Solar Wind Magnetic Fluctuations Diagnosing Local Reconnection Currents

The 20 years of ACE satellite measurements of B(t) at 1AU enable detailed spectral and dynamical analyses, here supplemented by radial dependencies from Ulysses and Mariner from 0.3 - 5 AU. 1) Variable-duration spectral analyses clearly show that there is no persistent magnetic "spiral" at 1AU, merely the statistical fluctuations of "random walk" dynamics. Similarly, spectral components B(f) above f$\cong $50$\mu $Hz clearly show the $\surd $N scaling of random noise. 2) Pervasive dynamical "arc" events are observed on time-scales 10\textasciicircum 3\textless $\tau $ \textless 10\textasciicircum 5 sec, presumably related to spiky "switchbacks" observed by PSP at 0.1AU. The dynamics appears as B$\theta $-Bz, Br-Bz, and Br-B$\theta $ temporal arcs, with occurrence rates differing by direction. The observed dynamics is closely modelled by finite-duration "pinched" $+$/- current filaments, representing charge non-neutrality of 10\textasciicircum -5 of the e-/p$+$ flux over distances d$\cong $10\textasciicircum 3Mm and times $\tau \cong $2000s. 3) The Br and B$\theta $ (but not Bz) spectral components at the solar rotation frequency f$_{\mathrm{rot}}$ are quite exceptional, varying between 0{\%} and 30{\%} (average 17{\%}) of the total Brms\textasciicircum 2 magnetic energy. In \textit{only} these variable components (with differing radial dependencies) is there a Br-B$\theta $ anti-correlation, which is traditionally mis-interpreted as a persistent spiral. These f$_{\mathrm{rot}}$ components probably reflect z-currents, arising from $\theta $-z-dependent electric potentials from exceedingly small differences in e-/p$+$ ejection from the rotating solar surface.