{"@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/1360004239676282240.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4357/aaebfc"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/869/i=2/a=99/pdf"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/869/i=2/a=99?key=crossref.00e9647cb345c28f6a46ce2b8d141e68"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/aaebfc"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/aaebfc/pdf"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1810.10808"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Statistical Relation between Solar Flares and Coronal Mass Ejections with Respect to Sigmoidal Structures in Active Regions"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>Statistical dependences among features of coronal mass ejections (CMEs), solar flares, and sigmoidal structures in soft-X-ray images were investigated. We applied analysis methods to all the features in the same way in order to investigate the reproducibility of the correlations among them, which may be found from previous statistical studies. Samples of 211 M-class and X-class flares, observed between 2006 and 2015 by the <jats:italic>Hinode</jats:italic>/X-ray telescope, <jats:italic>Solar and Heliospheric Observatory</jats:italic>/Large Angle and Spectrometric Coronagraph, and <jats:italic>Geostationary Operational Environmental Satellite</jats:italic>, were examined statistically. Five kinds of analysis were performed: occurrence rate analysis, linear-correlation analysis, association analysis, the Kolmogorov<jats:italic>–</jats:italic>Smirnov test, and the Anderson–Darling test. These give three main results. First, the sigmoidal structure and long-duration events (LDEs) have a stronger dependence on CME occurrence than large X-ray-class events in on-disk events. Second, for the limb events, a significant dependence exists between LDEs and CME occurrence, and between X-ray-class events and CME occurrence. Third, 32.4% of on-disk flare events have sigmoidal structure and are not accompanied by CMEs. However, the occurrence probability of CMEs without sigmoidal structure is very small, 8.8%, in on-disk events. While the first and second results are consistent with previous studies, we provide for the first time a difference between the on-disk and limb events. The third result, that non-sigmoidal regions produce fewer eruptive events, is also different from previous results. We suggest that sigmoidal structures in soft X-ray images will be a helpful feature for CME prediction in on-disk flare events.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004239676282122","@type":"Researcher","foaf:name":[{"@value":"Yusuke Kawabata"}]},{"@id":"https://cir.nii.ac.jp/crid/1420282801194270464","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"10706328"},{"@type":"NRID","@value":"1000010706328"},{"@type":"NRID","@value":"9000248219128"},{"@type":"NRID","@value":"9000287285261"},{"@type":"NRID","@value":"9000309174705"},{"@type":"NRID","@value":"9000412386601"},{"@type":"NRID","@value":"9000287285295"},{"@type":"NRID","@value":"9000014612721"},{"@type":"NRID","@value":"9000264265536"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/7000015518"}],"foaf:name":[{"@value":"Yusuke Iida"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239676282243","@type":"Researcher","foaf:name":[{"@value":"Takafumi Doi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239676282246","@type":"Researcher","foaf:name":[{"@value":"Sachiko Akiyama"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239676282241","@type":"Researcher","foaf:name":[{"@value":"Seiji Yashiro"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239676282247","@type":"Researcher","foaf:name":[{"@value":"Toshifumi Shimizu"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"0004637X"},{"@type":"EISSN","@value":"15384357"}],"prism:publicationName":[{"@value":"The Astrophysical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2018-12-14","prism:volume":"869","prism:number":"2","prism:startingPage":"99"},"reviewed":"false","dc:rights":["https://iopscience.iop.org/page/copyright","https://iopscience.iop.org/info/page/text-and-data-mining"],"url":[{"@id":"http://stacks.iop.org/0004-637X/869/i=2/a=99/pdf"},{"@id":"http://stacks.iop.org/0004-637X/869/i=2/a=99?key=crossref.00e9647cb345c28f6a46ce2b8d141e68"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/aaebfc"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/aaebfc/pdf"}],"createdAt":"2018-12-14","modifiedAt":"2024-01-12","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=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)"}],"project":[{"@id":"https://cir.nii.ac.jp/crid/1040000781833807488","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"15H05814"},{"@type":"JGN","@value":"JP15H05814"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PLANNED-15H05814/"}],"notation":[{"@language":"ja","@value":"太陽嵐の発生機構の解明と予測"},{"@language":"en","@value":"Understanding and prediction of the solar storm"}]},{"@id":"https://cir.nii.ac.jp/crid/1040000782439968640","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"15H05750"},{"@type":"JGN","@value":"JP15H05750"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-15H05750/"}],"notation":[{"@language":"ja","@value":"2次元画像比較を駆使した超高磁場リコネクションの巨大加熱・加速の解明と応用開拓"},{"@language":"en","@value":"Phyisics and Applications of High-Power Heating / Acceleration of Ultra-High Field Magnetic Reconnection by Use of 2D Imaging 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