Although spokes were observed frequently during the Voyager encounters, they were not seen during the Cassini mission until September 2005, possibly an indication of the effect of a different Sun angle on the production of charged grains.
The charging profiles of micron- and submicron-sized dust grains immersed in such plasma environments are strongly size- and temperature-dependent, and under certain conditions, the dust cloud can have various configurations of charged grains.
The authors described briefly the possibility of charged grains forming a Coulomb lattice.
Because of different types of dust charged grains in a plasma, a number of different wave modes are introduced, for example, dust acoustic mode [8], dust ion acoustic mode [9], dust lattice mode [10], Shukla Varma mode [11], dust Berstain Green Kruskal mode [12] and dust drift mode [13].
Using a standard grain charging model along with a modified Barnes–Hut tree code for calculating grain dynamics, this paper examines the effect of including initial grain charging in coagulation of clouds of negative grains, positive grains, and a mixture of oppositely charged grains.
Surface charging causes the electrostatic transport of charged dust grains.
The chapter also discusses the wake-potential and the associated attractive force that is responsible for the Coulomb crystallization of charged dust grains.
The outcome from the present study have direct implications to the analysis of plasma sheath structure and associated distribution in space of charged dust grains, which is relevant to the moon exploration near the optical terminator region or in shadowed craters in the moon.
The numerical model calculates the dynamics of charged dust grains and includes forces due to Saturn's gravitational field, the plasma polarization electric field, a third order harmonic expansion of Saturn's magnetic field, and the F-Ring's Shepherding moons, Prometheus and Pandora.
However, the presence of charged dust grains in a plasma gives rise to very low-frequency new mode (~10 15 Hz), called dust acoustic wave (DAW) [4, 5, 6, 7, 8], where the inertia is provided by the charged and massive dust grains.
From panels (a, b) it is clear that as (mu) increases, i.e., as the number of charged dust grains decreases, a part of the instability region (with (theta
