deletions | additions       diff --git a/subsection_Searching_for_a_second__.tex b/subsection_Searching_for_a_second__.tex  index 41d3f96..b3e59e0 100644  --- a/subsection_Searching_for_a_second__.tex  +++ b/subsection_Searching_for_a_second__.tex 
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\subsection{Searching for a second set of oscillations}  Given that the giants in KIC 9246715 are nearly twins, with $L_1/L_2 = 0.94$, $R_1/R_2 = 0.95$, $M_1/M_2 = 1.01$, and $T_1/T_2 = 1.01$, we test whether it is possible that we see only one set of oscillation modes because both stars are oscillating with virtually identical frequencies. It is unlikely that two sets of solar-like oscillations lie on top of one another, because the predicted $\nu_{\rm{max}}$ for these not-quite-identical stars are about $114.90 \pm 4.43$ and  $102.39 \pm 3.43\ \mu$Hz for star 1 and star  2 respectively  (from an inversion of Equations \ref{radeq} and \ref{masseq}), and the predicted $\Delta\nu_{\rm{obs}}$ are about $8.14 \pm 0.12 \ \mu$Hz for star 1 and star 2 respectively. The effective frequency resolution of the power spectrum for four years of \emph{Kepler} data is about $0.008 \ \mu \rm{Hz}$, and, more importantly, the intrinsic observed mode line widths is about $0.5 \ \mu \rm{Hz}$. % This is about five times as wide as normal RGs.  Given this, the oscillation pattern from a second star (if present) should \emph{not} appear to lie exactly on top of the oscillation pattern we do see. To illustrate this, the observed oscillation pattern in Figure \ref{fig:seismo} (red) is shown with predicted oscillation modes based on the physical parameters of both stars in the binary (OTHER COLOR(s) - UPDATE FIGURE AND THEN WRITE ABOUT IT). (I NEED TO PUT ERROR BARS ON THAT. WITH THE ERROR BARS, SPECTRA MIGHT OVERLAP PERFECTLY. I'LL DO THAT TOMORROW. P.G. 29.6.15. NEED ERRORBARS ON TEMPERATURES ACTUALLY... 30.6.15) 
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