deletions | additions       diff --git a/IGW_are_generated_by.tex b/IGW_are_generated_by.tex  index 5bc3b45..7df8564 100644  --- a/IGW_are_generated_by.tex  +++ b/IGW_are_generated_by.tex 
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\end{equation}  Turbulent convection generates waves with a spectrum of azimuthal numbers $m$ and angular frequencies $\omega$, the values given above are characteristic values which dominate the AM flux.  The waves carrying the most AM flux sometimes damp before they reach the core, and might not be able to affect the spin of the core. Then the waves with $\bar{m}$ and $\bar{\omega}$ would not dominate the AM flux to the core; instead, other waves in the turbulent spectrum become important (see Appendix \ref{wavestar}). However, as a first check to see if IGW can have any affect on the spin of the star, we assume all waves can propagate to the core. Then the characteristic wave spin-down timescale for waves to change the spin of the core by an amount $\omega_c$, $\omega_c$ is  \begin{align}  \label{eqn:twave}  t_{\rm waves} &= \frac{I_c \omega_c}{\dot{J}} \\