Components and Anisotropy of 3D QFP Waves During the Early Solar Eruption  

作　　者：Jialiang Hu Jing Ye Yuhao Chen Zhixing Mei Shanshan Xu Jun Lin 

机构地区：[1]Yunnan Observatories,Chinese Academy of Sciences,Kunming 650216,China [2]University of Chinese Academy of Sciences,Beijing 100049,China [3]Yunnan Key Laboratory of Solar Physics and Space Science,Kunming 650216,China [4]Yunnan Province China–Malaysia HF-VHF Advanced Radio Astronomy Technology International Joint Laboratory,Kunming 650216,China

出　　处：《Research in Astronomy and Astrophysics》2024年第12期105-115,共11页天文和天体物理学研究(英文版)

基　　金：supported by Strategic Priority Research Program of the Chinese Academy of Sciences No. XDB0560000;National Key R&D Program of China No. 2022YFF0503804;NSFC grants 11933009, 12273107, U2031141 and 12073073;grants associated with the Yunling Scholar Project of Yunnan Province;the Yunnan Province Scientist Workshop of Solar Physics;the Yunnan Key Laboratory of Solar Physics and Space Exploration of Code 202205AG070009;the Special Project for the construction of science and technology innovation centers faced to South Asiaand Southeast Asia-Yunnan International Joint Innovation Platform: “China-Malaysia HF-VHF Advanced Radio Astronomy Technology International Joint Laboratory of Yunnan” (202303AP140003);the support by grants associated with the Yunnan Revitalization Talent Support Program;the Foundation of the Chinese Academy of Sciences (Light of West China Program)。

摘　　要：The propagation of disturbances in the solar atmosphere is inherently three-dimensional(3D), yet comprehensive studies on the spatial structure and dynamics of 3D wave fronts are scarce. Here we conduct high-resolution 3D numerical simulations to investigate filament eruptions, focusing particularly on the 3D structure and genesis of extreme ultraviolet(EUV) waves. Our results demonstrate that the EUV wave front forms a dome-like configuration subdivided into three distinct zones. The foremost zone, preceding the flux rope, consists of fastmode shock waves that heat the adjacent plasma. Adjacent to either side of the flux rope, the second zone contains expansion waves that cool the nearby plasma. The third zone, at the juncture of the first two, exhibits minimal disturbances. This anisotropic structure of the wave front stems from the configuration and dynamics of the flux rope, which acts as a 3D piston during eruptions—compressing the plasma ahead to generate fast-mode shocks and evacuating the plasma behind to induce expansion waves. This dynamic results in the observed anisotropic wave front. Additionally, with synthetic EUV images from simulation data, the EUV waves are observable in Atmospheric Imaging Assembly 193 and 211 ?, which are identified as the fast-mode shocks. The detection of EUV waves varies with the observational perspective: the face-on view reveals EUV waves from the lower to the higher corona, whereas an edge-on view uncovers these waves only in the higher corona.

关 键 词：SUN corona-Sun coronal mass ejections(CMEs)-shock waves 

分 类 号：P182.62[天文地球—天文学]