The low luminosity of Uranus is still a puzzling phenomenon and has key implications for the thermal and compositional gradients within the planet. Recent studies have shown that planetary volatiles become ionically conducting under conditions that are present in the ice giants. Rapidly growing electrical conductivity with increasing depth would couple zonal flows to the background magnetic field in the planets, inducing poloidal and toroidal field perturbations $\mathbf{B}^ω = \mathbf{B}^ω_P + \mathbf{B}^ω_T$ via the $ω$-effect. Toroidal perturbations $\mathbf{B}^ω_T$ are expected to diffuse downwards and produce poloidal fields $\mathbf{B}^α_P$ through turbulent convection via the $α$-effect, comparable in strength to those of the $ω$-effect; $\mathbf{B}^ω_P$. To estimate the strength of poloidal field perturbations for various Uranus models in the literature, we generate wind decay profiles based on Ohmic dissipation constraints assuming an ionically conducting H$_2$-He-H$_2$O interior. Due to the higher metallicities in outer regions of hot Uranus models, zonal winds need to decay to $\sim$0.1% of their surface values in the outer 1% of Uranus to admit decay solutions in the Ohmic framework. Our estimates suggest that colder Uranus models could potentially have poloidal field perturbations that reach up to $\mathcal{O}(0.1)$ of the background magnetic field in the most extreme case. The possible existence of poloidal field perturbations spatially correlated with Uranus' zonal flows could be used to constrain Uranus' interior structure, and presents a further case for the $\textit{in situ}$ exploration of Uranus.
Detection of stratospheric HCN and tropospheric CO in Uranus and the implication for their sources
Univ. Bordeaux（波尔多大学）；Observatoire de Paris（巴黎天文台）；New York University（纽约大学）；American Museum of Natural History（美国自然历史博物馆）；Max-Planck-Institut für Astronomie（马克斯·普朗克天文学研究所）；Aix-Marseille Université（艾克斯-马赛大学）；University of Liège（列日大学）；Sorbonne Université（索邦大学）；Institut Pierre-Simon Laplace（皮埃尔-西蒙·拉普拉斯研究所）；Instituto de Astrofísica de Andalucía (IAA), CSIC（安达卢西亚天体物理研究所，西班牙高等科学研究委员会）；University of California, Berkeley（加州大学伯克利分校）；National Radio Astronomy Observatory（国家射电天文台）
Solar Magnetic Configuration Control over Radiation Belt Electrons
Northumbria University（诺森比亚大学）；University College London, Mullard Space Science Laboratory（伦敦大学学院穆拉德空间科学实验室）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；Johns Hopkins University, Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）
