deletions | additions       diff --git a/subsection_Stellar_evolution_and_tidal__.tex b/subsection_Stellar_evolution_and_tidal__.tex  index c01c8cf..1c1054f 100644  --- a/subsection_Stellar_evolution_and_tidal__.tex  +++ b/subsection_Stellar_evolution_and_tidal__.tex 
...
WRITE SOMETHING ABOUT RG MASS LOSS, WHICH ISN'T VERY WELL UNDERSTOOD.  To estimate how tidal forces may affect the orbital eccentricity, we follow the approach of \citet{ver95}, which uses the who use a  theory of the  equilibrium tide first proposed by \citet{zah77} to calculate a timescale for orbit circularization, $\tau_c$, as a star evolves. The total change in eccentricity over a binary's lifetime, $\Delta \ln e$, is found by integrating $1/\tau_c \equiv \rm{d} \ln e / \rm{d}t$: \begin{equation}\label{circ}  \Delta \ln e = \int_0^t \frac{\rm{d}t'}{\tau_c(t')}. 
...