Abstract
The γ-ray deposition in supernovae is calculated by solving the Spencer-Fano equation. Ionization, excitation, and heating rates are presented for the different chemical composition zones of a core collapse supernova, as well as for a solar composition applicable to for example, active galactic nuclei. The thermalization in pure helium, oxygen, and iron plasmas is also discussed. The latter is of particular interest for Type Ia supernovae. Convenient analytical expressions are given to facilitate the use of these results for the calculation of the physical conditions and emission from supernovae
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