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(Abridged) Wavelet analysis can be used to measure the power spectrum ofsolar wind fluctuations along a line in any direction with respect to the localmean magnetic field. This technique is applied to study solar wind turbulencein high-speed streams in the ecliptic plane near solar minimum using magneticfield measurements with a cadence of eight vectors per second. The analysis ofnine high-speed streams shows that the reduced spectrum of magnetic fieldfluctuations (trace power) is approximately azimuthally symmetric about B_0 inboth the inertial range and dissipation range; in the inertial range thespectra are characterized by a power-law exponent that changes continuouslyfrom 1.6 \pm 0.1 in the direction perpendicular to the mean field to 2.0 \pm0.1 in the direction parallel to the mean field. The large uncertaintiessuggest that the perpendicular power-law indices 3/2 and 5/3 are bothconsistent with the data. The results are similar to those found by Horbury etal. (2008) at high heliographic latitudes.

Dependence of solar wind power spectra on the direction of the local mean magnetic field