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The turbulent magnetic fields of a large set of fast solar wind streamsmeasured onboard ACE and STEREO A and B are analyzed in an effort to identifythe effects of the turbulence-level broad variations on the orientations of thelocal, time-averaged magnetic fields. The power level of turbulence, roughlydefined as the power in the transverse field fluctuations normalized to themedium-scale average background field, tightly orders the location of the peaksin the probability distribution functions (PDFs) of the angles between localfields and Parker spiral. As a result, the broad variations in the power levelof turbulence cause a steep dependence of the average power level of turbulenceon the angle of the local field to the Parker spiral, with the highestturbulence levels found near the normal to the Parker spiral and the lowestlevels near the Parker spiral direction. Generalized quasilinear estimates ofthe mean cross-field displacements adapted to intermittent time-varyingturbulence lead to accurate fits of the observed angle PDFs at all stablelevels of turbulence, supporting the idea that isotropic turbulence couldaccount for the observed angle PDFs. Modeling of the angles alpha_r betweenlocal fields and radial direction, from the PDFs of the angles alpha betweenlocal and background fields under an assumption of axisymmetry of the turbulentfields around a background field in or near the direction of the Parker spiral,also produces fairly good fits of the observed PDFs of alpha_r, therebyvalidating the assumption. Finally, local field reversals are found to be quitecommon even within very broad streams of "unipolar" fast solar wind.

Turbulence-Level Variations and Magnetic Field Orientations in the Fast Solar Wind