  Using binary evolution with Case-C mass transfer, the spins of several black
holes (BHs) in X$-$ray binaries (XBs) have been predicted and confirmed (three
cases) by observations. The rotational energy of these BHs is sufficient to
power up long gamma$-$ray bursts and hypernovae (GRBs/HNe) and still leave a
Kerr BH behind. However, strong magnetic fields and/or dynamo effects in the
interior of such stars deplete their cores from angular momentum preventing the
formation of collapsars. Thus, even though binaries can produce Kerr BHs, most
of their rotation is acquired from the stellar mantle, with a long delay
between BH formation and spin up. Such binaries would not form GRBs. We study
whether the conditions required to produce GRBs can be met by the progenitors
of such BHs. Tidal-synchronization and Alfv\'en timescales are compared for
magnetic fields of different intensities threading He stars. A search is made
for a magnetic field range which allows tidal spin up all the way in to the
stellar core but prevents its slow down during differential rotation phases.
The energetics for producing a strong magnetic field during core collapse,
which may allow for a GRB central engine, are also estimated. An
observationally-reasonable choice of parameters is found ($B \lesssim10^2$ G
threading a slowly-rotating He star) which allows Fe cores to retain
substantial angular momentum. Thus, the Case-C-mass-transfer binary channel is
capable of explaining long GRBs. However, the progenitors must have low initial
spin and low internal magnetic field throughout their H-burning and He-burning
phases.
