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We perform a high-resolution two-dimensional fully-kinetic numericalsimulation of a turbulent plasma system with observation-driven conditions, inorder to investigate the interplay between turbulence, magnetic reconnection,and particle heating from ion to sub-electron scales in the near-Sun solarwind. We find that the power spectra of the turbulent plasma andelectromagnetic fluctuations show multiple power-law intervals down to scalessmaller than the electron gyroradius. Magnetic reconnection is observed tooccur in correspondence of current sheets with a thickness of the order of theelectron inertial length, which form and shrink due to interacting ion-scalevortexes. In some cases, both ion and electron outflows are observed (theclassic reconnection scenario), while in others -- typically for the shortestcurrent sheets -- only electron jets are presents ("electron-onlyreconnection"). At the onset of reconnection, the electron temperature startsto increase and a strong parallel temperature anisotropy develops. Thissuggests that in strong turbulence electron-scale coherent structures may playa significant role for electron heating, as impulsive and localized phenomenasuch as magnetic reconnection may transfer energy from the electromagneticfields to particles more efficiently than damping mechanisms related tointeractions with wave-like fluctuations.

Anisotropic electron heating in turbulence-driven magnetic reconnection in the near-Sun solar wind