be observed in a supernova explosion depending on the extent of ejecta mixing, as discussed later in Section \[sec:observations\].

### Probes of the Supernova Explosion {#sec:probesnexp}

![image](K43_EnergyLines_linlog.pdf){width="32.00000%"} ![image](CA47_EnergyLines_linlog.pdf){width="32.00000%"} ![image](FE59_EnergyLines_linlog.pdf){width="32.00000%"}

As we discussed in Section \[sec:understanding\], the stronger the explosion energy, the higher the post-shock temperature. This can both destroy and create more of any given isotope. Isotopes that are good indicators of the explosion energy are ones where increasing the shock energy always produces more than it destroys. Examples of such isotopes that are ideal probes of the energy include $^{43}$K, $^{47}$Ca, and , which are shown in Figure \[fig:eexp\_probes\].

Detailed Discussion of Individual Yields
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We now examine in more detail the yields of each radioisotope.

###  and 

For the Alkali and Alkali Earth Metals, the neutron rich isotopes and , production is dominated in the burning shells. Though these isotopes are destroyed in the inner core, they are produced in greater quantity in the burning layers by neutron captures triggered by the activation of the Ne22(a,n)Mg25 before and during the SN explosion. Both of these isotopes have very similar initial abundance and production site patterns, as seen in Figure \[fig:alkali\]. Both isotopes demonstrate an energy dependant production in 