  This study explores the impact of a turbulent scattering mechanism, akin to
those influencing solar and galactic cosmic rays propagating in the
interplanetary medium, on the population of suprathermal electrons in the solar
wind. We employ a Fokker-Planck equation to model the radial evolution of
electron pitch angle distributions under the action of magnetic focusing, which
moves the electrons away from isotropy, and of a diffusion process that tends
to bring them back to it.
  We compare the steady-state solutions of this Fokker-Planck equation with
data obtained from the Solar Orbiter and Parker Solar Probe missions and find a
remarkable agreement, varying the turbulent mean free path as the sole free
parameter in our model. The obtained mean free paths are of the order of the
astronomical unit, and display weak dependence on electron energy within the
$100$ eV to $1$ keV range. This value is notably lower than Coulomb collision
estimates but aligns well with observed mean free paths of low-rigidity solar
energetic particles events.
  The strong agreement between our model and observations leads us to conclude
that the hypothesis of turbulent scattering at work on electrons at all
heliospheric distances is justified. We discuss several implications, notably
the existence of a low Knudsen number region at large distances from the Sun,
which offers a natural explanation for the presence of an isotropic ``halo''
component at all distances from the Sun -- electrons being isotropized in this
distant region before travelling back into the inner part of the interplanetary
medium.
