Speaker
Description
First Name: Weihang
Last Name: Zhang
Affiliation: Peking University
All Authors: Weihang Zhang, Hui Tian, Feng Chen, Yuhang Gao, Yajie Chen
Abstract: A prevailing hypothesis suggests that the fast solar wind is primarily driven by the mechanism of interchange reconnection. This process involves reconnection between low-lying closed magnetic loops and adjacent open magnetic field lines, converting magnetic energy into kinetic and thermal energy, which drives jets and excites Alfvén waves. As these waves propagate along open field lines, they may undergo turbulent dissipation and mode conversion, further heating and accelerating the plasma, thereby supplying the mass and energy required for the formation of the solar wind. In this process, magnetic reconnection and wave turbulence are the two primary mechanisms for mass and energy supply. However, their relative contributions remain poorly quantified. In this work, based on three-dimensional radiative magnetohydrodynamic (MHD) simulations using the MURaM code, where convective motions at the base continuously drive magnetic evolution, we self-consistently generate interchange reconnection and jets between low-lying closed loops and open field lines. We plan to investigate the evolution of velocity and amplitude, as well as possible wave mode changes, during the propagation of jets through the chromosphere, transition region, and corona. We aim to quantify the energy released by magnetic reconnection and dissipated by wave turbulence, and to evaluate their relative contributions to the nascent fast solar wind. Finally, we will synthesize multi-wavelength, multi-perspective imaging to assess the identifiability of jet, reconnection, and wave signals from a polar viewpoint. The results will establish a methodological foundation for the data analysis of future polar front-side imaging missions.