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In its first encounter at solar distances as close as r = 0.16AU, ParkerSolar Probe (PSP) observed numerous local reversals, or inversions, in theheliospheric magnetic field (HMF), which were accompanied by large spikes insolar wind speed. Both solar and in situ mechanisms have been suggested toexplain the existence of HMF inversions in general. Previous work using Helios1, covering 0.3-1AU, observed inverted HMF to become more common withincreasing r, suggesting that some heliospheric driving process creates oramplifies inversions. This study expands upon these findings, by analysinginversion-associated changes in plasma properties for the same large data set,facilitated by observations of 'strahl' electrons to identify the unperturbedmagnetic polarity. We find that many inversions exhibit anti-correlated fieldand velocity perturbations, and are thus characteristically Alfv\'enic, butmany also depart strongly from this relationship over an apparent continuum ofproperties. Inversions depart further from the 'ideal' Alfv\'enic case withincreasing r, as more energy is partitioned in the field, rather than theplasma, component of the perturbation. This departure is greatest forinversions with larger density and magnetic field strength changes, andcharacteristic slow solar wind properties. We find no evidence that inversionswhich stray further from 'ideal' Alfv\'enicity have different generationprocesses from those which are more Alfv\'enic. Instead, different inversionproperties could be imprinted based on transport or formation within differentsolar wind streams.

Evolving Solar Wind Flow Properties of Magnetic Inversions Observed by Helios