  We investigate the formation of hot and massive circumplanetary disks (CPDs)
and the orbital evolution of satellites formed in these disks. Because of the
comparatively small size-scale of the sub-disk, quick magnetic diffusion
prevents the magnetorotational instability (MRI) from being well-developed at
ionization levels that would allow MRI in the parent protoplanetary disk. In
the absence of significant angular momentum transport, continuous mass supply
from the parental protoplanetary disk leads to the formation of a massive CPD.
We have developed an evolutionary model for this scenario and have estimated
the orbital evolution of satellites within the disk. We find, in a certain
temperature range, that inward migration of a satellite can be stopped by a
change in the structure due to the opacity transitions. Moreover, by capturing
second and third migrating satellites in mean motion resonances, a compact
system in Laplace resonance can be formed in our disk models.
