Three-dimensional, Spherically Polarized Magnetic Fields

Abstract Turbulence in the solar wind is characterized by Alfvénic fluctuations that exhibit spherical polarization, a geometric condition resulting in the nearly constant magnitude of the magnetic field. This property persists even during the largest field fluctuations, sometimes leading to local polarity reversals known as switchbacks. A longstanding question is whether three-dimensional (3D) smooth magnetic fields can simultaneously satisfy the constant-∣ B ∣ constraint and how such fields can be constructed analytically or numerically. Here we propose a new numerical method that allows to construct a magnetic field that is exactly spherically polarized, reproducing key features of solar wind fluctuations. Using this framework, we find evidence that discontinuities are unavoidable for generic 3D configurations. Fundamentally, this implies that field rotations cannot maintain exactly constant ∣ B ∣ in an arbitrarily large spatial domain. Rather, field rotations with constant magnitude can exist in limited regions of space. We argue that these finite spatial domains are separated by discontinuities where a local departure from constant ∣ B ∣ is expected. These results provide insights into the structure of solar wind turbulence and more generally into the nature of nonlinear magnetic fluctuations in plasmas.