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Using high resolution Cluster satellite observations, we show that theturbulent solar wind is populated by magnetic discontinuities at differentscales, going from proton down to electron scales. The structure of theselayers resembles the Harris equilibrium profile in plasmas. Using amulti-dimensional intermittency technique, we show that these structures areconnected through the scales. Supported by numerical simulations of magneticreconnection, we show that observations are consistent with a scenario wheremany current layers develop in turbulence, and where the outflow of thesereconnection events are characterized by complex sub-proton networks ofsecondary islands, in a self-similar way. The present work establishes that thepicture of "reconnection in turbulence" and "turbulent reconnection",separately invoked as ubiquitous, coexist in space plasmas.

The Complex Structure of Magnetic Field Discontinuities in the Turbulent Solar Wind