  Recent evidence of the phenomenal energetics involved in gamma ray burst
events strongly suggests that the progenitor must efficiently convert
gravitational binding energy into a moderately collimated outflow, possibly in
the form of a Poynting jet. We show that an MHD-instability driven dynamo (IDD)
operating in a hot accretion disk is capable of generating energetically
adecuate 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. In
the comoving frame of a semi-thick, slim disk setting, the predominant field
components reside in surfaces perpendicular to the local meridian and the flux
is deposited in funnels that are relatively free of baryons. The efficiency of
magnetic energy deposition is estimated to be comparable to the neutrino losses
but the strong effective shear induced by the metric on the MRI favors pumping
magnetic field energy at low wavenumbers, i.e., field generation at large
coherence lengthscales. This, in turn, suggests that an MHD collimation
mechanism may deem this process a more viable alternative to
neutrino-burst--driven models of gamma ray bursts.
