  We show that an MHD-instability driven dynamo (IDD) operating in a hot
accretion disk is capable of generating energetically adequate magnetic flux
deposition rates above and below a mildly advective accretion disk structure.
  The dynamo is driven by the magnetorotational instability (MRI) of a toroidal
field in a shear flow and is limited by the buoyancy of `horizontal' flux and
by reconnection in the turbulent medium. The efficiency of magnetic energy
deposition is estimated to be comparable to the neutrino losses although an MHD
collimation mechanism may deem this process a more viable alternative to
neutrino-burst-driven models of gamma ray bursts.
