{"@context":{"@vocab":"https://cir.nii.ac.jp/schema/1.0/","rdfs":"http://www.w3.org/2000/01/rdf-schema#","dc":"http://purl.org/dc/elements/1.1/","dcterms":"http://purl.org/dc/terms/","foaf":"http://xmlns.com/foaf/0.1/","prism":"http://prismstandard.org/namespaces/basic/2.0/","cinii":"http://ci.nii.ac.jp/ns/1.0/","datacite":"https://schema.datacite.org/meta/kernel-4/","ndl":"http://ndl.go.jp/dcndl/terms/","jpcoar":"https://github.com/JPCOAR/schema/blob/master/2.0/"},"@id":"https://cir.nii.ac.jp/crid/1360869854377746176.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/2041-8213/ad5667"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/2041-8213/ad5667"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/2041-8213/ad5667/pdf"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"High-velocity Blue-shifted Fe xxv Heα Line during a Superflare of the RS Canum Venaticorum–type Star IM Peg"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>The Monitor of All-sky X-ray Image (MAXI) detected a superflare, releasing 5 × 10<jats:sup>37</jats:sup> erg in 2−10 keV, of the RS CVn-type star IM Peg at 10:41 UT on 2023 July 23 with its Gas Slit Camera (2−30 keV). We conducted X-ray follow-up observations of the superflare with the Neutron Star Interior Composition Explorer (NICER; 0.2−12 keV) starting at 16:52 UT on July 23 until 06:00 UT on August 2. NICER X-ray spectra clearly showed emission lines of the Fe <jats:sc>xxv</jats:sc> He<jats:italic>α</jats:italic> and Fe <jats:sc>xxvi</jats:sc> Ly<jats:italic>α</jats:italic> for ∼1.5 days since the MAXI detection. The Fe XXV He<jats:italic>α</jats:italic> line was blueshifted with its maximum Doppler velocity reaching −2200 ± 600 km s<jats:sup>−1</jats:sup>, suggesting an upward-moving plasma during the flare, such as a coronal mass ejection (CME) and/or chromospheric evaporation. This is the first case that the Fe <jats:sc>xxv</jats:sc> He<jats:italic>α</jats:italic> line is blueshifted during a stellar flare, and its velocity overwhelmingly exceeds the escape velocity of the star (−230 km s<jats:sup>−1</jats:sup>). One hour before the most pronounced blueshift detection, a signature of the reheating of the flare plasma was observed. We discuss the origin of the blueshift, a CME, or high-velocity chromospheric evaporation.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380869854377746178","@type":"Researcher","foaf:name":[{"@value":"Shun Inoue"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746307","@type":"Researcher","foaf:name":[{"@value":"Wataru Buz Iwakiri"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746182","@type":"Researcher","foaf:name":[{"@value":"Teruaki Enoto"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746179","@type":"Researcher","foaf:name":[{"@value":"Hiroyuki Uchida"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746183","@type":"Researcher","foaf:name":[{"@value":"Miki Kurihara"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746180","@type":"Researcher","foaf:name":[{"@value":"Masahiro Tsujimoto"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746048","@type":"Researcher","foaf:name":[{"@value":"Yuta Notsu"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746198","@type":"Researcher","foaf:name":[{"@value":"Kenji Hamaguchi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746210","@type":"Researcher","foaf:name":[{"@value":"Keith Gendreau"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746304","@type":"Researcher","foaf:name":[{"@value":"Zaven Arzoumanian"}]},{"@id":"https://cir.nii.ac.jp/crid/1380869854377746314","@type":"Researcher","foaf:name":[{"@value":"Takeshi Go Tsuru"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"20418205"},{"@type":"EISSN","@value":"20418213"}],"prism:publicationName":[{"@value":"The Astrophysical Journal Letters"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2024-06-26","prism:volume":"969","prism:number":"1","prism:startingPage":"L12"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","dc:rights":["http://creativecommons.org/licenses/by/4.0/","https://iopscience.iop.org/info/page/text-and-data-mining"],"url":[{"@id":"https://iopscience.iop.org/article/10.3847/2041-8213/ad5667"},{"@id":"https://iopscience.iop.org/article/10.3847/2041-8213/ad5667/pdf"}],"createdAt":"2024-06-27","modifiedAt":"2024-06-27","project":[{"@id":"https://cir.nii.ac.jp/crid/1040581456520393728","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"24KJ1483"},{"@type":"JGN","@value":"JP24KJ1483"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-24KJ1483/"}],"notation":[{"@language":"ja","@value":"多波長観測で明らかにする恒星磁気活動とその惑星形成への影響"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050572633033232896","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Probable detection of an eruptive filament from a superflare on a solar-type star"}]},{"@id":"https://cir.nii.ac.jp/crid/1050858906073401728","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Detection of a High-velocity Prominence Eruption Leading to a CME Associated with a Superflare on the RS CVn-type Star V1355 Orionis"}]},{"@id":"https://cir.nii.ac.jp/crid/1360017285250533376","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Solar Filament Eruptions as Precursors to Flare–CME Events: Establishing the Temporal Connection"}]},{"@id":"https://cir.nii.ac.jp/crid/1360021389808607360","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Apache Point Observatory (APO)/SMARTS Flare Star Campaign Observations. 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