deletions | additions       diff --git a/Asteroseismic Calculations.tex b/Asteroseismic Calculations.tex  index 0e970e5..cecf05f 100644  --- a/Asteroseismic Calculations.tex  +++ b/Asteroseismic Calculations.tex 
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\begin{equation}  \delta\nu_{n,\ell} = \frac{1}{2\pi} \int_0^R K_{n,\ell}(r) \, \Omega(r) \,\hbox{d}r  \end{equation}  The functions $K_{n,\ell}(r)$ are called rotational kernels of the modes and depend on the star's equilibrium structure and on the mode eigenfunctions. eigenfunctions \citep[See e.g.,][]{Aerts:2010}.  Therefore rotational splittings are basically a weighted measure of the star’s rotation rate through the  rotational kernels.