Tiny Quiet-Sun EUV Ejections Revealed by High-resolution Multiwavelength Observations
Abstract
We investigate two successive tiny quiet-Sun EUV ejections on 2022 October 29 using coordinated Solar Orbiter/EUI, IRIS, SDO/AIA, and Goode Solar Telescope observations. We examine their low-lying geometry and the chromospheric and transition-region response before and between the releases. A curved H-alpha thread is present beforehand, and Mg ii and Si iv spectra reveal a compact multithermal precursor 2.6--2.7 min before the first EUV brightening. EUI--AIA stereoscopy places the recurrent compact EUV kernel near 2.2 Mm and the sampled emission at approximately 0.6--4.2 Mm along inclined, locally arched structures. The first ejection shows multithreaded, helical-looking EUV strands; the second shows straighter strands and a decrease in the cross-ridge separation of redshifted and blueshifted Mg ii k3 samples from 1.47'' to 0.89''. Nevertheless, the two peaks have comparable emission-measure increments and estimated event-associated thermal contents of a few 10^26 erg under the same assumptions. Before the second ejection, the regional Si iv and k3 blueshift signals remain enhanced, while the Mg ii central reversal along the activated ridge remains shallower than before the event. Component reconnection between the curved structure and the surrounding field offers a possible explanation. The observations show that jet-like EUV emission can occur in low-lying structures. The second ejection begins before the chromospheric and transition-region spectra have returned to their pre-event states. Its spectral signatures may therefore depend on the atmospheric changes associated with the first ejection as well as on the additional energy input.
Related
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BibTeX
@misc{huang2026tiny,
title = {{Tiny Quiet-Sun EUV Ejections Revealed by High-resolution Multiwavelength Observations}},
author = {Nengyi Huang and Yuqian Wei and Qin Li and Jeongwoo Lee and Haimin Wang},
howpublished = {arXiv},
year = {2026},
month = nov,
doi = {10.48550/arxiv.2611.05934},
eprint = {2611.05934},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2611.05934},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Tiny Quiet-Sun EUV Ejections Revealed by High-resolution Multiwavelength Observations
AU - Nengyi Huang
AU - Yuqian Wei
AU - Qin Li
AU - Jeongwoo Lee
AU - Haimin Wang
PY - 2026
DA - 2026/11/04
PB - arXiv
DO - 10.48550/arxiv.2611.05934
UR - https://arxiv.org/abs/2611.05934
AB - We investigate two successive tiny quiet-Sun EUV ejections on 2022 October 29 using coordinated Solar Orbiter/EUI, IRIS, SDO/AIA, and Goode Solar Telescope observations. We examine their low-lying geometry and the chromospheric and transition-region response before and between the releases. A curved H-alpha thread is present beforehand, and Mg ii and Si iv spectra reveal a compact multithermal precursor 2.6--2.7 min before the first EUV brightening. EUI--AIA stereoscopy places the recurrent compact EUV kernel near 2.2 Mm and the sampled emission at approximately 0.6--4.2 Mm along inclined, locally arched structures. The first ejection shows multithreaded, helical-looking EUV strands; the second shows straighter strands and a decrease in the cross-ridge separation of redshifted and blueshifted Mg ii k3 samples from 1.47'' to 0.89''. Nevertheless, the two peaks have comparable emission-measure increments and estimated event-associated thermal contents of a few 10^26 erg under the same assumptions. Before the second ejection, the regional Si iv and k3 blueshift signals remain enhanced, while the Mg ii central reversal along the activated ridge remains shallower than before the event. Component reconnection between the curved structure and the surrounding field offers a possible explanation. The observations show that jet-like EUV emission can occur in low-lying structures. The second ejection begins before the chromospheric and transition-region spectra have returned to their pre-event states. Its spectral signatures may therefore depend on the atmospheric changes associated with the first ejection as well as on the additional energy input.
ER -