  The binary-driven hypernova (BdHN) model address long gamma-ray bursts (GRBs)
associated with type Ic supernovae (SNe) through a series of physical episodes
that occur in a binary composed of a carbon-oxygen (CO) star (of mass about 10
solar mass) and a neutron star (NS) companion (of mass about 2 solar mass) in a
compact orbit. The SN explosion of the CO star triggers sequence of seven
events. The BdHN model has followed the traditional picture of the SN from the
CO iron's core collapse. However, the lack of a solution to the problem of
producing successful SNe leaves room for alternative scenarios. We here show
that tidal synchronization of the CO-NS binary can lead the CO star to critical
conditions for fission, hence splitting into two stellar remnants, e.g., about
8.5 solar mass + 1.5 solar mass. We give specific examples of the properties of
the products for various orbital periods relevant to BdHNe. The astrophysical
consequences of this scenario are outlined.
