epsilon: specific internal energy (ie energy/mass)

git-svn-id: http://svn.einsteintoolkit.org/cactus/EinsteinEvolve/GRHydro/trunk@315 c83d129a-5a75-4d5a-9c4d-ed3a5855bf45

1 files changed, 6 insertions, 6 deletions

diff --git a/doc/documentation.tex b/doc/documentation.tex
index fdca0c8..9387fbf 100644
--- a/doc/documentation.tex
+++ b/doc/documentation.tex
@@ -204,11 +204,11 @@ still there for reference.
 
 For the equations of state, two ``types'' are recognized, controlled
 by the parameter {\tt GRHydro\_eos\_type}. These are {\tt "Polytype"}
-where the pressure is a function of the density, $P=P(\rho)$, and the
+where the pressure is a function of the rest-mass density, $P=P(\rho)$, and the
 more generic {\tt "General"} type where the pressure is a function
-of the density and the internal energy, $P=P(\rho, \epsilon)$. For the
+of the rest-mass density and the specific internal energy, $P=P(\rho, \epsilon)$. For the
 {\tt Polytype} equations of state one fewer equation is evolved and
-the specific internal energy is set directly from the density. The
+the specific internal energy is set directly from the rest-mass density. The
 actual equation of state used is controlled by the parameter {\tt
   GRHydro\_eos\_table}. Polytype equations of state include {\tt
   "2D\_Polytrope"} and general equations of state include {\tt
@@ -312,8 +312,8 @@ The five conserved variables are labeled $D$, $S^i$, and $\tau$, where
 $D$ is the generalized particle number density, $S^i$ are the generalized
 momenta in each direction, and $\tau$ is an internal energy term.
 These conserved variables are composed from a set of {\it primitive variables},
-which are $\rho$, the density, $p$, the
-pressure, $v^i$, the fluid 3-velocities, $\epsilon$, the internal
+which are $\rho$, the rest-mass density, $p$, the
+pressure, $v^i$, the fluid 3-velocities, $\epsilon$, the specific internal
 energy, and $W$, the Lorentz factor, via the following relations
 % from GRHydro/src/Prim2con.F90
 %  w = 1.d0 / sqrt(1.d0 - (gxx*dvelx*dvelx + gyy*dvely*dvely + gzz &
@@ -342,7 +342,7 @@ $h \equiv 1 + \epsilon + p/\rho$.
 Only five of the primitive variables are
 independent. Usually the Lorentz factor is defined in terms of the
 velocities and the metric as $W = (1-\gamma_{ij}v^i v^j)^{-1/2}$.  
-Also one of the pressure, density or internal energy terms is given in 
+Also one of the pressure, rest-mass density or specific internal energy terms is given in 
 terms of the other two by an {\it equation of state}.
 
 The fluxes are usually defined in terms of both the conserved