Issue |
A&A
Volume 695, March 2025
|
|
---|---|---|
Article Number | L2 | |
Number of page(s) | 9 | |
Section | Letters to the Editor | |
DOI | https://doi.org/10.1051/0004-6361/202452857 | |
Published online | 25 February 2025 |
Letter to the Editor
A filament eruption on the RS CVn-type star UX Ari
1
Yunnan Observatories, Chinese Academy of Sciences, Kunming 650216, China
2
Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650216, China
3
International Centre of Supernovae, Yunnan Key Laboratory, Kunming 650216, China
4
School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing 101408, China
⋆ Corresponding authors; dtcao@ynao.ac.cn; shenghonggu@ynao.ac.cn
Received:
4
November
2024
Accepted:
31
January
2025
Context. Stellar flares can be accompanied by filament or prominence eruptions, which may lead to stellar coronal mass ejections (CMEs) that have significant impacts on surrounding exoplanets and stellar evolution.
Aims. We report the capture of a filament eruption associated with an optical flare on the RS CVn-type star UX Ari.
Methods. Based on high-resolution spectroscopic observations, we investigated the Doppler-shifted absorption features appeared in the Hα flaring spectra, which can be indicative of a filament eruption.
Results. A huge optical flare was observed, which lasted for at least 150 hours and released an energy of about 1.47 × 1037 erg in the Hα line. The corresponding bolometric white-light energy is converted to be 1.03 × 1039 erg, indicating that the flare is comparable to the most intense stellar superflares. A blueshifted absorption feature with a bulk velocity of −143.9 km s−1 emerged in the Hα line region during the initial phase of the flare, which then decelerated and turned into redshifted absorption. This suggests that a filament eruption happened and ultimately fell back toward the star, suggesting that it represents a failed filament eruption. The erupted filament mass of 8.5 − 15.0 × 1020 g and the kinetic energy of 8.8 − 15.5 × 1034 erg are derived. Furthermore, the relationship between the filament eruption and the flare is likely characterized by a sympathetic eruption.
Key words: Sun: coronal mass ejections (CMEs) / Sun: filaments / prominences / stars: chromospheres / stars: coronae / stars: flare
© The Authors 2025
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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