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The interpretation of single-point spacecraft measurements of solar windturbulence is complicated by the fact that the measurements are made in a frameof reference in relative motion with respect to the turbulent plasma. TheTaylor hypothesis---that temporal fluctuations measured by a stationary probein a rapidly flowing fluid are dominated by the advection of spatial structuresin the fluid rest frame---is often assumed to simplify the analysis. Butmeasurements of turbulence in upcoming missions, such as Solar Probe Plus,threaten to violate the Taylor hypothesis, either due to slow flow of theplasma with respect to the spacecraft or to the dispersive nature of the plasmafluctuations at small scales. Assuming that the frequency of the turbulentfluctuations is characterized by the frequency of the linear waves supported bythe plasma, we evaluate the validity of the Taylor hypothesis for the linearkinetic wave modes in the weakly collisional solar wind. The analysis predictsthat a dissipation range of solar wind turbulence supported by whistler wavesis likely to violate the Taylor hypothesis, while one supported by kineticAlfven waves is not.

Validity of the Taylor Hypothesis for Linear Kinetic Waves in the Weakly Collisional Solar Wind