deletions | additions       diff --git a/Discussion.tex b/Discussion.tex  index 89c0985..3a48a95 100644  --- a/Discussion.tex  +++ b/Discussion.tex 
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\subsection{Comparison with asteroseismology}\label{seismo}  We expect the evolved giants in KIC 9246715 to exhibit solar-like oscillations. These should be observable as p-modes for radial oscillations and mixed p- and g- modes for dipolar and quadrupolar oscillations in \emph{Kepler} long-cadence data. For solar-like oscillators, the average large frequency separation of p-modes $\Delta \nu$ has been shown to scale with the square root of the mean density of the star, while the frequency of maximum oscillation power $\nu_{\rm{max}}$ carries information about the physical conditions near the stellar surface and is a function of surface gravity and temperature \citep{cha13} (CITE KJLEDSEN \& BEDDING 95 instead). Note these These  relations shouldin principle  be valid only  for oscillation modes of large radial orders $n$, where pressure modes can be mathematically described in the frame of the in the ``asymptotic development'' (CITE TASSOUL 1980). Even though red-giant do not match these conditions because radial orders of observed modes are less than 10, the scaling relations look working rather well, but we expect some inaccuracy resulting from such approximations. These scaling relations may be used to estimate a star's density and surface gravity: \begin{equation} \label{density}  {\frac{\bar{\rho}}{\bar{\rho}_{\odot}}} \simeq {\left( \frac{\Delta \nu}{\Delta \nu_{\odot}} \right)}^{2} 
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