{"@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/1360857593673665536.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1093/pasj/psac008"}},{"identifier":{"@type":"URI","@value":"https://academic.oup.com/pasj/article-pdf/74/2/477/54646466/psac008.pdf"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"X-ray/Hα scaling relationships in stellar flares"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>We report on the results of our simultaneous observations of three large stellar flares with soft X-rays (SXRs) and an Hα emission line from two binary systems of RS CVn type. The energies released in the X-ray and Hα emissions during the flares were 1036–1038 and 1035–1037 erg, respectively. This renders the set of the observations as the first successful simultaneous X-ray/Hα observations of the stellar flares with energies above 1035 erg; although the coverage of the Hα observations was limited, with $\\sim\\! 10\\%$ of the e-folding time in the decay phase of the flares, that of the SXR ones was complete. Combining the obtained physical parameters and those in literature for solar and stellar flares, we obtained a good proportional relation between the emitted energies of X-ray and Hα emissions for a flare energy range of 1029–1038 erg. The ratio of the Hα-line to bolometric X-ray emissions was ∼0.1, where the latter was estimated by converting the observed SXR emission to that in the 0.1–100 keV band according to the best-fitting thin thermal model. We also found that the e-folding times of the SXR and Hα light curves in the decaying phase of a flare are in agreement for a time range of 1–104 s. Even very large stellar flares with energies of six orders of magnitude larger than the most energetic solar flares follow the same scaling relationships with solar and much less energetic stellar flares. This fact suggests that their physical parameters can be estimated on the basis of the known physics of solar and stellar flares.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380298339679160464","@type":"Researcher","foaf:name":[{"@value":"Hiroki Kawai"}],"jpcoar:affiliationName":[{"@value":"Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1420282801200494464","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"70349223"},{"@type":"NRID","@value":"1000070349223"},{"@type":"NRID","@value":"9000010601522"},{"@type":"NRID","@value":"9000000120778"},{"@type":"NRID","@value":"9000331897754"},{"@type":"NRID","@value":"9000107395664"},{"@type":"NRID","@value":"9000237738480"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/read0083960"}],"foaf:name":[{"@value":"Yohko Tsuboi"}],"jpcoar:affiliationName":[{"@value":"Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380298339679160320","@type":"Researcher","foaf:name":[{"@value":"Wataru B Iwakiri"}],"jpcoar:affiliationName":[{"@value":"Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan"},{"@value":"RIKEN , 2-1 Hirosawa, Wako, Saitama 351-0198 , Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1420282801190430592","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"80342624"},{"@type":"NRID","@value":"1000080342624"},{"@type":"NRID","@value":"9000364781501"},{"@type":"NRID","@value":"9000412300529"},{"@type":"NRID","@value":"9000401950150"},{"@type":"NRID","@value":"9000388528799"},{"@type":"NRID","@value":"9000016669163"},{"@type":"NRID","@value":"9000264863274"},{"@type":"NRID","@value":"9000242630268"},{"@type":"NRID","@value":"9000006973425"},{"@type":"NRID","@value":"9000242572457"},{"@type":"NRID","@value":"9000402479592"},{"@type":"NRID","@value":"9000415101408"},{"@type":"NRID","@value":"9000264864012"},{"@type":"NRID","@value":"9000415102541"},{"@type":"NRID","@value":"9000244901634"},{"@type":"NRID","@value":"9000331897887"},{"@type":"NRID","@value":"9000408819486"},{"@type":"NRID","@value":"9000408819482"},{"@type":"NRID","@value":"9000401950541"},{"@type":"NRID","@value":"9000010161496"},{"@type":"NRID","@value":"9000238235541"},{"@type":"NRID","@value":"9000082935337"},{"@type":"NRID","@value":"9000376939844"},{"@type":"NRID","@value":"9000290358393"},{"@type":"NRID","@value":"9000408815804"},{"@type":"NRID","@value":"9000401950458"},{"@type":"NRID","@value":"9000404796482"},{"@type":"NRID","@value":"9000408828487"},{"@type":"NRID","@value":"9000408828493"},{"@type":"NRID","@value":"9000408843276"},{"@type":"NRID","@value":"9000408843257"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/yoshitomomaeda"}],"foaf:name":[{"@value":"Yoshitomo Maeda"}],"jpcoar:affiliationName":[{"@value":"Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency , 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5258 , Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380298339679160449","@type":"Researcher","foaf:name":[{"@value":"Satoru Katsuda"}],"jpcoar:affiliationName":[{"@value":"Graduate School of Science and Engineering, Saitama University , 255 Shimo-Okubo, Sakura-ku, Saitama, Saitama 338-8570 , Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380298339679160330","@type":"Researcher","foaf:name":[{"@value":"Ryo Sasaki"}],"jpcoar:affiliationName":[{"@value":"Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380298339679160457","@type":"Researcher","foaf:name":[{"@value":"Junya Kohara"}],"jpcoar:affiliationName":[{"@value":"Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00046264"},{"@type":"EISSN","@value":"2053051X"}],"prism:publicationName":[{"@value":"Publications of the Astronomical Society of Japan"}],"dc:publisher":[{"@value":"Oxford University Press (OUP)"}],"prism:publicationDate":"2022-03-21","prism:volume":"74","prism:number":"2","prism:startingPage":"477","prism:endingPage":"487"},"reviewed":"false","dc:rights":["https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model"],"url":[{"@id":"https://academic.oup.com/pasj/article-pdf/74/2/477/54646466/psac008.pdf"}],"createdAt":"2022-02-04","modifiedAt":"2023-12-22","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20Solar%20and%20Stellar%20Astrophysics","dc:title":"Astrophysics - Solar and Stellar Astrophysics"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20High%20Energy%20Astrophysical%20Phenomena","dc:title":"Astrophysics - High Energy Astrophysical Phenomena"}],"project":[{"@id":"https://cir.nii.ac.jp/crid/1040282256942297344","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"17K05392"},{"@type":"JGN","@value":"JP17K05392"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-17K05392/"}],"notation":[{"@language":"ja","@value":"恒星ハイパーフレアの発生環境の解明"},{"@language":"en","@value":"The physical environment when stellar hyper flares occur"}]},{"@id":"https://cir.nii.ac.jp/crid/1040566775636411008","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"19K21886"},{"@type":"JGN","@value":"JP19K21886"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-19K21886/"}],"notation":[{"@language":"ja","@value":"分光・偏光・撮像の3大観測能力を高いレベルで備えた新しいX線望遠鏡の開発"},{"@language":"en","@value":"Development of high-resolution Imaging and spectroscopic polarimetry"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050856893077653760","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Coalescence of black hole–neutron star binaries"},{"@value":"Solar flares: Magnetohydrodynamic processes"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002217650647040","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Gas Slit Camera (GSC) onboard MAXI on ISS"}]},{"@id":"https://cir.nii.ac.jp/crid/1360016868679760512","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Coordinated Exosat and spectroscopic observations of flare stars and coronal heating"}]},{"@id":"https://cir.nii.ac.jp/crid/1360283692627536128","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The MAXI/GSC Nova-Alert System and results of its first 68 months"}]},{"@id":"https://cir.nii.ac.jp/crid/1360290617548676096","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The RS CVn–type Star GT Mus Shows Most Energetic X-Ray Flares Throughout the 2010s"}]},{"@id":"https://cir.nii.ac.jp/crid/1360290617877265280","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Optical and X-ray observations of stellar flares on an active M dwarf AD Leonis with the Seimei Telescope, SCAT, NICER, and OISTER"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292618759031296","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The MAXI Mission on the ISS: Science and Instruments for Monitoring All-Sky X-Ray Images"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292621201478016","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Collisional Plasma Models with APEC/APED: Emission-Line Diagnostics of Hydrogen-like and Helium-like Ions"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292621325887488","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"ACCELERATION, MAGNETIC FLUCTUATIONS, AND CROSS-FIELD TRANSPORT OF ENERGETIC ELECTRONS IN A SOLAR FLARE LOOP"}]},{"@id":"https://cir.nii.ac.jp/crid/1360294646640489856","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The<i>XMM-Newton</i>serendipitous survey"}]},{"@id":"https://cir.nii.ac.jp/crid/1360298340984616448","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Optical identification of H0123 + 075 and 4U 1137-65 - 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