Volume 628, August 2019
|Number of page(s)||8|
|Section||Stellar structure and evolution|
|Published online||25 July 2019|
A meta-analysis of core-collapse supernova 56Ni masses
European Southern Observatory, Alonso de Córdova 3107, Casilla 19, Santiago, Chile
Accepted: 3 June 2019
Context. A fundamental property determining the transient behaviour of core-collapse supernovae (CC SNe) is the amount of radioactive 56Ni synthesised in the explosion. Using established methods, this is a relatively easy parameter to extract from observations.
Aims. I provide a meta-analysis of all published 56Ni masses for CC SNe.
Methods. Collating a total of 258 literature 56Ni masses, I compared distributions of the main CC SN types: SNe II, SNe IIb, SNe Ib, SNe Ic, and SNe IcBL.
Results. Using these published values, I calculated a median 56Ni mass of 0.032 M⊙ for SNe II (N = 115), 0.102 M⊙ for SNe IIb (N = 27), 0.163 M⊙ for SNe Ib (N = 33), 0.155 M⊙ for SNe Ic (N = 48), and 0.369 M⊙ for SNe IcBL (N = 32). On average, stripped-enevelope SNe (SE-SNe: IIb, Ib, Ic, and Ic-BL) have much higher values than SNe II. These observed distributions are compared to those predicted from neutrino-driven explosion models. While the SN II distribution follows model predictions, the SE-SNe have a significant fraction of events with 56Ni masses much higher than predicted.
Conclusions. If the majority of published 56Ni masses are to be believed, these results imply significant differences in the progenitor structures and/or explosion properties between SNe II and SE-SNe. However, such distinct progenitor and explosion properties are not currently favoured in the literature. Alternatively, the popular methods used to estimate 56Ni masses for SE-SNe may not be accurate. Possible issues with these methods are discussed, as are the implications of true 56Ni mass differences on progenitor properties of different CC SNe.
Key words: supernovae: general / stars: massive
© ESO 2019
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