A raft of papers in the last decade has advanced our understanding of the physics of floating sea ice covering tens of millions of kilometers of Earth's ocean. Seeding this research has been the need to quantify sea ice's role in global ocean circulation, a need to understand the stability of the ice through time, and interest in the ice itself as an ecological niche. One recent 1D model, by Buffo et al. (2018), captures the gravity drainage of brines initially entrained within forming ice, which flow through interconnected pores and melt channels within the ice. In follow-on work that was just published, Buffo et al. (2020) have extended their model to estimate the entrainment and transport of salts in the ice covering Jupiter's moon Europa. This type of work is timely, as the community of planetary scientists studying Europa and related ocean worlds sets its sails for NASA's Europa Clipper mission (Howell & Pappalardo, 2020), and ESA's JUpiter ICy moons Explorer (JUICE) mission (Grasset et al., 2013), planned to arrive at the Jupiter system toward the end of this decade. However, the work poses many further questions that will need to be addressed in the coming years. Europa's ice is global, and at least 3 km thick-possibly 30 km or more-covering an ocean as deep as 180 km (Anderson et al., 1998, Turtle & Pierazzo, 2001; Schenk et al., 2002). Sparse crater counts among the fractured ice suggest the average age of surface materials is less than 200 Myr (Zahnle et al., 2003). Materials retained in the ice could provide clues to the ocean's thermal and chemical evolution, its current composition, and the possible presence of life. Demonstrating mechanisms for extensive material entrainment into the ice would also support the existence of brine reservoirs near Europa's surface, hypothesized to explain the chaotic terrains covering much of Europa's surface (