Overview
- A UCLA team has submitted a study to The Astrophysical Journal that models Uranus and Neptune with a hydrogen/helium envelope, a mixed boundary layer of H, He, Mg and SiO, and a deep silicate-iron magma ocean.
- The simulations show hydrogen can dissolve into high‑pressure magma to create a well-mixed fluid that helps match the planets' bulk densities and unusual magnetic and heat-flow signatures.
- Authors say the magma‑ocean model is one plausible explanation among others and that its conclusions come from computer simulations rather than new spacecraft data.
- Voyager 2 remains the only spacecraft to visit these planets, and proposed missions such as the Uranus Orbiter and Probe and Neptune Odyssey are concepts that would be needed to test the model directly.
- If the model holds up, it would change how scientists link Solar System ice giants to common sub‑Neptune exoplanets and could prompt new thinking about how these planets form and retain rock-rich interiors.