Franci, LucaLucaFranciPAPINI, EMANUELEEMANUELEPAPINIMicera, AlfredoAlfredoMiceraLapenta, GiovanniGiovanniLapentaHellinger, PetrPetrHellingerDEL SARTO, DANIELEDANIELEDEL SARTOBurgess, DavidDavidBurgessLandi, SimoneSimoneLandi2025-02-262025-02-2620220004-637Xhttp://hdl.handle.net/20.500.12386/36295We perform a high-resolution, 2D, fully kinetic numerical simulation of a turbulent plasma system with observation-driven conditions, in order to investigate the interplay between turbulence, magnetic reconnection, and particle heating from ion to subelectron scales in the near-Sun solar wind. We find that the power spectra of the turbulent plasma and electromagnetic fluctuations show multiple power-law intervals down to scales smaller than the electron gyroradius. Magnetic reconnection is observed to occur in correspondence of current sheets with a thickness of the order of the electron inertial length, which form and shrink owing to interacting ion-scale vortices. In some cases, both ion and electron outflows are observed (the classic reconnection scenario), while in others—typically for the shortest current sheets—only electron jets are present (“electron-only reconnection”). At the onset of reconnection, the electron temperature starts to increase and a strong parallel temperature anisotropy develops. This suggests that in strong turbulence electron-scale coherent structures may play a significant role for electron heating, as impulsive and localized phenomena such as magnetic reconnection can efficiently transfer energy from the electromagnetic fields to particles.</jats:p>STAMPAenArticle10.3847/1538-4357/ac7da62-s2.0-85137719988https://iopscience.iop.org/article/10.3847/1538-4357/ac7da62022ApJ...936...27FFIS/06 - FISICA PER IL SISTEMA TERRA E IL MEZZO CIRCUMTERRESTRE