Phase separation of planetary ices explains nondipolar magnetic fields of Uranus and Neptune

• 成果类型: Article
• 署名作者: Militzer, Burkhard
• 署名单位: University of California System; University of California Berkeley; University of California System; University of California Berkeley
• 刊物名称: PROCEEDINGS OF THE NATIONAL ACADEMY OF SCIENCES OF THE UNITED STATES OF AMERICA
• ISSN/ISSBN: 0027-15094
• DOI: 10.1073/pnas.2403981121
• 发表日期: 2024-12-03
• 关键词: hydrogen; models; water; interior

摘要

The Voyager spacecraft discovered that the ice giants Uranus and Neptune have nondipolar magnetic fields, defying expectations that a thick interior layer of planetary ices would generate strong dipolar fields. Stanley and Bloxham showed that nondipolar fields emerge if the magnetic field is only generated in a thin outer layer. However, the origin and composition of this dynamo active layer has so far remained elusive. Here, we show with ab initio computer simulations that a mixture of H2O, CH4, and NH3 will phase separate under the pressure-temperature condition in the interiors of Uranus and Neptune, forming a H2O-dominated fluid in the upper mantle and a CH4-NH3 mixture below. We further demonstrate that with increasing pressure, the CH4-NH3 mixture becomes increasingly hydrogen depleted as it assumes the state of a polymeric C-N-H fluid. Since the amount of hydrogen loss increases with pressure, we propose that the C-N-H fluid forms a stably stratified layer. The magnetic fields are primarily generated in an upper layer that is H2O-rich, homogeneous, convective, and electrically conducting. Under these assumptions, we construct ensembles of models for the interiors of Uranus and Neptune with the Concentric MacLaurin Spheroid method. We demonstrate that the phase separation of the solar-type H2O-CH4-NH3 mixture leads to models that match the observed gravity field and to layer thicknesses that are compatible with magnetic field measurements.