deletions | additions       diff --git a/subsection_Stellar_evolution_and_tidal__.tex b/subsection_Stellar_evolution_and_tidal__.tex  index 9a4009d..0126df5 100644  --- a/subsection_Stellar_evolution_and_tidal__.tex  +++ b/subsection_Stellar_evolution_and_tidal__.tex 
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\subsection{Stellar evolution and tidal forces}\label{tides}  INTRODUCE MESA FIGURE HERE. MODEL AND CORRESPONDING FIGURE. ADDRESS RADIUS DISCREPANCY(?)  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}, a study of tidal circularization in binaries containing giant stars. A CLEARER INTRODUCTION/OVERVIEW OF THAT WORK NEEDS TO WILL  GO HERE. We consider a detached binary with constant $a$ and constant binary masses. Equations 5 and 6 \citep{ver95} state: \begin{equation}\label{tide1}  \Delta \ln e = -1.7 \times 10^{-5} \ f \ {\left( \frac{M}{M_{\odot}} \right)}^{-11/3} \ q(1+q)^{-5/3} \ I(t) {\left( \frac{P_{\rm{orb}}}{\rm{day}} \right)}^{-16/3}, 
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The fact that only one star is oscillating points to how tidal activity may affect oscillations.  Important for other people because over half of cool stars should be in binaries! Using RGs to probe the galaxy has to be done carefully because of external influences of binarity on oscillations.}