deletions | additions       diff --git a/IGW_are_generated_by.tex b/IGW_are_generated_by.tex  index 22b63a0..1ded666 100644  --- a/IGW_are_generated_by.tex  +++ b/IGW_are_generated_by.tex 
...
\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{MassiveIGWtime}. \ref{fig:MassiveIGWtime}.  Here, $r_c$ is the core radius that encloses the inner $\sim \! 1.2 M_\odot$, $T_{\rm shell}$ is the duration of the burning phase, and $\omega_{\rm con}$ is the convective turnover frequency. $\omega_*(r_c)$ is the wave frequency which dominates AM transport at $r_c$, while $P_{\rm min} = 2 \pi/\omega_*(r_c)$ is the 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. \end{table*}