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Many short GRBs show prompt tails lasting up to hundreds of seconds that canbe energetically dominant over the initial sub-second spike. In this paper wedevelop an electromagnetic model of short GRBs that explains the two stages ofthe energy release, the prompt spike and the prompt tail. The key ingredient ofthe model is the recent discovery that an isolated black hole can keep its openmagnetic flux for times much longer than the collapse time and, thus, canspin-down electromagnetically, driving the relativistic wind.  First, the merger is preceded by an electromagnetic precursor wind. If afraction of the wind power is converted into pulsar-like coherent radioemission, this may produce an observable radio burst of few milliseconds.  At the active stage of the merger, two neutron stars produces a black holesurrounded by an accretion torus in which the amplified magnetic field extractsthe rotational energy of the black hole and drives an axially-collimatedelectromagnetic wind. For observers nearly aligned with the orbital normal thisis seen as a classical short GRB.  After the accretion of the torus, the isolated black hole keeps the openmagnetic flux and drives the equatorially (not axially) collimated outflow,which is seen by an observer at intermediate polar angles as a prompt tail. Thetail carries more energy than the prompt spike, but its emission is de-boostedfor observers along the orbital normal. Observers in the equatorial plane missthe prompt spike and interpret the prompt tail as an energetic supernova-lesslong GRB.  We also demonstrate that episodic accretion onto the BH of magnetized cloudsthat carry non-zero magnetic flux can be highly efficient in extracting thespin energy of the BH, producing the outflows with the power exceeding theaverage accretion power.

The electromagnetic model of short GRBs, the nature of prompt tails, supernova-less long GRBs and highly efficient episodic accretion