deletions | additions       diff --git a/IGW_are_generated_by.tex b/IGW_are_generated_by.tex  index 831e29c..65d425b 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 thecore  radius that encloses at the base of  the inner $\sim \! 1.2 M_\odot$, convection zone in consideration,  $T_{\rm shell}$ is the duration of the burning phase, and $\omega_{\rm con}$ is the convective turnover frequency. $\omega_*(r_c)$ is For He and C burning phases, IGW may be able to spin down  the wave frequency which dominates AM transport at $r_c$, while core, and  $P_{\rm min} = 2 \pi/\omega_*(r_c)$ 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. \end{table*}