  We present the nucleosynthesis of magneto-rotational supernovae (MR-SNe)
including neutrino-driven and magneto-rotational-driven ejecta based, for the
first time, on 2D simulations with accurate neutrino transport. The models
analysed here have different rotation and magnetic fields, allowing us to
explore the impact of these two key ingredients. The accurate neutrino
transport of the simulations is critical to analyse the slightly neutron-rich
and proton-rich ejecta that are similar to the, also neutrino-driven, ejecta in
standard supernovae. In the model with strong magnetic field, the r-process
produces heavy elements up to the third r-process peak ($A\sim 195$), in
agreement with previous works. This model presents a jet-like explosion with
proton-rich jets surrounded by neutron-rich material where the r-process
occurs. We have estimated a lower limit for $^{56}$Ni of $2.5\times10^{-2}
M_\odot$, which is still well below the expected hypernova value. Longer
simulations including the accretion disc evolution are required to get a final
prediction. In addition, we have found that the late evolution is critical in a
model with weak magnetic field in which late-ejected neutron-rich matter
produces elements up to the second r-process peak. Even if we cannot yet
provide conclusions for hypernova nucleosynthesis, our results agree with
observations of old stars and radioactive isotopes in supernova remnants. This
makes MR-SNe a good additional scenario to neutron star mergers for the
synthesis of heavy elements and brings us closer to understand their origin and
the role of MR-SNe in the early Galaxy nucleosynthesis.
