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Jim Fuller edited Figure_refMassiveIGW.tex
about 9 years ago
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Figure \ref{fig:MassiveIGWtime} shows profiles of $\omega_*(r)$ and $t_*(r)$ at different stages of evolution in our stellar model. We have also shown the time until CC at each stage. Since each stage is much longer than subsequent stages (i.e., He core burning lasts for much longer than C-shell burning, etc.), the time until CC is also a good estimate of the duration of each evolutionary stage. Our results indicate that typical IGW spin-down times are shorter than the evolutionary time during most evolutionary stages. Therefore, IGW emitted from overlying convective regions can likely spin down the core, preventing it from spinning up as it contracts. The values of $\omega_*(r)$ near the core in Figure \ref{fig:MassiveIGWtime} therefore represent maximum angular spin frequencies obtainable by the core during the corresponding stage of evolution.
