\[fig:coreshell\]). More energetic explosions eject more of silicon layer (increasing the amount of material from this ejecta), but the additional heating can increase the destruction or production of isotopes in all layers. We will see that while for some species the production is dominated by one component (e.g., , from the explosive Si-buring/O-burning zones), most of radionuclides are efficiently made by at least two SN components.

![image](CA47_CoreShellFunc1.pdf){width=".32\linewidth"} ![image](K43_CoreShellFunc1.pdf){width=".32\linewidth"} ![image](FE59_CoreShellFunc1.pdf){width=".32\linewidth"}

The explosion energy not only determines the peak density and temperature of the ejecta, but also dictates how much material falls back onto the remnant and how much is ejected. Even if the material in core is heated extensively to produce an exciting set of radioactive isotopes, if it falls back onto the remnant, we will not observe these isotopes. The peak temperature and peak density of each explosion as functions of enclosed mass and explosion energy are illustrated in Figure \[fig:expparams\]. Not only does the innermost region of our 20M$_\odot$ star have a slightly lower pre-collapse density than our other stars. For the same explosion energy, the peak temperatures for matter at the same mass coordinate will be lower, affecting the yields. This explains differences in peak temperatures between the 