  Short Gamma-Ray Bursts (GRBs) are explosions of cosmic origin believed to be
associated with the merger of two compact objects, either two neutron stars, or
a neutron star and a black hole. The presence of at least one neutron star has
long been thought to be an essential element of the model: its tidal disruption
provides the needed baryonic material whose rapid accretion onto the
post-merger black hole powers the burst. The recent tentative detection by the
Fermi satellite of a short GRB in association with the gravitational wave
signal GW150914 produced by the merger of two black holes has challenged this
standard paradigm. Here we show that the evolution of two high-mass,
low-metallicity stars with main sequence rotational speeds a few tens of
percent of the critical speed eventually undergoing a weak supernova explosion
{\em can} produce a short gamma-ray burst. The outer layers of the envelope of
the last exploding star remain bound and circularize at large radii. With time,
the disk cools and becomes neutral, suppressing the magneto-rotational
instability, and hence the viscosity. The disk remains 'long-lived dead' until
tidal torques and shocks during the pre-merger phase heat it up and re-ignite
accretion, rapidly consuming the disk and powering the short gamma-ray burst.
