deletions | additions       diff --git a/IGW_are_generated_by.tex b/IGW_are_generated_by.tex  index c65d1cd..9418f0c 100644  --- a/IGW_are_generated_by.tex  +++ b/IGW_are_generated_by.tex 
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In the top panel of Figure \ref{fig:MassiveIGWtime}, we plot the amount of AM capable of being extracted by IGW during each burning phase,   \begin{equation}  J_{\rm ex} = \dot{J}_*(r) T_{\rm shell}. shell} \, .  \label{Jex}  \end{equation}  We plot both a pessimistic and optimistic estimate, corresponding to the left and right-hand sides of equation \ref{eqn:Ewaves}, respectively. We find that the values of $J_{\rm ex}$ is comparable to $J_0$ for waves emitted during He core burning and C shell burning. This entails that IGW emitted during these phases may be able to significantly spin down the cores of massive stars. However, given the uncertainties, it is unclear whether IGW have a significant effect. During O and Si shell burning, we find that IGW most likely cannot remove the AM contained within the core. However, if the core has been spun down by IGW during previous burning phases, or via magnetic torques, IGW may still modify the core spin rate (see Section \ref{spinup}).