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\label{fig:MassiveIGWtime} {\bf Top:} Angular frequency $\omega_*$ of IGW responsible for The thick black line shows  the bulk angular momentum $J_0$ contained within the mass coordinate $M(r)$  of AM transport, as our massive star model rotating with  a function period  of interior mass, for $P_0 \approx 1.5 {\rm d}$ on  the same stellar models shown in Figure \ref{fig:Massivestruc}. ZAMS.  Thevertical  shaded bars are drawn at the base of the convective zone from which regions indicate  the angular momentum $J_{\rm ex}$ (equation \ref{Jex}) that can be extracted by  IGW are launched. during the burning phases described in Figure \ref{fig:MassiveIGWstruc}.  The value of $\omega_*$ increases inward as lower frequency IGW are attenuated due to radiative damping/non-linear breaking. shaded  {\bf Bottom:} Wave spindown time scales, $t_*$ (equation \ref{eqn:tstar}) as a function of radius, during each stage of evolution. We have also plotted the time until CC as horizontal solid lines, which also correspond approximately to the duration of each stage, $T_{\rm shell}$, shown in Table \ref{tab:table}. Waves may spin down the core to angular frequencies $\omega_*$ as long as $t_*$ is shorter than the time until death. In this case, the value of $\omega_*$ at any radius represents the maximum expected angular spin frequency.