it is produced in greater quantity father out in the star. However, the details of observational prospects depend on the extent of ejecta mixing, and the life span of the isotopes. These details are discussed in Section \[sec:observations\]. Furthermore, nuclear uncertainties may also play an important role in affecting the production of these radioactive species. For instance, and production will strongly depend on neutron capture reaction rates of and , that are not experimentally known.

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###  and 

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![image](M15_SC47_EnergyAbus.pdf){width=".32\linewidth"} ![image](M20_SC47_EnergyAbus.pdf){width=".32\linewidth"} ![image](M25_SC47_EnergyAbus.pdf){width=".32\linewidth"}

The bulk of in a supernova is produced through the decay of . However, because of the 60y half-life of , the gamma-rays at early times from the decay of will be dominated by direct production, rather than this decay product. However, depending upon the amount of isomeric produced (we only consider the ground state), directly-produced is only important in the first few days. The direct production site of the proton-rich is dominated by the interior core while the production of the neutron-rich is dominated by the burning layers. Though is primarily produced in the core and the innermost C/O shell, there exists significant production of in the He shell. The 