  Parker spiral theory predicts the heliospheric magnetic field (HMF) will have
components of opposite polarity radially toward the Sun and tangentially
antiparallel to the solar rotation (i.e. in GSE coordinates, with Bx/By<0).
This theory explains the average orientation of the HMF very well but does not
predict orthogardenhose (OGH) flux with BX/BY>0 that is often observed. We here
study the occurrence and structure of OGH flux, as seen in near-Earth space
(r=1AU) and by the Helios spacecraft at 0.29<r<1AU, in order to evaluate the
contributions to OGH flux generation of the various mechanisms and factors that
are not accounted for in Parker spiral theory. We study the loss of OGH flux
with increasing averaging timescale between 16 seconds and 100 hours and so
determine its spectrum of scale sizes. OGH flux at sunspot minimum is shown to
be more common than at sunspot maximum and caused by smaller-scale structure in
the HMF, with a mode temporal scale at a fixed point of 10hrs compared to
40hrs. OGH generated by rotating the HMF through the radial direction is also
shown to differ in its spectrum of scale sizes from that generated by rotating
the HMF through the tangential direction: the former does not contribute to the
excess open heliospheric flux at a given r but the latter does. We show that
roughly half of the HMF deflection from the ideal Parker spiral giving OGH at
Earth occurs at r below 0.3AU. We highlight some questions which can be
addressed by the Parker Solar Probe mission which will study the HMF down to
r=0.046AU.
