Formation of Fast shocks by magnetic reconnection in the Solar corona

• Main Authors: MING-HSU HSIEH, 謝鳴旭
• Other Authors: Lou-Chuang Lee
• Format: Others
• Language: zh-TW
• Published: 2005
• Online Access: http://ndltd.ncl.edu.tw/handle/73481270034817684794

碩士 === 國立成功大學 === 物理學系碩博士班 === 93 === The fast shocks generated by magnetic reconnection can explain recent SOHO observations of the heating and acceleration of protons and heavier ions in the solar corona (Lee and Wu, 2000). The magnetic reconnection over the solar surface is expected to generate abundant shocks. However, the generation of fast shocks by magnetic reconnection process is relatively not well studied. In this study, we plan to demonstrate the generation of fast shocks by magnetic reconnection in various magnetic configurations on the solar surface. We will study the fast shock generations on x-z plane based on 2D resistive MHD simulations, and examine the plasma betam, phi, etal, and tstop effects on the generation. As time increasing we can find the plasma jets in the center of reconnection region spread out along positive and negative z direction. There is a pair of weak fast shocks propagated in x-z plane which are denoted by the increasing densities, pressure, temperatures, and magnetic fields. We also plan to study the generation and evolution of the magnetic bulge in process of transient magnetic reconnection.