  Binary-driven-hypernovae (BdHNe) within the induced gravitational collapse
(IGC) paradigm have been introduced to explain energetic ($E_{\rm iso}\gtrsim
10^{52}$~erg), long gamma-ray bursts (GRBs) associated with type Ic supernovae
(SNe). The progenitor is a tight binary composed of a carbon-oxygen (CO) core
and a neutron star (NS) companion, a subclass of the newly proposed
"ultra-stripped" binaries. The CO-NS short-period orbit causes the NS to
accrete appriciable matter from the SN ejecta when the CO core collapses,
ultimately causing it to collapse to a black hole (BH) and producing a GRB.
These tight binaries evolve through the SN explosion very differently than
compact binaries studied in population synthesis calculations. First, the
hypercritical accretion onto the NS companion alters both the mass and momentum
of the binary. Second, because the explosion timescale is on par with the
orbital period, the mass ejection can not be assumed to be instantaneous. This
dramatically affects the post-SN fate of the binary. Finally, the bow shock
created as the accreting NS plows through the SN ejecta transfers angular
momentum, braking the orbit. These systems remain bound even if a large
fraction of the binary mass is lost in the explosion (well above the canonical
50\% limit), and even large kicks are unlikely to unbind the system. Indeed,
BdHNe produce a new family of NS-BH binaries unaccounted for in current
population synthesis analyses and, although they may be rare, the fact that
nearly 100\% remain bound implies they may play an important role in the
compact merger rate, important for gravitational waves (GWs) that, in turn, can
produce a new class of ultrashort GRBs.

High Energy Astrophysical Phenomena