{"@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/1360572092575653760.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4357/abbacb"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/abbacb/pdf"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/abbacb"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Statistical and Observational Research on Solar Flare EUV Spectra and Geometrical Features"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>We performed statistical analysis on the flare emission data to examine parameters related to the flare extreme-ultraviolet (EUV) spectra. This study used the data from the Geostationary Operational Environmental Satellite X-ray Sensors to determine the fundamental flare parameters. The relationship between soft X-ray data and EUV emission data observed by the Extreme Ultraviolet Variability Experiment on board the Solar Dynamics Observatory (SDO) MEGS-A was investigated for 50 events. The results showed the hotter Fe line emissions have strong correlation with soft X-ray data in many cases. However, our statistical study revealed that EUV flare peak flux of Fe <jats:sc>xv</jats:sc>, Fe <jats:sc>xvi</jats:sc> and He <jats:sc>ii</jats:sc> lines have weak correlation with soft X-ray peak flux. In EUV line light curves, there was time difference in peak time, however the tendency to reach the peak in order from the hotter line to cooler line was not so clear. These results indicate that the temporal evolution of EUV emission can be roughly explained by soft X-ray data. However, the time changes of temperature and density distributions in the flare loop must be needed for accurate reproduction. Moreover, we compared the geometrical features of solar flares observed by the Atmospheric Imaging Assembly on board the SDO with the fundamental flare parameters for 32 events. The ribbon distance strongly correlated with both soft X-ray flare rise and decay times. This results indicate that the geometrical feature is essential parameter for predicting flare emission duration.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380572092575653767","@type":"Researcher","foaf:name":[{"@value":"Shohei Nishimoto"}]},{"@id":"https://cir.nii.ac.jp/crid/1380572092575653645","@type":"Researcher","foaf:name":[{"@value":"Kyoko Watanabe"}]},{"@id":"https://cir.nii.ac.jp/crid/1420001326209703424","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"40547965"},{"@type":"NRID","@value":"1000040547965"},{"@type":"NRID","@value":"9000014612722"},{"@type":"NRID","@value":"9000279645484"},{"@type":"NRID","@value":"9000414093069"},{"@type":"NRID","@value":"9000242559934"},{"@type":"NRID","@value":"9000415345102"},{"@type":"NRID","@value":"9000014151535"},{"@type":"NRID","@value":"9000244901697"},{"@type":"NRID","@value":"9000415345090"},{"@type":"NRID","@value":"9000334737564"},{"@type":"NRID","@value":"9000243709111"},{"@type":"NRID","@value":"9000018324808"},{"@type":"NRID","@value":"9000279645459"},{"@type":"NRID","@value":"9000333085884"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/read0138421"}],"foaf:name":[{"@value":"Shinsuke Imada"}]},{"@id":"https://cir.nii.ac.jp/crid/1380572092575653769","@type":"Researcher","foaf:name":[{"@value":"Tomoko Kawate"}]},{"@id":"https://cir.nii.ac.jp/crid/1380572092575653644","@type":"Researcher","foaf:name":[{"@value":"Kyoung-Sun Lee"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"0004637X"},{"@type":"EISSN","@value":"15384357"}],"prism:publicationName":[{"@value":"The Astrophysical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2020-11-01","prism:volume":"904","prism:number":"1","prism:startingPage":"31"},"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/abbacb/pdf"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/abbacb"}],"createdAt":"2020-11-20","modifiedAt":"2024-01-15","project":[{"@id":"https://cir.nii.ac.jp/crid/1040000781994470784","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"18H04452"},{"@type":"JGN","@value":"JP18H04452"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PUBLICLY-18H04452/"}],"notation":[{"@language":"ja","@value":"太陽フレア多波長スペクトルと地球環境への影響"}]},{"@id":"https://cir.nii.ac.jp/crid/1040848250659913472","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"20K20943"},{"@type":"JGN","@value":"JP20K20943"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-20K20943/"}],"notation":[{"@language":"ja","@value":"生命誕生時の太陽地球環境"},{"@language":"en","@value":"Solar-Terrestrial Environment at the Birth of Life"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360011146558348288","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"<title>GOES x-ray sensor and its use in predicting solar-terrestrial disturbances</title>"}]},{"@id":"https://cir.nii.ac.jp/crid/1360283692449006208","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"EVIDENCE FOR HOT FAST FLOW ABOVE A SOLAR FLARE ARCADE"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285708892265088","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Observation and numerical modeling of chromospheric evaporation during the impulsive phase of a solar flare"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285714649950592","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"IRIS, 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