In this study we analyze the evolution of solar wind turbulence from 0.3 to 1 AU using a database of 387 intervals from the Helios 1 spacecraft. Our results uphold the conclusion made by Smith et al. (2006), who used data from 1 AU, that the magnetic variance anisotropy scales with both proton beta and the amplitude of fluctuations in the power spectrum all the way down to 0.3 AU. We confirm the result of Bieber et al. (1996) that ∼80% of the energy is contained in the wave vectors perpendicular to the mean magnetic field and in light of Dasso et al. (2005) we compute the fraction of energy in field‐aligned wave vectors for high‐ and low‐speed intervals separately. As Hamilton et al. found at 1 AU, we also see no clear reliance of the energy contained in parallel and perpendicular wave vectors based on wind speed at any heliocentric distance between 0.3 and 1 AU in the range of frequencies we study (5 to 20 mHz). These results combine to tell the story that the turbulent properties of the solar wind we analyze are fully consistent with the 1 AU observations and no discernable evolution can be found.
