Commits January 2011

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7 participants
57 discussions

[svn:einsteintoolkit] EOS_Omni/trunk/src/nuc_eos/ (Rev. 33)
by schnetter＠cct.lsu.edu 26 Jan '11

26 Jan '11

User: eschnett Date: 2011/01/26 10:14 AM Modified: /trunk/src/nuc_eos/ linterp.f, linterp_many.F90, make.code.defn, nuc_eos.F90, readtable.F90 Log: Replace stop commands with calls to CCTK_WARN, since stop with a string argument is not supported by all Fortran compilers. File Changes: Directory: /trunk/src/nuc_eos/ ============================== File [modified]: linterp.f Delta lines: +3 -1 =================================================================== --- trunk/src/nuc_eos/linterp.f 2010-12-22 21:44:39 UTC (rev 32) +++ trunk/src/nuc_eos/linterp.f 2011-01-26 16:14:37 UTC (rev 33) @@ -1,3 +1,5 @@ +#include "cctk.h" + SUBROUTINE intp3d ( x, y, z, f, kt, ft, nx, ny, nz, xt, yt, zt, . d1, d2, d3 ) c @@ -50,7 +52,7 @@ double precision dx,dy,dz,dxi,dyi,dzi,dxyi,dxzi,dyzi,dxyzi integer n,ix,iy,iz - IF (kt .GT. ktx) STOP'***KTX**' + IF (kt .GT. ktx) call CCTK_WARN (0, '***KTX**') c c c------ determine spacing parameters of (equidistant!!!) table File [modified]: linterp_many.F90 Delta lines: +4 -2 =================================================================== --- trunk/src/nuc_eos/linterp_many.F90 2010-12-22 21:44:39 UTC (rev 32) +++ trunk/src/nuc_eos/linterp_many.F90 2011-01-26 16:14:37 UTC (rev 33) @@ -1,3 +1,5 @@ +#include "cctk.h" + SUBROUTINE intp3d_many ( x, y, z, f, kt, ft, nx, ny, nz, nvars, xt, yt, zt) ! implicit none @@ -43,7 +45,7 @@ real*8 dx,dy,dz,dxi,dyi,dzi,dxyi,dxzi,dyzi,dxyzi integer n,ix,iy,iz - IF (kt .GT. ktx) STOP'***KTX**' + IF (kt .GT. ktx) call CCTK_WARN(0, '***KTX**') ! ! !------ determine spacing parameters of (equidistant!!!) table @@ -65,7 +67,7 @@ ! !------- loop over all points to be interpolated ! - dO n = 1, kt + do n = 1, kt ! !------- determine location in (equidistant!!!) table ! File [modified]: make.code.defn Delta lines: +1 -1 =================================================================== --- trunk/src/nuc_eos/make.code.defn 2010-12-22 21:44:39 UTC (rev 32) +++ trunk/src/nuc_eos/make.code.defn 2011-01-26 16:14:37 UTC (rev 33) @@ -1,6 +1,6 @@ SRCS = eosmodule.F90 nuc_eos.F90 bisection.F90 \ findtemp.F90 findrho.F90 linterp_many.F90 readtable.F90 \ - linterp.f + linterp.F SUBDIRS = File [modified]: nuc_eos.F90 Delta lines: +16 -13 =================================================================== --- trunk/src/nuc_eos/nuc_eos.F90 2010-12-22 21:44:39 UTC (rev 32) +++ trunk/src/nuc_eos/nuc_eos.F90 2011-01-26 16:14:37 UTC (rev 33) @@ -17,6 +17,9 @@ ! 1 -> coming in with temperature ! 2 -> coming in with entropy ! + +#include "cctk.h" + subroutine nuc_eos_full(xrho,xtemp,xye,xenr,xprs,xent,xcs2,xdedt,& xdpderho,xdpdrhoe,xxa,xxh,xxn,xxp,xabar,xzbar,xmu_e,xmu_n,xmu_p, & xmuhat,keytemp,keyerr,rfeps) @@ -45,11 +48,11 @@ keyerrr = 0 if(xrho.gt.eos_rhomax) then - stop "nuc_eos: rho > rhomax" + call CCTK_WARN(0, "nuc_eos: rho > rhomax") endif if(xrho.lt.eos_rhomin) then - stop "nuc_eos: rho < rhomin" + call CCTK_WARN (0, "nuc_eos: rho < rhomin") endif if(xye.gt.eos_yemax) then @@ -64,11 +67,11 @@ if(keytemp.eq.1) then if(xtemp.gt.eos_tempmax) then - stop "nuc_eos: temp > tempmax" + call CCTK_WARN (0, "nuc_eos: temp > tempmax") endif if(xtemp.lt.eos_tempmin) then - stop "nuc_eos: temp < tempmin" + call CCTK_WARN (0, "nuc_eos: temp < tempmin") endif endif @@ -84,7 +87,7 @@ !need to find temperature based on xeps call findtemp(lr,lt,y,leps,keyerrt,rfeps) if(keyerrt.ne.0) then - stop "Did not find temperature" + call CCTK_WARN (0, "Did not find temperature") endif xtemp = 10.0d0**lt @@ -206,7 +209,7 @@ keyerrr = 0 if(xrho.gt.eos_rhomax) then - stop "nuc_eos: rho > rhomax" + call CCTK_WARN (0, "nuc_eos: rho > rhomax") endif if(xrho.lt.eos_rhomin*1.2d0) then @@ -227,7 +230,7 @@ if(keytemp.eq.1) then if(xtemp.gt.eos_tempmax) then - stop "nuc_eos: temp > tempmax" + call CCTK_WARN (0, "nuc_eos: temp > tempmax") endif if(xtemp.lt.eos_tempmin) then @@ -329,7 +332,7 @@ keyerrt = 0 if(xrho.gt.eos_rhomax) then - stop "nuc_eos: rho > rhomax" + call CCTK_WARN (0, "nuc_eos: rho > rhomax") endif if(xrho.lt.eos_rhomin*1.2d0) then @@ -349,7 +352,7 @@ if(keytemp.eq.1) then if(xtemp.gt.eos_tempmax) then - stop "nuc_eos: temp > tempmax" + call CCTK_WARN (0, "nuc_eos: temp > tempmax") endif if(xtemp.lt.eos_tempmin) then @@ -361,7 +364,7 @@ keyerr = 0 if(keytemp.gt.1) then - stop "eos_nuc_press does not support keytemp other than 0 and 1" + call CCTK_WARN (0, "eos_nuc_press does not support keytemp other than 0 and 1") endif lr = log10(xrho) @@ -408,7 +411,7 @@ keyerrt = 0 if(xrho.gt.eos_rhomax) then - stop "nuc_eos: rho > rhomax" + call CCTK_WARN (0, "nuc_eos: rho > rhomax") endif if(xrho.lt.eos_rhomin*1.2d0) then @@ -428,7 +431,7 @@ if(keytemp.eq.1) then if(xtemp.gt.eos_tempmax) then - stop "nuc_eos: temp > tempmax" + call CCTK_WARN (0, "nuc_eos: temp > tempmax") endif if(xtemp.lt.eos_tempmin) then @@ -455,7 +458,7 @@ xtemp = 10.0d0**lt elseif(keytemp.gt.1) then - stop "eos_nuc_press does not support keytemp > 1" + call CCTK_WARN (0, "eos_nuc_press does not support keytemp > 1") endif ! have temperature, proceed: File [modified]: readtable.F90 Delta lines: +4 -4 =================================================================== --- trunk/src/nuc_eos/readtable.F90 2010-12-22 21:44:39 UTC (rev 32) +++ trunk/src/nuc_eos/readtable.F90 2011-01-26 16:14:37 UTC (rev 33) @@ -42,7 +42,7 @@ call h5dclose_f(dset_id,error) if(error.ne.0) then - stop "Could not read EOS table file" + call CCTK_WARN (0, "Could not read EOS table file") endif dims1(1)=1 @@ -51,7 +51,7 @@ call h5dclose_f(dset_id,error) if(error.ne.0) then - stop "Could not read EOS table file" + call CCTK_WARN (0, "Could not read EOS table file") endif dims1(1)=1 @@ -60,7 +60,7 @@ call h5dclose_f(dset_id,error) if(error.ne.0) then - stop "Could not read EOS table file" + call CCTK_WARN (0, "Could not read EOS table file") endif ! write(message,"(a25,1P3i5)") "We have nrho ntemp nye: ", nrho,ntemp,nye @@ -213,7 +213,7 @@ accerr=accerr+error if(accerr.ne.0) then - stop "Problem reading EOS table file" + call CCTK_WARN (0, "Problem reading EOS table file") endif call h5fclose_f (file_id,error)

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[svn:einsteintoolkit] AHFinderDirect/trunk/ (Rev. 1554)
by knarf＠cct.lsu.edu 25 Jan '11

25 Jan '11

User: knarf Date: 2011/01/25 03:48 PM Modified: /trunk/ param.ccl, schedule.ccl Log: Change the number of timelevels of the ahmask to match the number which is used for the metric. Setting this to three unconditionally leads to problems when running with Carpet and prolongation_order_time=1 because all GFs in Carpet are expected to have the same number of timelevels: prolongation_order_time+1. This is not the ideal solution. That would eliminate also variables ala metric_timelevels, because they directly depend on prolongation_order_time and should not have to be set (correctly) in a parameter file. This could be done automatically. However, this patch for now uses metric_timelevels, in order to get AHFinderDirect working quickly. File Changes: Directory: /trunk/ ================== File [modified]: param.ccl Delta lines: +1 -0 =================================================================== --- trunk/param.ccl 2010-11-21 03:28:57 UTC (rev 1553) +++ trunk/param.ccl 2011-01-25 21:48:16 UTC (rev 1554) @@ -20,6 +20,7 @@ # note our access is read-only shares: ADMBase USES KEYWORD metric_type +USES CCTK_INT metric_timelevels # we need to look at SpaceMask::use_mask in order to find out about the # excision region File [modified]: schedule.ccl Delta lines: +13 -1 =================================================================== --- trunk/schedule.ccl 2010-11-21 03:28:57 UTC (rev 1553) +++ trunk/schedule.ccl 2011-01-25 21:48:16 UTC (rev 1554) @@ -2,8 +2,20 @@ # $Header$ storage: ah_radius ah_origin ah_centroid ah_flags -storage: ahmask[3] +if (metric_timelevels == 1) +{ + storage: ahmask[1] +} +else if (metric_timelevels == 2) +{ + storage: ahmask[2] +} +else if (metric_timelevels == 3) +{ + storage: ahmask[3] +} + # # setup #

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 21)
by bcmsma＠astro.rit.edu 24 Jan '11

24 Jan '11

User: bmundim Date: 2011/01/24 01:24 PM Modified: / ET.tex Log: Add RIT affiliation address. File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +4 -1 =================================================================== --- ET.tex 2011-01-24 19:15:09 UTC (rev 20) +++ ET.tex 2011-01-24 19:24:58 UTC (rev 21) @@ -78,6 +78,10 @@ \thanks{{}$^{(3)}$ Center for Computation \& Technology, Louisiana State University, Baton Rouge, LA 70803, USA} +\thanks{{}$^{(4)}$ Center for Computational Relativity \& Gravitation, + School of Mathematical Sciences, + Rochester Institute of Technology, Rochester, New York 14623, USA} + % TODO: Already add a few affiliations which we know are going % to be used @@ -413,7 +417,6 @@ \subsection{Initial Data} \todo{1/2 page Josh, Bruno} - The Einstein Toolkit contains many modules used to generate initial data for GR simulations, including both vacuum and hydrodynamical configurations. These include modules used primarily for testing out various components of

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 71)
by bcmsma＠astro.rit.edu 24 Jan '11

24 Jan '11

User: bmundim Date: 2011/01/24 01:15 PM Modified: /trunk/ einsteintoolkit.bib Log: Fix a few reference keys. File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.bib Delta lines: +11 -0 =================================================================== --- trunk/einsteintoolkit.bib 2011-01-24 19:01:49 UTC (rev 70) +++ trunk/einsteintoolkit.bib 2011-01-24 19:15:35 UTC (rev 71) @@ -230,6 +230,17 @@ SLACcitation = "%%CITATION = 0711.1097;%%" } +@Article{Brill:1959zz, + author = "Brill, Dieter R.", + title = "{On the positive definite mass of the Bondi-Weber-Wheeler + time-symmetric gravitational waves}", + journal = "Annals Phys.", + volume = "7", + year = "1959", + pages = "466-483", + SLACcitation = "%%CITATION = APNYA,7,466;%%" +} + @Article{Brown:2007pg, requested-for = "EinsteinInitialData/NoExcision", author = "David Brown and Olivier Sarbach and Erik Schnetter

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 20)
by bcmsma＠astro.rit.edu 24 Jan '11

24 Jan '11

User: bmundim Date: 2011/01/24 01:15 PM Modified: / ET.tex Log: Fix a few reference keys. File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +3 -3 =================================================================== --- ET.tex 2011-01-24 18:01:31 UTC (rev 19) +++ ET.tex 2011-01-24 19:15:09 UTC (rev 20) @@ -425,9 +425,9 @@ numerical software packages that are included in the toolkit as External libraries. The {\tt twopunctures} module \cite{Ansorg:2004ds}, commonly used in numerical relativity to generate binary black hole data, invokes -the GNU Scientific Library [GSL; \cite{Galassi:2009}]. Several modules +the GNU Scientific Library [GSL; \cite{GSL:web,Galassi:2009}]. Several modules have also been implemented to read in datafiles generated by the {\tt Lorene -code} \cite{Lorene:web,GGTMB}, including the BHBH, BHNS, and NSNS data +code} \cite{Lorene:web,Gourgoulhon:2000nn}, including the BHBH, BHNS, and NSNS data made publicly available through the Lorene website. Scheduling of initial data routines generally follows a standard format. @@ -469,7 +469,7 @@ \end{enumerate} \item Vacuum gravitational wave configurations: \begin{enumerate} -\item {\tt IDBrillData}: A Brill wave spacetime \cite{Brill:1959}. +\item {\tt IDBrillData}: A Brill wave spacetime \cite{Brill:1959zz}. \item {\tt IDLinearWaves}: A spacetime containing a linear gravitational wave. \end{enumerate} \item Black Hole configurations:

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 70)
by bcmsma＠astro.rit.edu 24 Jan '11

24 Jan '11

User: bmundim Date: 2011/01/24 01:01 PM Modified: /trunk/ einsteintoolkit.bib Log: GSL website. File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.bib Delta lines: +5 -0 =================================================================== --- trunk/einsteintoolkit.bib 2011-01-24 17:55:14 UTC (rev 69) +++ trunk/einsteintoolkit.bib 2011-01-24 19:01:49 UTC (rev 70) @@ -483,6 +483,11 @@ SLACcitation = "%%CITATION = GR-QC/0701109;%%" } +@Misc{GSL:web, + note = {{GSL}: The {GNU} Scientific Library}, + url = {http://www.gnu.org/software/gsl/}, +} + @Article{Gopakumar:2007vh, author = "Gopakumar, Achamveedu and Hannam, Mark and Husa, Sascha and Bruegmann, Bernd",

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 19)
by bcmsma＠astro.rit.edu 24 Jan '11

24 Jan '11

User: bmundim Date: 2011/01/24 12:01 PM Modified: / ET.tex Log: Following Frank's suggestion of breaking lines around column 80. File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +55 -41 =================================================================== --- ET.tex 2011-01-24 17:52:33 UTC (rev 18) +++ ET.tex 2011-01-24 18:01:31 UTC (rev 19) @@ -414,48 +414,58 @@ \subsection{Initial Data} \todo{1/2 page Josh, Bruno} -The Einstein Toolkit contains many modules used to generate initial data for GR simulations, -including both vacuum and hydrodynamical configurations. These include modules used primarily -for testing out various components of the evolution scheme as well as physically motivated -configurations that describe single of binary blacks and/or neutron stars. Many of the modules -are self-contained, consisting of either all the code to generate exact initial solutions or -the numerical tools required to construct solutions known semi-analytically. Others, though, -require the installation of other numerical software packages that are included in the toolkit -as External libraries. The {\tt twopunctures} module \cite{Ansorg:2004ds}, commonly used in numerical -relativity to generate binary black hole data, invokes the GNU Scientific Library [GSL; \cite{Galassi:2009}]. -Several modules have also been implemented to read in datafiles generated by the -{\tt Lorene code} \cite{Lorene:web,GGTMB}, including the BHBH, BHNS, and NSNS data made publicly -available through the Lorene website. +The Einstein Toolkit contains many modules used to generate initial data for +GR simulations, including both vacuum and hydrodynamical configurations. +These include modules used primarily for testing out various components of +the evolution scheme as well as physically motivated configurations that +describe single of binary blacks and/or neutron stars. Many of the modules +are self-contained, consisting of either all the code to generate exact +initial solutions or the numerical tools required to construct solutions +known semi-analytically. Others, though, require the installation of other +numerical software packages that are included in the toolkit as External +libraries. The {\tt twopunctures} module \cite{Ansorg:2004ds}, commonly +used in numerical relativity to generate binary black hole data, invokes +the GNU Scientific Library [GSL; \cite{Galassi:2009}]. Several modules +have also been implemented to read in datafiles generated by the {\tt Lorene +code} \cite{Lorene:web,GGTMB}, including the BHBH, BHNS, and NSNS data +made publicly available through the Lorene website. -Scheduling of initial data routines generally follows a standard format. User-defined parameters -are run through a parameter check designed to catch obvious internal inconsistencies, in addition to -any known incompatibilities with other modules of the toolkit. Initial data is then generated -at the proper stage within the Cactus framework, determined primarily by whether the configuration -in question represents vacuum or a hydrodynamical configuration. Finally, any necessary cleanup -is typically performed at the end of the initial step, prior to the iterations forward in time. +Scheduling of initial data routines generally follows a standard format. +User-defined parameters are run through a parameter check designed to catch +obvious internal inconsistencies, in addition to any known incompatibilities +with other modules of the toolkit. Initial data is then generated at the proper +stage within the Cactus framework, determined primarily by whether the +configuration in question represents vacuum or a hydrodynamical configuration. +Finally, any necessary cleanup is typically performed at the end of the initial +step, prior to the iterations forward in time. -For vacuum initial data configurations, an initial data module must supply $g_{ij}$, the spatial 3-metric, -and $K_{ij}$, the extrinsic curvature. While the evolution scheme typically makes use of the BSSN formalism, -the conversion between the physical and conformal metric and extrinsic curvature is handled solely within -evolution modules, and is not referenced by initial data ones. Optionally, many initial data modules also -supply values for the lapse and shift vector, and in some cases time derivatives as well, though these -may be supplied by other routines depending on the freedom to choose gauge conditions envisioned for a -specific configuration. +For vacuum initial data configurations, an initial data module must supply +$g_{ij}$, the spatial 3-metric, and $K_{ij}$, the extrinsic curvature. +While the evolution scheme typically makes use of the BSSN formalism, +the conversion between the physical and conformal metric and extrinsic +curvature is handled solely within evolution modules, and is not referenced +by initial data ones. Optionally, many initial data modules also supply values +for the lapse and shift vector, and in some cases time derivatives as well, +though these may be supplied by other routines depending on the freedom +to choose gauge conditions envisioned for a specific configuration. -For hydrodynamic configurations, assuming that an equation of state has been specified, the user must also -supply the values of hydrodynamic variables at all grid locations, in particular the primitive variables -$\rho$, $v_i$ and the energy variable $\epsilon$ for all cases where we don't have a polytype EOS in the -form $P=P(\rho)$ (see Sec.~\ref{???} for a discussion of the use of EOS in the ET). For an MHD configuration, -one must supply all of these along with the initial magnetic field $B^i$ as well. +For hydrodynamic configurations, assuming that an equation of state has been +specified, the user must also supply the values of hydrodynamic variables +at all grid locations, in particular the primitive variables $\rho$, $v_i$ and +the energy variable $\epsilon$ for all cases where we don't have a polytype EOS +in the form $P=P(\rho)$ (see Sec.~\ref{???} for a discussion of the use of EOS +in the ET). For an MHD configuration, one must supply all of these along with +the initial magnetic field $B^i$ as well. The initial data routines currently implemented include the following: \begin{itemize} \item Vacuum spacetime tests: \begin{enumerate} -\item {\tt IDConstraintViolate}: A vacuum spacetime in which the diagonal terms in the spatial metric are -modified by a spatial deformation to explicitly violate the Hamiltonian constraint. -\item {\tt Exact}: A set of exact spacetimes in various coordinates, along with tools to Lorentz boost -those configurations. +\item {\tt IDConstraintViolate}: A vacuum spacetime in which the diagonal terms +in the spatial metric are modified by a spatial deformation to explicitly +violate the Hamiltonian constraint. +\item {\tt Exact}: A set of exact spacetimes in various coordinates, along with +tools to Lorentz boost those configurations. \end{enumerate} \item Vacuum gravitational wave configurations: \begin{enumerate} @@ -464,13 +474,17 @@ \end{enumerate} \item Black Hole configurations: \begin{enumerate} -\item {\tt IDAnalyticBH}: This module can generate Schwarzchild black holes, as well as the Misner solution -for multiple BHs and the brill-Lindquist binary BH solution. -\item {\tt IDAxibrillBH,~IDAxiOddBrillBH}: These modules generate single black holes deformed by even and -odd parity axisymmetric perturbations, respectively. -\item {\tt DistortedBHIVP,~RotatingDBHIVP}: These modules generate single black holes distorted by even -and odd-parity non-axisymmetric perturbation, respectivey. -\item {\tt TwoPunctures}: This module generates accurate binary black-hole initial data. +\item {\tt IDAnalyticBH}: This module can generate Schwarzchild black holes, +as well as the Misner solution for multiple BHs and the brill-Lindquist binary +BH solution. +\item {\tt IDAxibrillBH,~IDAxiOddBrillBH}: These modules generate single +black holes deformed by even and odd parity axisymmetric perturbations, +respectively. +\item {\tt DistortedBHIVP,~RotatingDBHIVP}: These modules generate single +black holes distorted by even and odd-parity non-axisymmetric perturbation, +respectivey. +\item {\tt TwoPunctures}: This module generates accurate binary black-hole +initial data. \end{enumerate} \end{itemize}

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 69)
by bcmsma＠astro.rit.edu 24 Jan '11

24 Jan '11

User: bmundim Date: 2011/01/24 11:55 AM Modified: /trunk/ einsteintoolkit.bib Log: Lorene entry File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.bib Delta lines: +5 -0 =================================================================== --- trunk/einsteintoolkit.bib 2011-01-24 17:52:03 UTC (rev 68) +++ trunk/einsteintoolkit.bib 2011-01-24 17:55:14 UTC (rev 69) @@ -693,6 +693,11 @@ ##L ############################################################################ +@Misc{Lorene:web, + note = {{LORENE}: Langage Objet pour la RElativite NumeriquE}, + url = {http://www.lorene.obspm.fr/}, +} + @Article{Lousto:2007db, author = "Lousto, Carlos O. and Zlochower, Yosef", title = "{Further insight into gravitational recoil}",

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[svn:einsteintoolkit] Paper_EinsteinToolkit_2010/ (Rev. 18)
by bcmsma＠astro.rit.edu 24 Jan '11

24 Jan '11

User: bmundim Date: 2011/01/24 11:52 AM Modified: / ET.tex Log: Update Lorene entry. File Changes: Directory: / ============ File [modified]: ET.tex Delta lines: +1 -1 =================================================================== --- ET.tex 2011-01-24 17:50:29 UTC (rev 17) +++ ET.tex 2011-01-24 17:52:33 UTC (rev 18) @@ -424,7 +424,7 @@ as External libraries. The {\tt twopunctures} module \cite{Ansorg:2004ds}, commonly used in numerical relativity to generate binary black hole data, invokes the GNU Scientific Library [GSL; \cite{Galassi:2009}]. Several modules have also been implemented to read in datafiles generated by the -{\tt Lorene code} \cite{Loreneweb,GGTMB}, including the BHBH, BHNS, and NSNS data made publicly +{\tt Lorene code} \cite{Lorene:web,GGTMB}, including the BHBH, BHNS, and NSNS data made publicly available through the Lorene website. Scheduling of initial data routines generally follows a standard format. User-defined parameters

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[svn:einsteintoolkit] manifest/trunk/ (Rev. 68)
by knarf＠cct.lsu.edu 24 Jan '11

24 Jan '11

User: knarf Date: 2011/01/24 11:52 AM Modified: /trunk/ einsteintoolkit.bib Log: more references File Changes: Directory: /trunk/ ================== File [modified]: einsteintoolkit.bib Delta lines: +53 -0 =================================================================== --- trunk/einsteintoolkit.bib 2011-01-24 17:08:52 UTC (rev 67) +++ trunk/einsteintoolkit.bib 2011-01-24 17:52:03 UTC (rev 68) @@ -74,6 +74,20 @@ SLACcitation = "%%CITATION = GR-QC/0404056;%%" } +@ARTICLE{Arnowitt:1962hi, + author = "Arnowitt, Richard L. and Deser, Stanley and Misner, Charles W.", + title = "{The dynamics of general relativity}", + journal = {General Relativity and Gravitation}, + year = 2008, + month = sep, + volume = 40, + pages = {1997-2027}, + doi = {10.1007/s10714-008-0661-1}, + eprint = "gr-qc/0405109", + archivePrefix = "arXiv", + SLACcitation = "%%CITATION = GR-QC/0405109;%%" +} + ##B ############################################################################ @Article{Baiotti:2004wn, @@ -181,6 +195,17 @@ SLACcitation = "%%CITATION = 0708.4202;%%" } +@article{Banyuls:1997zz, + key = {Banyuls97}, + author = {F. Banyuls and J.~A. Font and J.~M. Ib{\'a}{\~n}ez and + J.~M. Mart{\'\i} and J.~A. Miralles}, + title = {Numerical {3+1} General-Relativistic Hydrodynamics: A Local Characteristic Approach }, + journal = {Astrophys. J.}, + volume = {476}, + year = {1997}, + pages = {221} +} + @Article{Baumgarte:2006en, author = "Thomas Baumgarte and Patrick Brady and Jolien D E Creighton and Luis Lehner and Frans Pretorius and Ricky DeVoe", title = "Learning about compact binary merger: The interplay between @@ -640,6 +665,23 @@ } ##I ############################################################################ + +@Inproceedings{Ibanez:2001:godunov, + author={J.M. Ib{\'a}{\~n}ez and M.A. Aloy and J.A. Font and + J.M. Mart{\'\i} and J.A. Miralles and J.A. Pons}, + title={}, + booktitle = {Proceedings of Godunov Methods, Theory and Applications 1999}, + conferencetitle = {Godunov Methods, Theory and Applications}, + conferencedate = {1999}, + conferencelocation = {Oxford}, + edition = {first}, + pages = {}, + editor={E.F. Toro}, + publisher = {Kluwer Academic/Plenum Publishers}, + address={New York}, + year={2001} +} + ##J ############################################################################ ##K ############################################################################ @@ -679,6 +721,17 @@ ##M ############################################################################ +@article{Marti:1991wi, + key = {Marti91}, + author = {J.~M. Mart{\'\i} and J.~M. Ib{\'a}{\~n}ez and J.~M. Miralles}, + title = {Numerical relativistic hydrodynamics: Local characteristic + approach}, + journal = {Phys. Rev. D}, + volume = {43}, + year = {1991}, + pages = {3794-3801} +} + @Misc{McLachlan:web, suggested-for ="McLachlan/ML_BSSN", note = {{McLachlan}, a Public {BSSN} Code},

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Commits January 2011