Heliospheric Magnetic Fields Generated by Solar Wind Current Fluctuations.

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. We find:

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≅50μHz clearly show the √N scaling of random noise.

2) Pervasive dynamical "arc" events are observed on time-scales 10^3< τ < 10^5 sec, presumably related to spiky "switchbacks" observed by PSP at 0.1AU. The dynamics appears as Bθ-Bz, Br-Bz, and Br-Bθ temporal arcs, with occurrence rates differing by direction. The observed dynamics is modeled by finite-duration "pinched" +/- current filaments, representing charge non-neutrality of 10^-5 in the e-/p+ flux over distances d≅10^3Mm and times τ≅2000s.

3) The Br and Bθ (but not Bz) spectral components at the solar rotation frequency frot are exceptional, varying between 0% and 30% (average 17%) of the total Brms^2 magnetic energy. In only these variable components (arising from variable surface emission) is there a Br-Bθ anti-correlation, which is traditionally mis-interpreted as the magnetic spiral. NNP.ucsd.edu/Solar/