deletions | additions       diff --git a/IGW_are_generated_by.tex b/IGW_are_generated_by.tex  index 4330b4b..e2f702a 100644  --- a/IGW_are_generated_by.tex  +++ b/IGW_are_generated_by.tex 
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\hline  \end{tabular}  \end{center}  \label{tab:table} Properties of IGW AM transport during evolutionary stages corresponding to the stellar models shown in Figures \ref{fig:Massivestruc} and \ref{fig:MassiveIGWtime}. Here, $r_c$ is the radius at the base of the convection zone in consideration, $T_{\rm shell}$ is the duration of the burning phase, and $\omega_{\rm con}$ is the convective turnover frequency. For He and C burning phases, IGW may be able to spin down the core, and $P_{\rm min}$ is the approximate minimum rotation period set by IGW during each phase. $P_{\rm min,Fe}$ is the minimum rotation period if AM is conserved until just before CC (when the iron core has a radius of 1500 km), and $P_{\rm min,NS}$ is the minimum rotation period if AM is conserved until NS birth. The listed values of $P_{\rm min}$ can only be set if IGW are able to extract sufficient AM from the core (see text), which is unlikely to occur during O/Si shell burning.  \end{table*}