{"@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/1360005669368893440.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4357/ab14e6"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/ab14e6/pdf"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/ab14e6"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1904.00142"}},{"identifier":{"@type":"HANDLE","@value":"1887/85026"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Do Kepler Superflare Stars Really Include Slowly Rotating Sun-like Stars?—Results Using APO 3.5 m Telescope Spectroscopic Observations and Gaia-DR2 Data"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>We report the latest view of <jats:italic>Kepler</jats:italic> solar-type (G-type main-sequence) superflare stars, including recent updates with Apache Point Observatory (APO) 3.5 m telescope spectroscopic observations and <jats:italic>Gaia</jats:italic>-DR2 data. First, we newly conducted APO 3.5 m spectroscopic observations of 18 superflare stars found from <jats:italic>Kepler</jats:italic> 1-minute time-cadence data. More than half (43 stars) are confirmed to be “single” stars, among 64 superflare stars in total that have been spectroscopically investigated so far in this APO 3.5 m and our previous Subaru/HDS observations. The measurements of <jats:italic>v</jats:italic> sin <jats:italic>i</jats:italic> (projected rotational velocity) and chromospheric lines (Ca <jats:sc>ii</jats:sc> H and K and Ca <jats:sc>ii</jats:sc>\n                  <jats:italic>λ</jats:italic>8542) support that the brightness variation of superflare stars is caused by the rotation of a star with large starspots. We then investigated the statistical properties of <jats:italic>Kepler</jats:italic> solar-type superflare stars by incorporating <jats:italic>Gaia</jats:italic>-DR2 stellar radius estimates. As a result, the maximum superflare energy continuously decreases as the rotation period <jats:italic>P</jats:italic>\n                  <jats:sub>rot</jats:sub> increases. Superflares with energies ≲5 × 10<jats:sup>34</jats:sup> erg occur on old, slowly rotating Sun-like stars (<jats:italic>P</jats:italic>\n                  <jats:sub>rot</jats:sub> ∼ 25 days) approximately once every 2000–3000 yr, while young, rapidly rotating stars with <jats:italic>P</jats:italic>\n                  <jats:sub>rot</jats:sub> ∼ a few days have superflares up to 10<jats:sup>36</jats:sup> erg. The maximum starspot area does not depend on the rotation period when the star is young, but as the rotation slows down, it starts to steeply decrease at <jats:italic>P</jats:italic>\n                  <jats:sub>rot</jats:sub> ≳ 12 days for Sun-like stars. These two decreasing trends are consistent since the magnetic energy stored around starspots explains the flare energy, but other factors like spot magnetic structure should also be considered.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380005669368893316","@type":"Researcher","foaf:name":[{"@value":"Yuta Notsu"}]},{"@id":"https://cir.nii.ac.jp/crid/1420564276185218048","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"40456851"},{"@type":"NRID","@value":"1000040456851"},{"@type":"ORCID","@value":"0000-0003-0332-0811"},{"@type":"NRID","@value":"9000249538160"},{"@type":"NRID","@value":"9000323844365"},{"@type":"NRID","@value":"9000250750216"},{"@type":"NRID","@value":"9000237870922"},{"@type":"NRID","@value":"9000244902160"},{"@type":"NRID","@value":"9000310465778"},{"@type":"NRID","@value":"9000019229102"},{"@type":"NRID","@value":"9000403553662"},{"@type":"NRID","@value":"9000285477513"},{"@type":"NRID","@value":"9000399527262"},{"@type":"NRID","@value":"9000403553716"},{"@type":"NRID","@value":"9000237870991"},{"@type":"NRID","@value":"9000244901889"},{"@type":"NRID","@value":"9000253678536"},{"@type":"NRID","@value":"9000246809119"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/h.maehara"}],"foaf:name":[{"@value":"Hiroyuki Maehara"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005669368893572","@type":"Researcher","foaf:name":[{"@value":"Satoshi Honda"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005669368893825","@type":"Researcher","foaf:name":[{"@value":"Suzanne L. Hawley"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005669368893697","@type":"Researcher","foaf:name":[{"@value":"James R. A. Davenport"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005669368893569","@type":"Researcher","foaf:name":[{"@value":"Kosuke Namekata"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005669368893570","@type":"Researcher","foaf:name":[{"@value":"Shota Notsu"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005669368893828","@type":"Researcher","foaf:name":[{"@value":"Kai Ikuta"}]},{"@id":"https://cir.nii.ac.jp/crid/1420282801206033536","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"20332728"},{"@type":"NRID","@value":"1000020332728"},{"@type":"ORCID","@value":"0000-0001-9588-1872"},{"@type":"NRID","@value":"9000000122293"},{"@type":"NRID","@value":"9000237871111"},{"@type":"NRID","@value":"9000242546870"},{"@type":"NRID","@value":"9000237871074"},{"@type":"NRID","@value":"9000323844370"},{"@type":"NRID","@value":"9000279644560"},{"@type":"NRID","@value":"9000237871072"},{"@type":"NRID","@value":"9000237871300"},{"@type":"NRID","@value":"9000262347417"},{"@type":"NRID","@value":"9000401948763"},{"@type":"NRID","@value":"9000237871073"},{"@type":"NRID","@value":"9000000122110"},{"@type":"NRID","@value":"9000237870989"},{"@type":"NRID","@value":"9000313618294"},{"@type":"NRID","@value":"9000305623653"},{"@type":"NRID","@value":"9000290358365"},{"@type":"NRID","@value":"9000014145387"},{"@type":"NRID","@value":"9000244901817"},{"@type":"NRID","@value":"9000237871157"},{"@type":"NRID","@value":"9000275831899"},{"@type":"NRID","@value":"9000237871327"},{"@type":"NRID","@value":"9000250750332"},{"@type":"NRID","@value":"9000237871274"},{"@type":"NRID","@value":"9000237870356"},{"@type":"NRID","@value":"9000341541965"},{"@type":"NRID","@value":"9000000122412"},{"@type":"NRID","@value":"9000237871112"},{"@type":"NRID","@value":"9000237871178"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/read0069959"}],"foaf:name":[{"@value":"Daisaku Nogami"}]},{"@id":"https://cir.nii.ac.jp/crid/1380005669368893699","@type":"Researcher","foaf:name":[{"@value":"Kazunari Shibata"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"0004637X"},{"@type":"EISSN","@value":"15384357"},{"@type":"PISSN","@value":"https://id.crossref.org/issn/0004637X"}],"prism:publicationName":[{"@value":"The Astrophysical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2019-05-01","prism:volume":"876","prism:number":"1","prism:startingPage":"58"},"reviewed":"false","dc:rights":["https://iopscience.iop.org/page/copyright","https://iopscience.iop.org/info/page/text-and-data-mining"],"url":[{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/ab14e6/pdf"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/ab14e6"}],"createdAt":"2019-05-03","modifiedAt":"2024-01-12","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Earth%20and%20Planetary%20Astrophysics%20(astro-ph.EP)","dc:title":"Earth and Planetary Astrophysics (astro-ph.EP)"},{"@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=FOS:%20Physical%20sciences","dc:title":"FOS: Physical sciences"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20and%20Stellar%20Astrophysics%20(astro-ph.SR)","dc:title":"Solar and Stellar Astrophysics (astro-ph.SR)"},{"@id":"https://cir.nii.ac.jp/all?q=Astrophysics%20-%20Earth%20and%20Planetary%20Astrophysics","dc:title":"Astrophysics - Earth and Planetary Astrophysics"}],"project":[{"@id":"https://cir.nii.ac.jp/crid/1040000781996075264","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"18J20048"},{"@type":"JGN","@value":"JP18J20048"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-18J20048/"}],"notation":[{"@language":"ja","@value":"恒星観測から迫る、太陽・恒星の磁気活動性の統一的理解"},{"@language":"en","@value":"Observational Studies of Solar-type Stars toward an Universal Understanding of Solar and Stellar Magnetic Activity"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282256880745984","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"16J00320"},{"@type":"JGN","@value":"JP16J00320"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16J00320/"}],"notation":[{"@language":"ja","@value":"スーパーフレア星の観測から迫る、太陽型恒星の磁気活動とダイナモ理論"},{"@language":"en","@value":"Magnetic activities of solar-type stars and dynamo theory investigated through the observations of superflare stars"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282256932838016","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"17H02865"},{"@type":"JGN","@value":"JP17H02865"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-17H02865/"}],"notation":[{"@language":"ja","@value":"高速分光観測による恒星フレアの機構の解明"},{"@language":"en","@value":"Investigation of the mechanism of stellar flares by high speed spectroscopy"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282256942312320","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"17K05400"},{"@type":"JGN","@value":"JP17K05400"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-17K05400/"}],"notation":[{"@language":"ja","@value":"太陽型星の高精度測光データから探る巨大黒点の性質とスーパーフレアの関係"},{"@language":"en","@value":"On the correlation between starspot activity and superflares on solar-type stars"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050282810809482624","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Statistical properties of superflares on solar-type stars based on 1-min cadence data"}]},{"@id":"https://cir.nii.ac.jp/crid/1050295956119976960","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Discovery of a Long-duration Superflare on a Young Solar-type Star EK Draconis with Nearly Similar Time Evolution for H alpha and White-light Emissions"},{"@value":"Discovery of a Long-duration Superflare on a Young Solar-type Star EK Draconis with Nearly Similar Time Evolution for Hα and White-light Emissions"},{"@value":"Discovery of a long-duration superflare on a young solar-type star EK Draconis with nearly similar time evolution for Ha and white-light emissions"}]},{"@id":"https://cir.nii.ac.jp/crid/1050296575288219008","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Starspot Mapping with Adaptive Parallel Tempering. 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STATISTICAL PROPERTIES OF SUPERFLARES"}]},{"@id":"https://cir.nii.ac.jp/crid/1360283692627477760","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"High dispersion spectroscopy of solar-type superflare stars. I. 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