First Time Observed M-Shaped Coronal Mass Ejection Associated with a Blowout Jet and an Extreme Ultraviolet Wave

TL;DR

This study reports the first observational evidence of an M-shaped CME formed by a single coronal blowout jet that also launches an EUV wave. Using high-resolution, multi-angle data from SDO/AIA, STEREO/EUVI, and COR1, the authors show that the EUV wave splits into two components that drive two bubble-like CMEs, while a jet-like CME arises directly from the blowout jet. They propose the jet-wave-multi-CME framework to explain the coupled evolution of the jet, EUV wave, and multiple CMEs, supported by NLFFF and PFSS magnetic-field reconstructions. The results illuminate the energy transfer and magnetic topology governing complex solar eruptive phenomena and offer new constraints for MHD modeling and space weather forecasting.

Abstract

The coronal blowout jet, extreme ultraviolet (EUV) wave and coronal mass ejection (CME) are common phenomena in the solar atmosphere. In this paper, we report the occurrence of an M-shaped CME event associated with a blowout jet and an EUV wave using high-resolution, multi-angle and multi-wavelength observations taken from Solar Dynamics Observatory, and Solar TErrestrial RElations Observatory. Interestingly, and for the first time, it is found that two bubble-like CMEs and a jet-like CME were simultaneously triggered by the same eruptive event. Our observational analyses and findings indicate the following: (1) the eruption of a blowout jet led to a large-scale EUV wave; (2) the eruption of the EUV wave swept a small filament (prominence) and a long filament; (3) eventually the EUV wave split-up into two parts, leading to the two bubble-like CMEs, while the blowout jet induced a jet-like CME. The combined events appear to form an M-shape like structure CME, that we sketch throughout a proposed cartoon tentatively explaining the observed complex configuration. Based on observational diagnosis, we argue that the jet, the EUV wave and the multi-CME are highly interlinked. A suggested eruption-model, from the solar atmosphere to the space, is outlined and discussed, providing a possibly new way to probe the relationship between the solar eruptions and the surrounding space. The investigation of such rare phenomenon can be a key point for better understanding of the physical associated triggering mechanisms and energy transport in the solar atmosphere, crucial for MHD simulations and modeling.

Figures (6)

• Figure 1: The white curved lines indicate the EUV wave propagation path and profile at the AIA 171, 193 and 304 Å channels. The blowout jet is also shown in panels (a2), (a3), (b2) and (b3). The white boxes indicate the small filament (prominence) evolution in panels (d1)-(d3). The bottom three panels refer to the observations from the FOV of STA at 304 Å. The white boxes mark the small prominence (filament) designated with the "P" symbols. The white contour line represents the profile of the small prominence. "LF" represents the long filament structure that indicated by the white arrow. The zoomed views highlight the prominence evolution. An accompanying movie (animation1.mpeg) is available in the online journal.
• Figure 2: The top and bottom panels report the observations from SDO/AIA 171 and 193 Å running-difference images, respectively. The white-dotted curved lines indicate the wavefront of the EUV wave. The reflect wave is also displayed in panel (a2). An accompanying movie (animation2.mpeg) is available in the online journal.
• Figure 3: A set of original 304 Å and running difference COR1 combined images illustrating the M-shaped CME evolution from the two viewpoints of STA and STB. The blowout jet is also indicated with white arrows in the panels (a1), (b1). Panels (a3), (b3) display the structures of the three CMEs. The red arrows indicate the jet-like CME, while the two white arch lines represent the two bubble-like CMEs. An animated version (animation3.mpeg) of this figure is available in the online journal.
• Figure 4: A set of running difference 195 Å and COR1 combined images showing the EUVI bubble and the first bubble-like CME (bubble-like CME 1) evolution from the two viewpoints of STA and STB (see animation4.mpeg).
• Figure 5: STEREO/COR1 running-different images at 07:10 UT from two views in panels (a) and (b). Slices A1-A3 and slices B1-B3 are used to obtain the time-distance diagrams shown in panels (a1)-((a3) and (b1)-(b3), respectively.