The magnetosphere of Uranus is far from well known since there was only one fly-by measurement in history. In order to study the magnetosphere and its coupling mechanism with the solar wind, we used our multifluid magnetohydrodynamics (MHD) model [Cao and Paty, 2017] to successfully simulate the variation of the global magnetosphere of Uranus and have predicted potential favorable reconnection locations.

The airborne dust has been well recognized to have a significant impact on the climate system at varying spatial scales (through direct, indirect, and semi-direct effects), on biochemistry (providing marine phytoplankton with iron nutrient), and on human health (causing severe disease) during the past decades. However, current estimations of these effects are still very uncertain because the dust cycle involves many complex physical and chemical processes in the atmosphere at different spatial and temporal scales, as well as the state of surfaces prone to the dust emission.

We present results from a three‐dimensional simulation model of the complex plasma environment near the Jovian moon Callisto. Beneath Callisto’s icy crust possibly lies a liquid saltwater ocean, properties of which can be constrained through magnetic induction signatures generated by Jupiter’s time‐varying magnetospheric field.