  Parker Solar Probe and Solar Orbiter data are used to investigate the radial
evolution of magnetic turbulence between $0.06 ~ \lesssim R ~\lesssim 1$ au.
The spectrum is studied as a function of scale, normalized to the ion inertial
scale $d_{i}$. In the vicinity of the Sun, the inertial range is limited to a
narrow range of scales and exhibits a power-law exponent of, $\alpha_{B} =
-3/2$, independent of plasma parameters. The inertial range grows with
distance, progressively extending to larger spatial scales, while steepening
towards a $\alpha_{B} =-5/3$ scaling. It is observed that spectra for intervals
with large magnetic energy excesses and low Alfv\'enic content steepen
significantly with distance, in contrast to highly Alfv\'enic intervals that
retain their near-Sun scaling. The occurrence of steeper spectra in slower wind
streams may be attributed to the observed positive correlation between solar
wind speed and Alfv\'enicity.
