  In its first encounter at solar distances as close as r = 0.16AU, Parker
Solar Probe (PSP) observed numerous local reversals, or inversions, in the
heliospheric magnetic field (HMF), which were accompanied by large spikes in
solar wind speed. Both solar and in situ mechanisms have been suggested to
explain the existence of HMF inversions in general. Previous work using Helios
1, covering 0.3-1AU, observed inverted HMF to become more common with
increasing r, suggesting that some heliospheric driving process creates or
amplifies inversions. This study expands upon these findings, by analysing
inversion-associated changes in plasma properties for the same large data set,
facilitated by observations of 'strahl' electrons to identify the unperturbed
magnetic polarity. We find that many inversions exhibit anti-correlated field
and velocity perturbations, and are thus characteristically Alfv\'enic, but
many also depart strongly from this relationship over an apparent continuum of
properties. Inversions depart further from the 'ideal' Alfv\'enic case with
increasing r, as more energy is partitioned in the field, rather than the
plasma, component of the perturbation. This departure is greatest for
inversions with larger density and magnetic field strength changes, and
characteristic slow solar wind properties. We find no evidence that inversions
which stray further from 'ideal' Alfv\'enicity have different generation
processes from those which are more Alfv\'enic. Instead, different inversion
properties could be imprinted based on transport or formation within different
solar wind streams.
