Authors: Chen Shi (Department of Physics, Auburn University)

The solar wind is highly turbulent, containing fluctuations that span a wide range of spatial and temporal scales. However, how turbulent energy is transferred across scales and ultimately dissipated remains an open question. In recent years, Parker Solar Probe has provided valuable observations of the solar wind at unprecedentedly close heliocentric distances, offering new insights into the dynamic processes in the young solar wind. In this presentation, I will review our current understanding of solar wind turbulence in the inner heliosphere and summarize recent progress in observations, numerical simulations, and theory. In particular, I will focus on the roles of intermittency, magnetic reconnection, and kinetic-scale waves in turbulent energy transfer.