Nature of Transonic Sub-Alfvénic Turbulence and Density Fluctuations in the Near-Sun Solar Wind: Insights from Magnetohydrodynamic Simulations and Nearly-Incompressible Models

Abstract

Recent Parker Solar Probe measurements have revealed that solar wind (SW) turbulence transits from a subsonic to a transonic regime near the Sun, while remaining sub-Alfvénic. These observations call for a revision of existing SW models, where turbulence is considered to be both subsonic and sub-Alfvénic. In this Letter, we introduce a new magnetohydrodynamic (MHD) model of Transonic sub-Alfvénic Turbulence (TsAT). Our model shows that turbulence is effectively nearly-incompressible (NI) and has a 2D + slab geometry not only in the subsonic limit, but also in the transonic regime, as long as it remains sub-Alfvénic, a condition essentially enforced everywhere in the heliosphere by the strong local magnetic field. These predictions are consistent with 3D MHD simulations, showing that transonic turbulence is dominated by low frequency quasi-2D incompressible structures, while compressible fluctuations are a minor component corresponding to low frequency slow modes and high frequency fast modes. Our new TsAT model extends existing NI theories of turbulence, and is potentially relevant for the theoretical and numerical modeling of space and astrophysical plasmas, including the near-Sun SW, the solar corona, and the interstellar medium.

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