 8, 4) + + +#plt.show() +plt.savefig('mode_spectrum.pdf') + Property changes on: examples/tov/mode_spectrum.py ___________________________________________________________________ File [removed]: mode_spectrum.svg Delta lines: +0 -210 =================================================================== --- examples/tov/mode_spectrum.svg 2011-09-09 18:23:23 UTC (rev 130) +++ examples/tov/mode_spectrum.svg 2011-09-13 04:29:02 UTC (rev 131) @@ -1,210 +0,0 @@ -<?xml version="1.0" encoding="utf-8" standalone="no"?> -<!DOCTYPE svg PUBLIC "-//W3C//DTD SVG 1.1//EN" - 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stroke-linecap:butt; stroke-linejoin:miter"> - <path d='M164.0,128.9 L164.0,40.8 M286.9,128.9 L286.9,40.8 M382.8,128.9 L382.8,40.8 M473.8,128.9 L473.8,40.8 - M562.5,128.9 L562.5,40.8 '></path> -</g> -<g style="fill:none; color:blue; stroke:currentColor; stroke-width:1.00; stroke-linecap:butt; stroke-linejoin:miter"> -</g> -<g style="fill:none; color:black; stroke:currentColor; stroke-width:1.00; stroke-linecap:butt; stroke-linejoin:miter"> - <path d='M93.4,40.8 L93.4,187.6 L582.7,187.6 L582.7,40.8 L93.4,40.8 Z '></path> -</g> -</svg> - File [removed]: modes.dat Delta lines: +0 -8 =================================================================== --- examples/tov/modes.dat 2011-09-09 18:23:23 UTC (rev 130) +++ examples/tov/modes.dat 2011-09-13 04:29:02 UTC (rev 131) @@ -1,8 +0,0 @@ -1.44252691528028 F -3.95408396916149 H1 -5.91494894170517 H2 -7.77382493405710 H3 -9.58768293806276 H4 -11.3772129983097 H5 -13.1520241905666 H6 -14.9172321735655 H7

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[svn:einsteintoolkit] www/documentation/ (Rev. 609)
by knarf＠cct.lsu.edu 12 Sep '11

12 Sep '11

User: knarf Date: 2011/09/12 01:21 PM Modified: /documentation/ send-account.php Log: fix variable interpretation File Changes: Directory: /documentation/ ========================== File [modified]: send-account.php Delta lines: +1 -1 =================================================================== --- documentation/send-account.php 2011-08-31 21:17:37 UTC (rev 608) +++ documentation/send-account.php 2011-09-12 18:21:50 UTC (rev 609) @@ -16,7 +16,7 @@ $mentionadvisor = 'This student\'s advisor is '.$advisor.'.'; } else { -$mentionadvisor = '"$advisor" was mentioned as advisor.'; +$mentionadvisor = '"'.$advisor.'" was mentioned as advisor.'; } if (! empty($department)){

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 130)
by knarf＠cct.lsu.edu 09 Sep '11

09 Sep '11

User: knarf Date: 2011/09/09 01:23 PM Added: /examples/tov/ rho_max.pdf, rho_max.plot, rho_max.svg Modified: / ET.tex /examples/tov/ make_plots.sh, mode_spectrum.pdf, mode_spectrum.plot, mode_spectrum.svg, modes.dat Log: more on the stable tov File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: <Unavailable> Directory: /examples/tov/ ========================= File [modified]: make_plots.sh Delta lines: <Unavailable> File [modified]: mode_spectrum.pdf Delta lines: <Unavailable> File [modified]: mode_spectrum.plot Delta lines: <Unavailable> File [modified]: mode_spectrum.svg Delta lines: <Unavailable> File [modified]: modes.dat Delta lines: <Unavailable> File [added]: rho_max.pdf Delta lines: <Unavailable> File [added]: rho_max.plot Delta lines: <Unavailable> File [added]: rho_max.svg Delta lines: <Unavailable>

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 109)
by knarf＠cct.lsu.edu 06 Sep '11

06 Sep '11

User: knarf Date: 2011/09/06 04:01 PM Modified: /trunk/ einsteintoolkit.th Log: reflect move of LocalReduce and LocalInterp File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.th Delta lines: +2 -2 =================================================================== --- trunk/einsteintoolkit.th 2011-08-26 15:00:33 UTC (rev 108) +++ trunk/einsteintoolkit.th 2011-09-06 21:01:51 UTC (rev 109) @@ -71,8 +71,6 @@ CactusBase/IOASCII CactusBase/IOBasic CactusBase/IOUtil -CactusBase/LocalInterp -CactusBase/LocalReduce CactusBase/SymBase CactusBase/Time @@ -89,6 +87,8 @@ CactusNumerical/Cartoon2D CactusNumerical/Dissipation CactusNumerical/InterpToArray +CactusNumerical/LocalInterp +CactusNumerical/LocalReduce CactusNumerical/MoL CactusNumerical/Noise CactusNumerical/Norms

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[svn:einsteintoolkit] SphericalHarmonicRecon/trunk/ (Rev. 7)
by knarf＠cct.lsu.edu 06 Sep '11

06 Sep '11

User: knarf Date: 2011/09/06 01:39 PM Modified: /trunk/ README Log: test change File Changes: Directory: /trunk/ ================== File [modified]: README Delta lines: +1 -0 =================================================================== --- trunk/README 2011-09-05 13:20:25 UTC (rev 6) +++ trunk/README 2011-09-06 18:39:29 UTC (rev 7) @@ -49,3 +49,4 @@ Please contact the maintainers of the code if you require write access. +

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[svn:einsteintoolkit] SphericalHarmonicRecon/trunk/test/ (Rev. 6)
by yosef＠astro.rit.edu 05 Sep '11

05 Sep '11

User: zlochower Date: 2011/09/05 08:20 AM Added: /trunk/test/ metric_test_case.h5, regression_test.par, test.ccl /trunk/test/regression_test/ NewsB[0]_2D.asc, NewsB[0]_norm2.xg, regression_test.par Log: regression test for CCE File Changes: Directory: /trunk/test/regression_test/ ======================================= File [added]: NewsB[0]_2D.asc Delta lines: <Unavailable> File [added]: NewsB[0]_norm2.xg Delta lines: <Unavailable> File [added]: regression_test.par Delta lines: <Unavailable> Directory: /trunk/test/ ======================= File [added]: metric_test_case.h5 Delta lines: <Unavailable> File [added]: regression_test.par Delta lines: <Unavailable> File [added]: test.ccl Delta lines: <Unavailable>

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