Speaker
Description
First Name: Jiayi
Last Name: Liu
Affiliation: Nanjing University
All Authors: Xin Chen, Yulei Wang, Fanpeng Shi, Cheng Xin
Abstract: Magnetic reconnection is a key mechanism that triggers the solar eruptions and heats the low corona. While the dynamic features of magnetic reconnection are extensively studied with MHD simulations, they are not well quantified by observations. Using ultra-high-resolution observations from EUI on board Solar Orbiter at a scale of about 300 km, we quantitatively study the dynamic process of a coronal jet triggered by 3D magnetic reconnection. We first analyze the formation of the current sheet and the persistent production of plasmoids during the gentle phase of reconnection. We then analyze the fine-scale features of the curtain-like structures in the jet with a speed of about 260 km/s after the eruption of a mini-filament. We finally compare these results with a 3D MHD simulation.