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We investigate spectral properties of turbulence in the solar wind that is aweakly collisional astrophysical plasma, accessible to in-situ observations.Using the Helios search coil magnetometer measurements in the fast solar wind,in the inner heliosphere, we focus on properties of the turbulent magneticfluctuations at scales smaller than the ion characteristic scales, theso-called kinetic plasma turbulence. At such small scales, we show that themagnetic power spectra between 0.3 and 0.9 AU from the Sun have a generic shape$\sim f^{-8/3}\exp{(-f/f_d)}$ where the dissipation frequency $f_d$ iscorrelated with the Doppler shifted frequency $f_{\rho e}$ of the electronLarmor radius. This behavior is statistically significant: all the observedkinetic spectra are well described by this model, with $f_d = f_{\rho e}/1.8$.Our results indicate that the electron gyroradius plays the role of thedissipation scale and marks the end of the electromagnetic cascade in the solarwind.

Spectrum of kinetic plasma turbulence at 0.3-0.9 astronomical units from the Sun