  As the data from space missions and laboratories improve, a research domain
combining plasmas and charged dust is gaining in prominence. Our solar system
provides many natural laboratories such as planetary rings, comet comae and
tails, ejecta clouds around moons and asteroids, and Earth's noctilucent clouds
for which to closely study plasma-embedded cosmic dust. One natural laboratory
to study electromagnetically-controlled cosmic dust has been provided by the
Jovian dust streams and the data from the instruments which were on board the
Galileo spacecraft. Given the prodigious quantity of dust poured into the
Jovian magnetosphere by Io and its volcanoes resulting in the dust streams, the
possibility of dusty plasma conditions exist. This paper characterizes the main
parameters for those interested in studying dust embedded in a plasma with a
focus on the Jupiter environment. I show how to distinguish between
dust-in-plasma and dusty-plasma and how the Havnes parameter P can be used to
support or negate the possibility of collective behavior of the dusty plasma.
The result of applying these tools to the Jovian dust streams reveals mostly
dust-in-plasma behavior. In the orbits displaying the highest dust stream
fluxes, portions of orbits E4, G7, G8, C21 satisfy the minimum requirements for
a dusty plasma. However, the P parameter demonstrates that these mild dusty
plasma conditions do not lead to collective behavior of the dust stream
particles.
