deletions | additions       diff --git a/More Discussion.tex b/More Discussion.tex  index d3986a8..4501683 100644  --- a/More Discussion.tex  +++ b/More Discussion.tex 
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where $f$ is a factor of order unity, $q$ is the ratio of the companion star's mass $M_2$ to the primary star's mass $M$, and  \begin{equation}  I(t) \equiv \int_0^t {\left( \left(  \frac{T_{\rm{eff}}(t')}{4500 \rm{K}} \right)}^{4/3} \right)^{4/3}  \ {\left( \left(  \frac{M_{\rm{env}}(t')}{M_{\odot}} \right)}^{2/3} \right)^{2/3}  \ {\left( \left(  \frac{R(t')}{R_{\odot}} \right)}^8 \right)^8  \ dt', \end{equation}  where $M_{\rm{env}}$ is the mass of the convective envelope of the primary star. 
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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.