  $PSP$ and $SolO$ data are utilized to investigate magnetic field
intermittency in the solar wind (SW). Small-scale intermittency $(20-100d_{i})$
is observed to radially strengthen when methods relying on higher-order moments
are considered ($SF_q$, $SDK$), but no clear trend is observed at larger
scales. However, lower-order moment-based methods (e.g., PVI) are deemed more
appropriate for examining the evolution of the bulk of Coherent Structures
(CSs), $PVI \ge 3$. Using PVI, we observe a scale-dependent evolution in the
fraction of the dataset occupied by CSs, $f_{PVI \ge 3}$. Specifically,
regardless of the SW speed, a subtle increase is found in $f_{PVI\ge3}$ for
$\ell =20 d_i$, in contrast to a more pronounced radial increase in CSs
observed at larger scales. Intermittency is investigated in relation to plasma
parameters. Though, slower SW speed intervals exhibit higher $f_{PVI \geq 6}$
and higher kurtosis maxima, no statistical differences are observed for $f_{PVI
\geq 3}$. Highly Alfv\'enic intervals, display lower levels of intermittency.
The anisotropy with respect to the angle between the magnetic field and SW
flow, $\Theta_{VB}$ is investigated. Intermittency is weaker at $\Theta_{VB}
\approx 0^{\circ}$ and is strengthened at larger angles. Considering the
evolution at a constant alignment angle, a weakening of intermittency is
observed with increasing advection time of the SW. Our results indicate that
the strengthening of intermittency in the inner heliosphere is driven by the
increase in comparatively highly intermittent perpendicular intervals sampled
by the probes with increasing distance, an effect related directly to the
evolution of the Parker spiral.
