Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis
Stellar coronal mass ejections (CMEs) have recently received much attention for their impacts on exoplanets and stellar evolution. Detecting prominence eruptions, the initial phase of CMEs, as the blueshifted excess component of Balmer lines is a technique to capture stellar CMEs. However, most of p...
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/acb7e8 |
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| author | Shun Inoue Hiroyuki Maehara Yuta Notsu Kosuke Namekata Satoshi Honda Keiichi Namizaki Daisaku Nogami Kazunari Shibata |
| author_facet | Shun Inoue Hiroyuki Maehara Yuta Notsu Kosuke Namekata Satoshi Honda Keiichi Namizaki Daisaku Nogami Kazunari Shibata |
| author_sort | Shun Inoue |
| collection | DOAJ |
| description | Stellar coronal mass ejections (CMEs) have recently received much attention for their impacts on exoplanets and stellar evolution. Detecting prominence eruptions, the initial phase of CMEs, as the blueshifted excess component of Balmer lines is a technique to capture stellar CMEs. However, most of prominence eruptions identified thus far have been slow and less than the surface escape velocity. Therefore, whether these eruptions were developing into CMEs remained unknown. In this study, we conducted simultaneous optical photometric observations with Transiting Exoplanet Survey Satellite and optical spectroscopic observations with the 3.8 m Seimei Telescope for the RS CVn-type star V1355 Orionis that frequently produces large-scale superflares. We detected a superflare releasing 7.0 × 10 ^35 erg. In the early stage of this flare, a blueshifted excess component of H α extending its velocity up to 760–1690 km s ^−1 was observed and thought to originate from prominence eruptions. The velocity greatly exceeds the escape velocity (i.e., ∼350 km s ^−1 ), which provides important evidence that stellar prominence eruptions can develop into CMEs. Furthermore, we found that the prominence is very massive (9.5 × 10 ^18 g < M < 1.4 × 10 ^21 g). These data will clarify whether such events follow existing theories and scaling laws on solar flares and CMEs even when the energy scale far exceeds solar cases. |
| first_indexed | 2024-03-12T04:49:35Z |
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| id | doaj.art-111d0966a0f84e22a1fedb9084c0c765 |
| institution | Directory Open Access Journal |
| issn | 1538-4357 |
| language | English |
| last_indexed | 2024-03-12T04:49:35Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj.art-111d0966a0f84e22a1fedb9084c0c7652023-09-03T09:24:19ZengIOP PublishingThe Astrophysical Journal1538-43572023-01-019481910.3847/1538-4357/acb7e8Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 OrionisShun Inoue0https://orcid.org/0000-0003-3085-304XHiroyuki Maehara1https://orcid.org/0000-0003-0332-0811Yuta Notsu2https://orcid.org/0000-0002-0412-0849Kosuke Namekata3https://orcid.org/0000-0002-1297-9485Satoshi Honda4https://orcid.org/0000-0001-6653-8741Keiichi Namizaki5Daisaku Nogami6https://orcid.org/0000-0001-9588-1872Kazunari Shibata7https://orcid.org/0000-0003-1206-7889Department of Physics, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606–8502, Japan ; inoue.shun.57c@kyoto-u.jpOkayama Branch Office, Subaru Telescope, NAOJ, NINS , Kamogata, Asakuchi, Okayama, 719–0232, JapanLaboratory 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, USA; Department of Earth and Planetary Sciences, Tokyo Institute of Technology , Ookayama, Meguro-ku, Tokyo, 152–8551, JapanALMA Project, NAOJ, NINS , Osawa, Mitaka, Tokyo, 181–8588, JapanNishi-Harima Astronomical Observatory, Center for Astronomy, University of Hyogo , Sayo, Hyogo, 679–5313, JapanDepartment of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606–8502, JapanDepartment of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, 606–8502, Japan; Astronomical Observatory, Kyoto University , Sakyo-ku, Kyoto, 606–8502, JapanKwasan Observatory, Kyoto University , Yamashina, Kyoto, 607–8471, Japan; School of Science and Engineering, Doshisha University , Kyotanabe, Kyoto, 610–0321, JapanStellar coronal mass ejections (CMEs) have recently received much attention for their impacts on exoplanets and stellar evolution. Detecting prominence eruptions, the initial phase of CMEs, as the blueshifted excess component of Balmer lines is a technique to capture stellar CMEs. However, most of prominence eruptions identified thus far have been slow and less than the surface escape velocity. Therefore, whether these eruptions were developing into CMEs remained unknown. In this study, we conducted simultaneous optical photometric observations with Transiting Exoplanet Survey Satellite and optical spectroscopic observations with the 3.8 m Seimei Telescope for the RS CVn-type star V1355 Orionis that frequently produces large-scale superflares. We detected a superflare releasing 7.0 × 10 ^35 erg. In the early stage of this flare, a blueshifted excess component of H α extending its velocity up to 760–1690 km s ^−1 was observed and thought to originate from prominence eruptions. The velocity greatly exceeds the escape velocity (i.e., ∼350 km s ^−1 ), which provides important evidence that stellar prominence eruptions can develop into CMEs. Furthermore, we found that the prominence is very massive (9.5 × 10 ^18 g < M < 1.4 × 10 ^21 g). These data will clarify whether such events follow existing theories and scaling laws on solar flares and CMEs even when the energy scale far exceeds solar cases.https://doi.org/10.3847/1538-4357/acb7e8Stellar flaresStellar coronal mass ejectionsStellar mass loss |
| spellingShingle | Shun Inoue Hiroyuki Maehara Yuta Notsu Kosuke Namekata Satoshi Honda Keiichi Namizaki Daisaku Nogami Kazunari Shibata Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis The Astrophysical Journal Stellar flares Stellar coronal mass ejections Stellar mass loss |
| title | Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis |
| title_full | Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis |
| title_fullStr | Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis |
| title_full_unstemmed | Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis |
| title_short | Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis |
| title_sort | detection of a high velocity prominence eruption leading to a cme associated with a superflare on the rs cvn type star v1355 orionis |
| topic | Stellar flares Stellar coronal mass ejections Stellar mass loss |
| url | https://doi.org/10.3847/1538-4357/acb7e8 |
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