On quark deconfinement in the accreting neutron stars of binarydriven hypernovae

In the binary-driven hypernova (BdHN) scenario, long gamma-ray bursts (GRBs) originate in a binary system composed of a carbon-oxygen (CO) star and a neutron star (NS) companion in close orbit. The collapse of the CO star generates a newborn NS (νNS) at its center and a type Ic supernova (SN) explosion. Part of the SN ejecta is accreted onto the NS companion and onto the νNS by fallback. The accretion process occurs at hypercritical (highly super-Eddington) rates, transferring mass and angular momentum to the stars. We here assess whether or not quark deconfinement can occur either in the νNS or in the NS companion during the hypercritical accretion process.