2023MNRAS.518.1557R

Magnetorotational supernovae are a rare type of core-collapse supernovae where the magnetic field and rotation play a central role in the dynamics of the explosion. We present the post-processed nucleosynthesis of state-of-the-art neutrino-MHD supernova models that follow the post explosion evolution for few seconds. We find three different dynamical mechanisms to produce heavy r-process elements: (i) a prompt ejection of matter right after core bounce, (ii) neutron-rich matter that is ejected at late times due to a reconfiguration of the protoneutronstar shape, (iii) small amount of mass ejected with high entropies in the centre of the jet. We investigate total ejecta yields, including the ones of unstable nuclei such as ²⁶Al, ⁴⁴Ti, ⁵⁶Ni, and ⁶⁰Fe. The obtained ⁵⁶Ni masses vary between $0.01\!-\!1\, \mathrm{M_\odot }$. The latter maximum is compatible with hypernova observations. Furthermore, all of our models synthesize Zn masses in agreement with observations of old metal-poor stars. We calculate simplified light curves to investigate whether our models can be candidates for superluminous supernovae. The peak luminosities obtained from taking into account only nuclear heating reach up to a few $\sim 10^{43} \, \mathrm{erg\, s^{-1}}$. Under certain conditions, we find a significant impact of the ⁶⁶Ni decay chain that can raise the peak luminosity up to $\sim 38{{\ \rm per \, cent}}$ compared to models including only the ⁵⁶Ni decay chain. This work reinforces the theoretical evidence on the critical role of magnetorotational supernovae to understand the occurrence of hypernovae, superluminous supernovae, and the synthesis of heavy elements.