  We perform spherically symmetric simulations of the core collapse of a single
progenitor star of zero age main sequence mass $M_{\rm ZAMS} = 15 \, M_{\odot}$
with two models of heavy sterile neutrinos in the mass range of hundred
MeV$/c^2$. According to both models, these hypothetical particles are copiously
produced in the center, stream outwards a subsequently decay releasing energy
into final states (including neutrinos) of the Standard Model. We find that
they can lead to a successful explosion in otherwise non-exploding progenitors.
Depending on their unknown parameters (e.g., mass and coupling constants with
matter), we obtain either no explosion or an explosion of one of two types,
i.e., through heating of gas downstream of the stalled shock wave, similarly to
the standard scenario for supernova explosions or through heating of gas at
higher radii that ejects matter from the outer core or the envelope while the
center continues to accrete matter. In both cases, the explosion energies can
be very high. We presume that this new type of explosion would produce an
electromagnetic signal that significantly differs from common events because of
the relative absence of heavy elements in the ejecta. The combination of
core-collapse simulations and astrophysical observations may further constrain
the parameters of the sterile neutrinos.
