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Turbulence, a ubiquitous phenomenon in interplanetary space, is crucial forthe energy conversion of space plasma at multiple scales. This work focuses onthe propagation, polarization and wave composition properties of the solar windturbulence within 0.3AU, and its variation with heliocentric distances at MHDscales (from 10s to 1000s in the spacecraft frame). We present the probabilitydensity function of propagation wavevectors (${\rm{PDF}}(k_\parallel,k_\perp)$)for solar wind turbulence winthin 0.3 AU for the first time: (1) wavevectorscluster quasi-(anti-)parallel to the local background magnetic field for$kd_{\rm i}<0.02$, where $d_{\rm i}$ is the ion inertial length; (2)wavevectors shift to quasi-perpendicular directions for $kd_{\rm i}>0.02$.Based on our wave composition diagnosis, we find that: the outward/anti-sunwardAlfv\'en mode dominates over the whole range of scales and distances, thespectral energy density fraction of the inward/sunward fast mode decreases withdistance, and the fractional energy densities of the inward and outward slowmode increase with distance. The outward fast mode and inward Alfv\'en moderepresent minority populations throughout the explored range of distances andscales. On average, the degree of anisotropy of the magnetic fluctuationsdefined with respect to the minimum variation direction decreases withincreasing scale, with no trend in distance at all scales. Our results providecomprehensive insight into the scenario of transport and transfer of the solarwind fluctuations/turbulence in the inner heliosphere.

Wave Composition, Propagation, and Polarization of MHD Turbulence within 0.3AU as Observed by PSP