Internal conversion electrons and supernova light curves

TL;DR

This paper highlights the importance of internal conversion electrons in supernova light curves, showing they significantly contribute to heating and affect the interpretation of nucleosynthetic yields, especially at late times.

Contribution

It introduces internal conversion electrons as a crucial heat source in supernovae, expanding beyond gamma-ray and positron contributions in previous models.

Findings

Internal conversion electrons significantly influence supernova light curves.

Accounting for these electrons explains the light curve slowing in SN 1998bw and SN 2003hv.

They are important for accurately deriving 44Ti yields from SN 1987A data.

Abstract

Radioactive decays contribute significantly to the re-heating of supernova ejecta. Previous works mainly considered the energy deposited by gamma-rays and positrons produced by 56Ni, 56Co, 57Ni, 57Co, 44Ti, and 44Sc. We point out that Auger and internal conversion electrons constitute an additional heat source. At late times, these electrons can contribute significantly to supernova light curves for reasonable nucleosynthetic yields. In particular, the internal conversion electrons emitted in the decay of 57Co are an important heating channel for supernovae that have become largely transparent to gamma-rays. We show that when the heating by these electrons is accounted for, the slowing down of the light curves of SN 1998bw and SN 2003hv is naturally obtained for typical nucleosynthetic yields. Additionally, we show that for SN 1987A the effects of internal conversion electrons are likely significant for the derivation of 44Ti yields from its late time bolometric light curve.