High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions
M dwarfs show frequent flares and associated coronal mass ejections (CMEs) may significantly impact close-in habitable planets. M dwarf flares sometimes show blue/red asymmetries in the H α line profile, suggesting prominence eruptions as an early stage of CMEs. However, their high-time-cadence obse...
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2025-01-01
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| author | Yuto Kajikiya Kosuke Namekata Yuta Notsu Hiroyuki Maehara Bunei Sato Daisaku Nogami |
| author_facet | Yuto Kajikiya Kosuke Namekata Yuta Notsu Hiroyuki Maehara Bunei Sato Daisaku Nogami |
| author_sort | Yuto Kajikiya |
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| description | M dwarfs show frequent flares and associated coronal mass ejections (CMEs) may significantly impact close-in habitable planets. M dwarf flares sometimes show blue/red asymmetries in the H α line profile, suggesting prominence eruptions as an early stage of CMEs. However, their high-time-cadence observations are limited. We conducted spectroscopic monitoring observations of the active M dwarf YZ Canis Minoris with an ∼1 minute time cadence using the Seimei telescope, simultaneously with the optical photometric observations by Transiting Exoplanet Survey Satellite. We detected 27 H α flares with H α energies ranging from 1.7 × 10 ^29 to 3.8 × 10 ^32 erg and durations from 8 to 319 minutes. Among them, we identified three blue asymmetry and five red asymmetry events based on criteria using the Bayesian information criterion. The maximum velocity of the blueshifted and redshifted components ranges from 200 to 450 km s ^−1 and 190 to 400 km s ^−1 , respectively. The duration and time evolution show variety, and in particular, we discovered rapid, short-duration blue/red asymmetry events with the duration of 6–8 minutes. Among the eight blue/red asymmetry events, two blue and one red asymmetry events are interpreted as prominence eruptions because of their fast velocity and time evolution. Based on this interpretation, the lower limit of occurrence frequency of prominence eruptions can be estimated to be ∼1.1 events per day. Our discovery of short-duration events suggests that previous studies with low time cadence may have missed these events, potentially leading to an underestimation of the occurrence frequency of prominence eruptions/CMEs. |
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| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal |
| spelling | doaj-art-56ad038efde74dc19499f328cf695ff82025-01-20T13:38:47ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0197919310.3847/1538-4357/ad91b9High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence EruptionsYuto Kajikiya0https://orcid.org/0009-0000-2704-9785Kosuke Namekata1https://orcid.org/0000-0002-1297-9485Yuta Notsu2https://orcid.org/0000-0002-0412-0849Hiroyuki Maehara3https://orcid.org/0000-0003-0332-0811Bunei Sato4https://orcid.org/0000-0001-8033-5633Daisaku Nogami5https://orcid.org/0000-0001-9588-1872Department of Earth and Planetary Sciences, Institute of Science Tokyo , 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, JapanThe Hakubi Center for Advanced Research, Kyoto University , Yoshida-Honmachi, Sakyo-ku, Kyoto 606-8501, Japan; Department of Physics, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606-8502, Japan; Division of Science, National Astronomical Observatory of Japan , NINS, Osawa, Mitaka, Tokyo, 181-8588, Japan; Heliophysics Science Division, NASA Goddard Space Flight Center , 8800 Greenbelt Road, Greenbelt, MD 20771, USA; The Catholic University of America , 620 Michigan Avenue, N.E. Washington, DC 20064, USALaboratory for Atmospheric and Space Physics, University of Colorado Boulder , 3665 Discovery Drive, Boulder, CO 80303, USA; National Solar Observatory , 3665 Discovery Drive, Boulder, CO 80303, USASubaru Telescope Okayama Branch Office, National Astronomical Observatory of Japan , 3037-5 Honjo, Kamogata, Asakuchi, Okayama 719-0232, JapanDepartment of Earth and Planetary Sciences, Institute of Science Tokyo , 2-12-1 Ookayama, Meguro-ku, Tokyo 152-8551, JapanDepartment of Astronomy, Kyoto University , Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, JapanM dwarfs show frequent flares and associated coronal mass ejections (CMEs) may significantly impact close-in habitable planets. M dwarf flares sometimes show blue/red asymmetries in the H α line profile, suggesting prominence eruptions as an early stage of CMEs. However, their high-time-cadence observations are limited. We conducted spectroscopic monitoring observations of the active M dwarf YZ Canis Minoris with an ∼1 minute time cadence using the Seimei telescope, simultaneously with the optical photometric observations by Transiting Exoplanet Survey Satellite. We detected 27 H α flares with H α energies ranging from 1.7 × 10 ^29 to 3.8 × 10 ^32 erg and durations from 8 to 319 minutes. Among them, we identified three blue asymmetry and five red asymmetry events based on criteria using the Bayesian information criterion. The maximum velocity of the blueshifted and redshifted components ranges from 200 to 450 km s ^−1 and 190 to 400 km s ^−1 , respectively. The duration and time evolution show variety, and in particular, we discovered rapid, short-duration blue/red asymmetry events with the duration of 6–8 minutes. Among the eight blue/red asymmetry events, two blue and one red asymmetry events are interpreted as prominence eruptions because of their fast velocity and time evolution. Based on this interpretation, the lower limit of occurrence frequency of prominence eruptions can be estimated to be ∼1.1 events per day. Our discovery of short-duration events suggests that previous studies with low time cadence may have missed these events, potentially leading to an underestimation of the occurrence frequency of prominence eruptions/CMEs.https://doi.org/10.3847/1538-4357/ad91b9Stellar flaresStellar coronal mass ejectionsOptical flaresM dwarf starsFlare stars |
| spellingShingle | Yuto Kajikiya Kosuke Namekata Yuta Notsu Hiroyuki Maehara Bunei Sato Daisaku Nogami High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions The Astrophysical Journal Stellar flares Stellar coronal mass ejections Optical flares M dwarf stars Flare stars |
| title | High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions |
| title_full | High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions |
| title_fullStr | High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions |
| title_full_unstemmed | High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions |
| title_short | High-time-cadence Spectroscopy and Photometry of Stellar Flares on M dwarf YZ Canis Minoris with the Seimei Telescope and TESS. I. Discovery of Rapid and Short-duration Prominence Eruptions |
| title_sort | high time cadence spectroscopy and photometry of stellar flares on m dwarf yz canis minoris with the seimei telescope and tess i discovery of rapid and short duration prominence eruptions |
| topic | Stellar flares Stellar coronal mass ejections Optical flares M dwarf stars Flare stars |
| url | https://doi.org/10.3847/1538-4357/ad91b9 |
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