  In this paper, the dynamical analysis of the Jovian dust originating from the
four Galilean moons is presented. High accuracy orbital integrations of dust
particles are used to determine their dynamical evolution. A variety of forces
are taken into account, including the Lorentz force, solar radiation pressure,
Poynting-Robertson drag, solar gravity, the satellites' gravity, plasma drag,
and gravitational effects due to non-sphericity of Jupiter. More than 20,000
dust particles from each source moon in the size range from 0.05 micron to 1 cm
are simulated over 8,000 (Earth) years until each dust grain hits a sink
(moons, Jupiter, or escape from the system). Configurations of dust number
density in the Jovicentric equatorial inertial frame are calculated and shown.
In a Jovicentric frame rotating with the Sun the dust distributions are found
to be asymmetric. For certain small particle sizes, the dust population is
displaced towards the Sun, while for certain larger sizes, the dust population
is displaced away from the Sun. The average lifetime as a function of particle
size for ejecta from each source moon is derived, and two sharp jumps in the
average lifetime are analyzed. Transport of dust between the Galilean moons and
to Jupiter is investigated. Most of the orbits for dust particles from Galilean
moons are prograde, while, surprisingly, a small fraction of orbits are found
to become retrograde mainly due to solar radiation pressure and Lorentz force.
The distribution of orbital elements is also analyzed.
