deletions | additions       diff --git a/figures/MassiveIGWtime/caption.tex b/figures/MassiveIGWtime/caption.tex  index fb74923..be5c596 100644  --- a/figures/MassiveIGWtime/caption.tex  +++ b/figures/MassiveIGWtime/caption.tex 
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\label{fig:MassiveIGWtime} {\bf Top:} The thick black line shows the angular momentum $J_0$ contained within the mass coordinate $M(r)$ of our massive star model rotating with a period of $P_0 \approx 1.5 {\rm d}$ on the ZAMS. The shaded regions indicate the angular momentum $J_{\rm ex}$ (equation \ref{Jex}) \ref{eqn:Jex})  that can be extracted by IGW during the burning phases described shown  in Figure \ref{fig:MassiveIGWstruc}. The shaded {\bf Bottom:} Wave spindown time scales, $t_*$ (equation \ref{eqn:tstar}) as regions are bounded by lines calculated with  a function of radius, during each stage pessimistic and optimistic estimate for IGW fluxes (see equation \ref{eqn:Ewaves}), and are shown in regions below the base  ofevolution. We have also plotted  the time until CC as horizontal solid lines, convective zones (marked by the vertical dashed lines) from  which also correspond approximately to IGW are launched. In  the duration of each stage, $T_{\rm shell}$, shown in Table \ref{tab:table}. Waves He and C burning phases, $J_{\rm ex} \sim J_0$, indicating IGW  may be able to significantly  spin down the core to angular frequencies $\omega_*$ as long as $t_*$ is shorter than core. {\bf Bottom:} Spin periods $P_0$ of our model in  the time until death. In this case, absence of angular momentum transport. As star evolves,  the value of $\omega_*$ at any radius represents $P_0$ decreases in  the maximum expected angular contracting core. We have also plotted the approximate minimum  spin frequency. periods $P_{\rm min}$ which may be enforced by IGW during the core He-burning and C-shell burning phases.