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In order to resolve and characterize anisotropy in turbulent plasma flows aproper estimation of the background magnetic field is crucially important.Various approaches to calculate the background magnetic fields, ranging fromlocal fields to globally averaged fields, are commonly used in the analysis ofturbulent data. Here we investigate how the uncertainty in the orientation of ascale dependent background magnetic field influences the ability to resolveanisotropy. Therefore we introduce a quantitative measure, the angleuncertainty, which characterizes the uncertainty of the orientation of thebackground magnetic field which turbulent structures are exposed to. The angleuncertainty can be used as a condition to estimate the ability to resolveanisotropy with certain accuracy. We apply our description to resolve spectralanisotropy in fast solar wind data. We show that if the angle uncertainty growstoo large, the power of the turbulent fluctuations is attributed to false localmagnetic field angles, which may lead to an incorrect estimation of spectralindices. In our results an apparent robustness of the spectral anisotropy tofalse local magnetic field angles is observed, which can be explained by astronger increase of power for lower frequencies when the scale of the localmagnetic field is increased. The frequency dependent angle uncertainty is ameasure which can be applied to any turbulent system.

The uncertainty of local background magnetic field orientation in anisotropic plasma turbulence