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Single point spacecraft observations of the turbulent solar wind flow exhibita characteristic nonaxisymmetric anisotropy that depends sensitively on theperpendicular power spectral exponent. For the first time we use thisnonaxisymmetric anisotropy as a function of wave vector direction to testmodels of magnetohydrodynamic (MHD) turbulence. Using Ulysses magnetic fieldobservations in the fast, quiet polar solar wind we find that theGoldreich-Sridhar model of MHD turbulence is not consistent with the observedanisotropy, whereas the observations are well reproduced by the "Slab + 2D"model. The Golderich-Sridhar model alone can not account for the observationsunless an additional component is also present.

Nonaxisymmetric Anisotropy of Solar Wind Turbulence as a Direct Test for the Models of Magnetohydrodynamic Tubulence