56.5%
  t$_{1/2}=$44.49 d                  1291.6 keV           43.2%
  $\rightarrow$                      1377.6 keV           81.7%
  t$_{1/2}=$35.6 h                  1919.52 keV           12.3%
  $\rightarrow$                      6.391 keV            16.6%
  t$_{1/2}=$271.74 d                 6.404 keV            32.9%
                                     122.1 keV            85.6%
                                     136.5 keV            10.7%
  $\rightarrow$                      1808.7 keV           99.8%
  t$_{1/2}=7.17 \times 10^5$ y                      

  : List of the radioactive nuclei and their decay lines used in this study.

\[tab:decay\]

Basic Trends in the Yields
--------------------------

### Understanding the Yields of Radioactive Isotopes {#sec:understanding}

![Mass fraction of as a function of mass coordinate for each explosion scenario (color indicated by explosion energy color bar), the average of the explosions (black dashed), and the initial abundances (magenta) for our 25 solar mass progenitor. The dashed vertical lines denote the edge of the iron core (see Figure \[fig:progenitors\]. With strong explosion energies, is produced further out, but there is not a decisive trend in the total mass produced as a function of energy.[]{data-label="fig:exampleenergy1"}](M25_NI57_EnergyAbus_zoomed.pdf){width="\linewidth"}

We expect the nucleosynthetic yields to probe both the stellar structure and the supernova explosion because the nucleosynthetic yields depend on the temperature and density evolution, both the peak temperatures and densities and the subsequent evolution. The temperature and density after the supernova shock ($T_{\rm peak},\rho_{\rm peak}$) can be determined in the strong shock limit: $$a/3 