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Electron scale solar wind turbulence has attracted great interest in recentyears. Clear evidences have been given from the Cluster data that turbulence isnot fully dissipated near the proton scale but continues cascading down to theelectron scales. However, the scaling of the energy spectra as well as thenature of the plasma modes involved at those small scales are still not fullydetermined. Here we survey 10 years of the Cluster search-coil magnetometer(SCM) waveforms measured in the solar wind and perform a statistical study ofthe magnetic energy spectra in the frequency range [$1, 180$]Hz. We show that alarge fraction of the spectra exhibit clear breakpoints near the electongyroscale $\rho_e$, followed by steeper power-law like spectra. We show thatthe scaling below the electron breakpoint cannot be determined unambiguouslydue to instrumental limitations that will be discussed in detail. We compareour results to recent ones reported in other studies and discuss theirimplication on the physical mechanisms and the theoretical modeling of energydissipation in the SW.

Scaling of the electron dissipation range of solar wind turbulence