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| author | bmundim <bmundim@1bdb13ef-5d69-4035-bb54-08abeb3aa7f1> | 2010-05-03 03:06:10 +0000 |
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| committer | bmundim <bmundim@1bdb13ef-5d69-4035-bb54-08abeb3aa7f1> | 2010-05-03 03:06:10 +0000 |
| commit | 98def174f187fcd32539695e7de6d2ec022fb44a (patch) | |
| tree | 59d25e16af51d0e6ca20f1fbed7df40ce0174cd7 /doc | |
| parent | d0457002f0b35f50e898d1147aa72dfb0e729746 (diff) | |
file/parameter string replacement from whisky to GRHydro
git-svn-id: http://svn.einsteintoolkit.org/cactus/EinsteinInitialData/TOVSolver/trunk@109 1bdb13ef-5d69-4035-bb54-08abeb3aa7f1
Diffstat (limited to 'doc')
| -rw-r--r-- | doc/documentation.tex | 2 |
1 files changed, 1 insertions, 1 deletions
diff --git a/doc/documentation.tex b/doc/documentation.tex index d84d659..00e4d65 100644 --- a/doc/documentation.tex +++ b/doc/documentation.tex @@ -332,7 +332,7 @@ the current thorns ({\tt CosmologicalConstant}, the hydro code, the scalar field code) all use the {\tt CalcTmunu} interface. You also have the possibility to use a parameter -{\tt whiskytovsolver::TOV\_Separation} to obtain a spacetime consisting +{\tt GRHydrotovsolver::TOV\_Separation} to obtain a spacetime consisting of one TOV-system for $x>0$ and a second (similar) for $x<0$. This parameter sets the separation of the centers of two neutron stars, has to be positive and should be larger than twice the radius of one star.\\ |