deletions | additions       diff --git a/subsection_Stellar_evolution_and_tidal__.tex b/subsection_Stellar_evolution_and_tidal__.tex  index 163de92..0b50888 100644  --- a/subsection_Stellar_evolution_and_tidal__.tex  +++ b/subsection_Stellar_evolution_and_tidal__.tex 
...
\begin{itemize}  \item Mass loss: Adding a prescription for moderate red-giant-branch mass loss ($\eta = 0.4$, see \citealt{mig12}) to the MESA model does not appreciably change stellar radius as a function of evolutionary stage. Even a more extreme mass-loss rate ($\eta = 0.7$) does not significantly affect the radii, essentially because the star is too low-mass to lose much mass.  \item He abundance: Increasing the initial He fraction in the MESA model does not allow for smaller stars in the red clump phase, because shell-H burning is very efficient with additional He present. As a result, the star maintains a high luminosity and therefore a larger radius as it evolves from the tip of the red giant branch to the red clump.  \item Convective overshoot: The MESA models in this work assume a reasonable overshoot efficiency as described above ($f = 0.016$). We tried varying this from 0--0.03, and can barely make a red clump star as small as $R_2 \simeq 8.3 $8.3  \ R_\odot$ when $f = 0.01$. With less overshoot, the RGB phase as shown in Figure \ref{fig:mesa} increases in duration, which allows a higher probability for stars of $M_1$ and $M_2$ to both be on the RGB. \item Period spacing: The period spacing \revise{$\Delta \Pi_1 = 150.4 \pm 1.4 \ \rm{s}$} may not be measuring what we expect due to rotational splitting of mixed oscillation modes. If the true period spacing is closer to $\Delta \Pi_1 \simeq 80 \ \rm{sec}$, \revise{this would put the oscillating star on the red giant branch. However, as demonstrated in Section \ref{subsubsec_mixed}, the mixed modes do agree best with a secondary red clump star.} A detailed discussion of rotational splitting behavior in slowly rotating red giants is explored in \citet{gou13}.  \item Mixing length: \revise{As discussed above,} increasing the mixing-length parameter from the standard solar value of $\alpha = 2$ to $\alpha = 2.5$ in the MESA model, which effectively increases the efficiency of convection, produces a red clump star small enough to agree with both measured radii. This is because it reduces the temperature gradient in the near-surface layers, increasing the effective temperature while reducing the radius at constant luminosity. \revise{This is what we employ to make horizontal branch stars that agree with $R_1$ and $R_2$.}  \end{itemize}