  We suggest that the energetic radiation from core-collapse super-energetic
supernovae (SESNe) is due to a long lasting accretion process onto the newly
born neutron star (NS), resulting from an inefficient operation of the
jet-feedback mechanism. The jets that are launched by the accreting NS or black
hole (BH) maintain their axis due to a rapidly rotating pre-collapse core, and
do not manage to eject core material from near the equatorial plane. The jets
are able to eject material from the core along the polar directions, and reduce
the gravity near the equatorial plane. The equatorial gas expands, and part of
it falls back over a timescale of minutes to days to prolong the jets-launching
episode. According to the model for SESNe proposed in the present paper, the
principal parameter that distinguishes between the different cases of CCSN
explosions, such as between normal CCSNe and SESNe, is the efficiency of the
jet-feedback mechanism. This efficiency in turn depends on the pre-collapse
core mass, envelope mass, core convection, and most of all on the angular
momentum profile in the core. One prediction of the inefficient jet-feedback
mechanism for SESNe is the formation of a slow equatorial outflow in the
explosion. Typical velocity and mass of this outflow are estimated to be
approximately 1000 km/s and greater than about 1 solar mass, respectively,
though quantitative values will have to be checked in future hydrodynamic
simulations.
