| Issue |
A&A
Volume 665, September 2022
|
|
|---|---|---|
| Article Number | A51 | |
| Number of page(s) | 6 | |
| Section | The Sun and the Heliosphere | |
| DOI | https://doi.org/10.1051/0004-6361/202243924 | |
| Published online | 08 September 2022 | |
White-light QFP wave train and the associated failed breakout eruption⋆
1
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, PR China
e-mail: ydshen@ynao.ac.cn
2
State Key Laboratory of Space Weather, Chinese Academy of Sciences, Beijing 100190, PR China
3
University of Chinese Academy of Sciences, Beijing 100049, PR China
4
Department of Physics and Electronic Engineering, Sichuan Normal University, Chengdu 610101, PR China
5
Yunnan Key Laboratory of Solar Physics and Space Science, Kunming 650216, PR China
Received:
2
May
2022
Accepted:
16
July
2022
Quasi-periodic fast-propagating (QFP) magnetosonic wave trains are commonly observed in the low corona at extreme ultraviolet wavelength bands. Here, we report the first white-light imaging observation of a QFP wave train propagating outwardly in the outer corona ranging from 2 to 4 R⊙. The wave train was recorded by the Large Angle Spectroscopic Coronagraph on board the Solar and Heliospheric Observatory (SOHO), and was associated with a GOES M1.5 flare in NOAA active region AR12172 at the southwest limb of the solar disk. Measurements show that the speed and period of the wave train were about 218 km s−1 and 26 min, respectively. The extreme ultraviolet imaging observations taken by the Atmospheric Imaging Assembly on board the Solar Dynamic Observatory reveal that in the low corona the QFP wave train was associated with the failed eruption of a breakout magnetic system consisting of three low-lying closed loop systems enclosed by a high-lying large-scale one. Data analysis results show that the failed eruption of the breakout magnetic system was mainly because of the magnetic reconnection that occurred between the two lateral low-lying closed-loop systems. This reconnection enhances the confinement capacity of the magnetic breakout system because the upward-moving reconnected loops continuously feed new magnetic fluxes to the high-lying large-scale loop system. For the generation of the QFP wave train, we propose that it could be excited by the intermittent energy pulses released by the quasi-periodic generation, rapid stretching, and expansion of the upward-moving, strongly bent reconnected loops.
Key words: shock waves / Sun: activity / Sun: flares / Sun: corona / Sun: magnetic fields
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© Y. Shen et al. 2022
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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