Coupling Eruptive Dynamics Models to Multi-fluid Plasma Dynamic Simulations at Enceladus

Details Coupling Eruptive Dynamics Models to Multi-fluid Plasma Dynamic Simulations at Enceladus Coupling Eruptive Dynamics Models to Multi-fluid Plasma Dynamic Simulations at Enceladus

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsm21b2017p&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SM21B-2017

Physics

[2732] Magnetospheric Physics / Magnetosphere Interactions With Satellites And Rings, [5421] Planetary Sciences: Solid Surface Planets / Interactions With Particles And Fields, [6063] Planetary Sciences: Comets And Small Bodies / Volcanism, [6280] Planetary Sciences: Solar System Objects / Saturnian Satellites

Scientific paper

The interaction of Saturn's magnetosphere with Enceladus provides an exciting natural laboratory for expanding our understanding of charge-neutral-dust interactions and their impact on mass and momentum loading of the system and the associated magnetic perturbations. However, one of the more challenging questions regarding the Enceladus plume relates to the subsurface eruptive mechanism responsible for generating the observed jets of material that compose the plume, and the three-dimensional distribution of neutral gas and dust in the plume. In this work we implement a multiphase eruptive dynamics model [cf. Dufek & Bergantz, 2007; Dufek and Bergantz, 2005] to examine the evolution of the plume morphology for a given eruption. We model the eruptive mechanism in a two-part, coupled domain including a fissure model and a plume model. A high resolution, multiphase, fissure model examines eruptive processes in a fissure from fragmentation to the surface. The fissure model is two-dimensional and provides spatial and temporal information about the dust/ice grains and gas. The depth to the fragmentation surface is currently treated as a free parameter and we examine a range of fissure morphologies. We do not explicitly force choked conditions at the vent, but rather due to the geometry, the velocities of the particle and gas mixture approach the sound speed for a 'dusty' gas mixture. The fissure model provides a source for the 3D plume model which examines the morphology of the plume resulting from different fissure configurations and provides a self-consistent physical basis to link concentrations in different regions of the plume to an eruptive mechanism. These initial models describing the resulting gas and dust grain distribution will be presented in the context of existing observations. We will also demonstrate the first stages of integration of these results into the existing multi-fluid plasma dynamic simulations of Enceladus' interaction with Saturn's magnetosphere. These more sophisticated plume morphologies and their effects on the plasma dynamic interaction will be assessed in the context of existing modeling efforts for this system.

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