  We present an overview of the formation of Jupiter and its associated
circumplanetary disk. Jupiter forms via a combination of planetesimal accretion
and gravitational accumulation of gas from the surrounding solar nebula. The
formation of the circumjovian gaseous disk, or subnebula, straddles the
transitional stage between runaway gas accretion and Jupiter's eventual
isolation from the solar disk. This isolation, which effectively signals the
termination of Jupiter's accretion, takes place as Jupiter opens a deep gas gap
in the solar nebula, or the solar nebula gas dissipates. We describe the
conditions for accretion of the Galilean satellites, including the timescales
for their formation, and mechanisms for their survival, all within the context
of key constraints for satellite formation models. The environment in which the
regular satellites form is tied to the timescale for circumplanetary disk
dispersal, which depends on the nature and persistence of turbulence. In the
case that subnebula turbulence decays as gas inflow wanes, we present a novel
mechanism for satellite survival involving gap opening by the largest
satellites. On the other hand, assuming that sustained turbulence drives
subnebula evolution on a short timescale compared to the satellite formation
timescale, we review a model that emphasizes collisional processes to explain
satellite observations. We briefly discuss the mechanisms by which solids may
be delivered to the circumplanetary disk. However, we expect that planetesimal
delivery mechanisms likely provide the bulk of material for satellite
accretion.
