The presence of liquid water has long guided the search for life beyond Earth (Des Marais et al., 2003). Once thought to be confined to the "Goldilocks zone," vast oceans have been inferred to exist beneath the thick ice shells of moons in the outer solar system (Hand et al., 2020). Although these sub-ice oceans represent the most compelling potential habitats in the outer solar system (Shematovich, 2018), they are covered by ice shells that can range from kilometers to hundreds of kilometers thick (Soderlund et al., 2020). Impurities within the ice shell, such as salts, acids, or organic compounds, could allow for liquid water to remain stable at temperatures well below that predicted by the pressure-melting curve of pure water (Marion et al., 2003(Marion et al., , 2005Ruiz et al., 2007). These impurities support the formation of intra-ice shell brine pockets, which could represent potential habitats that might be more accessible than the sub-ice ocean (Kargel et al., 2000;Marion et al., 2003).Estimating the distribution of brine in an ice shell represents an important step in studying the habitability of ocean worlds. The brine volume fraction governs a number of bulk ice thermophysical properties, such as density, thermal conductivity, specific heat capacity, and viscosity (Petrich & Eicken, 2017). These thermophysical properties in turn govern processes of surface-ice-ocean exchange (e.g., solid-state convection, subduction, diapirism),