The induced gravitational collapse ( IGC ) paradigm explains a class of energetic , E _ { iso } \gtrsim 10 ^ { 52 } Â erg , long-duration gamma-ray bursts ( GRBs ) associated with Ic supernovae , recently named binary-driven hypernovae ( BdHNe ) .
The progenitor is a tight binary system formed of a carbon-oxygen ( CO ) core and a neutron star companion .
The supernova ejecta of the exploding CO core trigger a hypercritical accretion process onto the neutron star , which reaches in a few seconds the critical mass , and gravitationally collapses to a black hole emitting a GRB .
In our previous simulations of this process we adopted a spherically symmetric approximation to compute the features of the hypercritical accretion process .
We here present the first estimates of the angular momentum transported by the supernova ejecta , L _ { acc } , and perform numerical simulations of the angular momentum transfer to the neutron star during the hyperaccretion process in full general relativity .
We show that the neutron star : i ) reaches in a few seconds either mass-shedding limit or the secular axisymmetric instability depending on its initial mass ; ii ) reaches a maximum dimensionless angular momentum value , [ cJ / ( GM ^ { 2 } ) ] _ { max } \approx 0.7 ; iii ) can support less angular momentum than the one transported by supernova ejecta , L _ { acc } > J _ { NS,max } , hence there is an angular momentum excess which necessarily leads to jetted emission .