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The physical connection between thermal convection in the solar interior andthe solar wind remains unclear due to their significant scale separation. Usingan extended version of the three-dimensional radiative magnetohydrodynamic codeRAMENS, we perform the first comprehensive simulation of the solar windformation, starting from the wave excitation and the small-scale dynamo belowthe photosphere. The simulation satisfies various observational constraints asa slow solar wind emanating from the coronal hole boundary. The magnetic energyis persistently released in the simulated corona, showing a hot upward flow atthe interface between open and closed fields. To evaluate the energeticcontributions from Alfv\'en wave and interchange reconnection, we develop a newmethod to quantify the cross-field energy transport in the simulatedatmosphere. The measured energy transport from closed coronal loops to openfield accounts for approximately half of the total. These findings suggest asignificant role of the supergranular-scale interchange reconnection in solarwind formation.

the astrophysical journal. letters

A Comprehensive Simulation of Solar Wind Formation from the Solar  Interior: Significant Cross-field Energy Transport by Interchange  Reconnection near the Sun