  Among supernovae (SNe) of different luminosities, many double-peaked light
curves (LCs) have been observed, representing a broad morphological variety. In
this work, we investigate which of these can be modelled by assuming a
double-peaked distribution of their radioactive material, as originally
proposed for SN2005bf. The inner zone corresponds to the regular explosive
nucleosynthesis and extends outwards, according to the usual scenario of
mixing. The outer 56Ni-rich shell may be related to the effect of jet-like
outflows that have interacted with more distant portions of the star before the
arrival of the SN shock. As the outer layer is covered by matter that is
optically less thick, its energy emerges earlier and generates a first peak of
radiation. To investigate this scenario in more detail, we have applied our
hydrodynamic code that follows the shock propagation through the progenitor
star and takes into account the effect of the gamma-ray photons produced by the
decay of the radioactive isotopes. We present a simple parametric model for the
56Ni abundance profile and explore the consequences on the LC of individually
varying the quantities that define this distribution, setting our focus onto
the stripped-envelope progenitors. In this first study, we are interested in
the applicability of this model to SNe that have not been classified as
superluminous, thus, we have selected our parameter space accordingly. Then,
within the same mathematical prescription for the 56Ni-profile, we revisited
the modelling process for a series of objects: SN2005bf, PTF2011mnb, SN2019cad,
and SN2008D. In some cases, a decrease in the gamma ray opacity is required to
fit the late time observations. We also discuss the other cases in which this
scenario might be likely to explain the LC morphology.
