Abstract DGP2026-115

The Saturnian system with its active moon Enceladus is a key target for cosmic dust research.

Its dusty rings are fed by multiple processes that produce a complex dust environment.

For the E ring, cryovolcanic activity on Enceladus is the primary source, while additional 

dust populations are generated on all moons through impact ejecta processes.

 

Here we present first results from our ongoing effort to model the dust 

environment in the Saturnian system as part of an ESA activity to assess the hazards for space

missions. This also provides a wealth of opportunities to address scientific

questions. We present the results from our simulation runs covering a variety of source

moons, but also discuss the technical aspects of the model and the effort that went into

creating an adequate representation of Saturn's plasma environment for this activity.

 

The Saturn Dust model follows the trajectories of test particles

from source to sink. The particles are ejected in the plumes of

Enceladus feeding the E ring and in impact ejecta processes on the surfaces of airless bodies.

Their trajectories are numerically integrated taking into account all relevant forces, 

i.e. gravity, radiation pressure, Lorentz force, plasma drag, as well as sputtering and the

electric charging in the plasma environment. 

 

We give an overview of the first simulation results from various source moons, and

discuss aspects of the orbital dynamics of dust in this environment, as a result 

from our model.