ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software O B-Model I-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Software O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O B-Model O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O
tokens: shells, with secondary typical scales as small as (0.5–1) × 10 9 cm. The slope of the VSH power spectra stays consistent over time regardless of the presence or absence of rotation. In all cases we find nearly circular shapes for the characteristic convective elements. In terms of the 2D convective flow properties, our results are in agreement with those of Meakin Arnett ( 2007 ; see also Meakin et al. 2015 ; Cristini et al. 2016 ). In particular, we find a highly intermittent flow and mixing due to turbulent entrainment. In terms of the effects of rotation on the strength and properties of convection alone we find our 2D simulations suggest minimal impact and generally lead to an overall small reduction of the total convective power stored in solenoidal motions (“no-rot” versus “rot-2” models) regardless of the nature of convective burning (C, O, or Si shell). We suggest this is due to the effects of the centrifugal forces mildly expanding the star, and thus changing the locations of the convective shells over time, subjecting the shell material to lower temperatures that, in turn, trigger lower nuclear burning rates and weaker convection. That alone may lead to initial velocity perturbations of smaller amplitude than in the case of zero rotation which may have a small impact on the susceptibility to a successful SN explosion following iron core collapse (Couch Ott 2013 ). We emphasize that, to answer the question of whether the inclusion of rotation significantly changes the ICs to the core-collapse SN mechanism, self-consistent evolution with the effects of rotation included is the proper approach to take. In our analysis we have followed the evolution of a 20 M ⊙ SN progenitor with both the effects of rotation and magnetic fields included in the transport of angular momentum and chemical mixing using the MESA code (“rot-ST” models). We find differences in the sign of the effect depending on the nature of convective shell-burning: during C- O-shell burning there is more power stored in the solenoidal components than in the case of no rotation while during Si-shell burning the effects are very small, with hints of even reduction of the solenoidal mode power by the end of the simulation. We attribute this effect to differences in the initial MESA models for the two distinct shell-burning stages. A careful look in the upper panel of Figure 2 shows that the “rot-ST” nuc profile during C- O-shell burning has a secondary peak (due to O-burning) that is nearly an order of magnitude greater than the corresponding one for the “no-rot” model. On the contrary, in Figure 3 we see that during Si-shell burning the peaks in the nuc profile for the “no-rot” model in the region (4–6) × 10 8 cm are greater than the corresponding ones for “rot-ST.” This is due to the enhanced chemical mixing by the ST mechanism during the C- O-shell burning phase that effectively recycles fresh fuel from outer layers to deeper and hotter regions enabling faster specific