Investigating the Role of Inward Alfvén Waves and Structures in the Slow Solar Wind

The solar wind dynamics are thought to be governed by counter-propagating Alfv & eacute;n waves. Alfv & eacute;n waves generate a turbulent cascade through nonlinear couplings between shearing wave packets. However, imbalances, structures, and intermittency complicate the solar wind's magnetohydrodynamic (MHD) turbulence. Simulations and theories have suggested that dynamic alignment, or the tendency for velocity and magnetic fluctuations to become more correlated as a function of scale, may dictate the turbulent cascade. Observations have hinted at dynamic alignment at large scales but remain inconclusive at small scales. To investigate the nature of dynamically aligning fluctuations in the solar wind, we examine slow wind intervals from the Helios 2 spacecraft. We develop a two-component model of solar wind turbulence consisting of Alfv & eacute;nic and non-Alfv & eacute;nic contributions. We assume that only counter-propagating Alfv & eacute;n waves experience dynamic alignment, and the non-Alfv & eacute;nic structures do not participate in the alignment process. Our model allows us to constrain the relative contribution of inward Alfv & eacute;n waves and non-Alfv & eacute;nic structures with respect to the amplitude of outward Alfv & eacute;n waves in the slow solar wind as a function of scale under the assumption of dynamic alignment. We show that the power ratio of inward to outward Alfv & eacute;n fluctuations decreases as a function of scale. At the same time, the non-Alfv & eacute;nic structures to outward Alfv & eacute;n fluctuations increase with decreasing scale. Increasing structures provide a possible explanation for no dynamic alignment at small scales. Our study implies the need for new theoretical models to fully account for the solar wind's compressibility, intermittency, and imbalanced nature.