Analyzing Ocean Currents on Icy Moons, Europa and Enceladus

Abstract
This study investigates the rotational dynamics of ocean currents on Jupiter’s and Saturn’s icy moons, Europa and Enceladus. The research aims to quantify the relationships between ocean depth, rotational forces, and the transit times of nano-sized silica particles. Numerical simulations were conducted to model the subsurface ocean dynamics of these moons. Python libraries, including Matplotlib for visualization and NetCDF for data management, were employed to process and analyze time-series data, enabling the examination of particle transit times in relation to varying ocean depths and rotational forces. The results demonstrate that the Rossby number governs particle transit times, adhering to distinct power laws: Ro−3/2^{-3/2}−3/2 for small Rossby numbers and Ro−2/3^{-2/3}−2/3 for large ones. Within the tangent cylinder—a region aligned with the moon’s axis of rotation—structured east-west zonal flows enhance particle transport, whereas regions outside exhibit less efficient, chaotic flow patterns. These findings provide insights into how rotational fluid mechanics influence material distribution in icy moon oceans, contributing to the understanding of their potential habitability.

Research Period
January 2022 – August 2022

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