Homologous Accelerated Electron Beams, Quasi-periodic fast-propagating Wave and CME Observed in one Fan-spine Jet

Abstract

Using imaging and radio multi-wavelength observations, we studied the origin of two homologous accelerated electron beams and a quasi-periodic fast-propagating (QFP) wave train associated with a solar jet on 2012 July 14. The jet occurred in a small-scale fan-spine magnetic system embedding in a large-scale pseudostreamer, which associated with a GOES C1.4 flare, a jet-like coronal mass ejection (CME), a type II radio burst, and a type III radio burst. During the initial stage, a QFP wave train and a fast moving on-disk radio source were detected in succession ahead of the jet along the outer spine of the fan-spine system. When the jet reached a height of about 1.3 solar radii, it underwent a bifurcation into two branches. Based on our analysis results, all the observed phenomena in association with the jet can be explained by using a fanspine magnetic system. We propose that both the type III radio burst and the on-disk fast moving radio source were caused by the same physical process, i.e., the energetic electrons accelerated by the magnetic reconnection at the null point, and they were along the open field lines of the pseudostreamer and the closed outer spine of the fanspine structure, respectively. Due to the bifurcation of the jet body, the lower branch along the closed outer spine of the fan-spine structure fell back to the solar surface, while the upper branch along the open field lines of the pseudostreamer caused the jet-like CME in the outer corona.

Three-dimensional Propagation of the Global EUV Wave associated with a solar eruption on 2021 October 28

“…For instance, the wavefronts could not only exhibit reflections (Li et al 2012;Olmedo et al 2012;Shen et al 2013;Yang et al 2013;Liu et al 2018;Zhou et al 2021b), transmissions (Olmedo et al 2012;Liu et al 2012;Shen et al 2013;Liu et al 2018), and refractions (Thompson et al 2000;Shen & Liu 2012b;Shen et al 2013), but also result in oscillations of coronal loops (Liu et al 2012;Shen & Liu 2012b;Zheng et al 2013b) and filaments (Okamoto et al 2004;Asai et al 2012;Shen et al 2014aShen et al ,b, 2017. EUV waves are often accompanied by quasi-periodic fast-mode propagating wave trains (Liu & Ofman 2014;Shen et al 2021;Duan et al 2022). Signatures of coronal heating have also been found near wave fronts (Wills-Davey & Thompson 1999;Downs et al 2012;Liu et al 2018).…”