  The SN explosion in the closed binary can give the magnetospheric flare
possessing the properties of GRB. The SN shock, flowing around the
magnetosphere of a magnetized neutron star or a white dwarf, produces a narrow
magnetic tail 10^9 cm long, 10^8 cm wide and a magnetic field of 10^6 Gauss.
Fast particles (Lorentz factor of 10^4), generated in the tail by reconnection
processes, radaite gamma rays of the 100 KeV - 1 MeV energies. The duration of
radiation T<1 sec corresponds to a short GRB. Apart, the powerful shock can
tear and accelerate part of the tail. That is the relativistic, strongly
magnetized jet, producing gamma radiation and also X-rays and optic afterglow.
That is long (T> 10 sec) GRB. The duration of the afterglow is inversly
proportional to the photon energy and is several months for optic.
