Late-time supernova light curves

Abstract

Energy release from radioactive decays contributes significantly to supernova light curves. Previous works, which considered the energy deposited by γ-rays and positrons produced by 56Ni, 56Co, 57Ni, 57Co, 44Ti and 44Sc, have been quite successful in explaining the light curves of both core collapse and thermonuclear supernovae. We point out that Auger and internal conversion electrons, together with the associated X-ray cascade, constitute an additional heat source. When a supernova is transparent to γ-rays, these electrons can contribute significantly to light curves for reasonable nucleosynthetic yields. In particular, the electrons emitted in the decay of 57Co, which are largely due to internal conversion from a fortuitously low-lying 3/2- state in the daughter 57Fe, constitute an additional significant energy-deposition channel. We show that when the heating by these electrons is accounted for, a slow-down in the light curve of SN 1998bw is naturally obtained for typical hypernova nucleosynthetic yields. Additionally, we show that for generic Type Ia supernova yields, the Auger electrons emitted in the ground-state to ground-state electron capture decay of 55Fe exceed the energy released by the 44Ti decay chain for many years after the explosion. Show more