  We investigate whether the regular Galilean satellites could have formed in
the dead zone of a circumplanetary disc. A dead zone is a region of weak
turbulence in which the magnetorotational instability (MRI) is suppressed,
potentially an ideal environment for satellite formation. With the grid-based
hydrodynamic code, FARGO3D, we examine the evolution of a circumplanetary disc
model with a dead zone. Material accumulates in the dead zone of the disc
leading to a higher total mass and but a similar temperature profile compared
to a fully turbulent disc model. The tidal torque increases the rate of mass
transport through the dead zone leading to a steady state disc with a dead zone
that does not undergo accretion outbursts. We explore a range of disc, dead
zone and mass inflow parameters and find that the maximum mass of the disc is
around 0.001 MJ . Since the total solid mass of such a disc is much lower, we
find that there is not sufficient material in the disc for in situ formation of
the Galilean satellites and that external supplement is required.
