{"@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/1361131415956201856.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1007/s11207-020-01602-6"}},{"identifier":{"@type":"URI","@value":"http://link.springer.com/content/pdf/10.1007/s11207-020-01602-6.pdf"}},{"identifier":{"@type":"URI","@value":"http://link.springer.com/article/10.1007/s11207-020-01602-6/fulltext.html"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.2003.02908"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Locating Hot Plasma in Small Flares using Spectroscopic Overlappogram Data from the Hinode EUV Imaging Spectrometer"}],"description":[{"notation":[{"@value":"One of the key processes associated with the \"standard\" flare model is chromospheric evaporation, a process where plasma heated to high temperatures by energy deposition at the flare footpoints is driven upwards into the corona. Despite several decades of study, a number of open questions remain, including the relationship between plasma produced during this process and observations of earlier \"superhot\" plasma. Hinode/EIS has a wide slot often used as a flare trigger in the He II emission line band. Once the intensity passes a threshold level, the study switches to one focussed on the flaring region. However, when the intensity is not high enough to reach the flare trigger threshold, these datasets are available during the entire flare period and provide high-cadence spectroscopic observations over a large field of view. We use one-minute cadence data from two such studies of a C4.7 flare and a C1.6 flare to probe the relationship between hot Fe XXIV plasma and plasmas observed by RHESSI and XRT to track where the emission comes from, and when it begins. Although the spatial and spectral information are merged in the wide-slot data, it is still possible to extract when the hot plasma appears using the Fe XXIV spectral image. It is also possible to derive spectrally pure Fe XXIV light curves from the EIS data, and compare them with those derived from hard X-rays, enabling a full exploration of the evolution of hot emission. The Fe XXIV emission peaks just after the peak in the hard X-ray lightcurve; consistent with an origin in the evaporation of heated plasma following the transfer of energy to the lower atmosphere. A peak was also found for the C4.7 flare in the RHESSI peak temperature, which occurred before the hard X-rays peaked. This suggests that the first peak in hot-plasma emission is likely directly related to the energy-release process."}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1381131415956201603","@type":"Researcher","foaf:name":[{"@value":"Louise Harra"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131415956201606","@type":"Researcher","foaf:name":[{"@value":"Sarah Matthews"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131415956201600","@type":"Researcher","foaf:name":[{"@value":"David Long"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131415956201862","@type":"Researcher","foaf:name":[{"@value":"Takahiro Hasegawa"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131415956201859","@type":"Researcher","foaf:name":[{"@value":"Kyoung-Sun Lee"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131415956201602","@type":"Researcher","foaf:name":[{"@value":"Katharine K. Reeves"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131415956201601","@type":"Researcher","foaf:name":[{"@value":"Toshifumi Shimizu"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131415956201731","@type":"Researcher","foaf:name":[{"@value":"Hirohisa Hara"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131415956201736","@type":"Researcher","foaf:name":[{"@value":"Magnus Woods"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00380938"},{"@type":"EISSN","@value":"1573093X"}],"prism:publicationName":[{"@value":"Solar Physics"}],"dc:publisher":[{"@value":"Springer Science and Business Media LLC"}],"prism:publicationDate":"2020-02","prism:volume":"295","prism:number":"2","prism:startingPage":"34"},"reviewed":"false","dc:rights":["http://www.springer.com/tdm","http://www.springer.com/tdm"],"url":[{"@id":"http://link.springer.com/content/pdf/10.1007/s11207-020-01602-6.pdf"},{"@id":"http://link.springer.com/article/10.1007/s11207-020-01602-6/fulltext.html"}],"createdAt":"2020-02-27","modifiedAt":"2021-02-26","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=Flares","dc:title":"Flares"},{"@id":"https://cir.nii.ac.jp/all?q=Corona","dc:title":"Corona"},{"@id":"https://cir.nii.ac.jp/all?q=FOS:%20Physical%20sciences","dc:title":"FOS: Physical sciences"},{"@id":"https://cir.nii.ac.jp/all?q=520","dc:title":"520"},{"@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/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 Measurements"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1360025430644951936","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Magnetic Reconnection in Solar Flares and the Near-Sun Solar Wind"}]},{"@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, Hinode, SDO, and RHESSI Observations of a White Light Flare Produced Directly by Non-thermal Electrons"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285714650456960","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Measuring Velocities in the Early Stage of an Eruption: Using “Overlappogram” Data from Hinode EIS"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292617907565696","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The X-Ray Telescope (XRT) for the Hinode Mission"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292621569840512","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Coronal-Temperature-Diagnostic Capability of the Hinode/X-Ray Telescope Based on Self-consistent Calibration. 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Calibration with On-Orbit Data"}]},{"@id":"https://cir.nii.ac.jp/crid/1360565165385289856","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Interface Region Imaging Spectrograph (IRIS)"}]},{"@id":"https://cir.nii.ac.jp/crid/1360574092890249600","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The EUV Imaging Spectrometer for Hinode"}]},{"@id":"https://cir.nii.ac.jp/crid/1360574092892862720","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI)"}]},{"@id":"https://cir.nii.ac.jp/crid/1360574094100689024","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Analysis and modelling of recurrent solar flares observed  with Hinode/EIS on March 9, 2012"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855567870980480","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Hinode (Solar-B) Mission: An Overview"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855569193452160","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"RHESSI Aspect Reconstruction"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855570062166528","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"VELOCITY CHARACTERISTICS OF EVAPORATED PLASMA USING<i>HINODE</i>/EUV IMAGING SPECTROMETER"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137046115804544","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"<i>RHESSI</i>\n                    LINE AND CONTINUUM OBSERVATIONS OF SUPER-HOT FLARE PLASMA"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418519935477504","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"STATISTICAL PROPERTIES OF SUPER-HOT SOLAR FLARES"}]},{"@id":"https://cir.nii.ac.jp/crid/1361418520576517760","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Calibrating Data from the Hinode/X-Ray Telescope and Associated Uncertainties"}]},{"@id":"https://cir.nii.ac.jp/crid/1361981468565575552","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"THE 2014 MARCH 29 X-FLARE: SUBARCSECOND RESOLUTION OBSERVATIONS OF Fe XXI λ1354.1"}]},{"@id":"https://cir.nii.ac.jp/crid/1361981469496119424","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"An Observational Overview of Solar Flares"}]},{"@id":"https://cir.nii.ac.jp/crid/1362262943649527168","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Solar Dynamics Observatory (SDO)"}]},{"@id":"https://cir.nii.ac.jp/crid/1362825895050520064","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Constraints on energy release in solar flares from RHESSI and GOES X-ray observations"}]},{"@id":"https://cir.nii.ac.jp/crid/1362825895495527808","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"SIMULTANEOUS IRIS AND HINODE/EIS OBSERVATIONS AND MODELING OF THE 2014 OCTOBER 27 X2.0 CLASS FLARE"}]},{"@id":"https://cir.nii.ac.jp/crid/1363388843654557312","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Yohkoh observations of the creation of high-temperature plasma in the flare of 16 December 1991"}]},{"@id":"https://cir.nii.ac.jp/crid/1363388845132604672","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"YOHKOH Observations of Fe XXVI X-Ray Line Emission from Solar Flares"}]},{"@id":"https://cir.nii.ac.jp/crid/1363951795561172864","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Multiple loop activations and continuous energy release in the solar flare of June 15, 1973"}]},{"@id":"https://cir.nii.ac.jp/crid/1364233269750512640","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"HARD X-RAY FOOTPOINT SIZES AND POSITIONS AS DIAGNOSTICS OF FLARE ACCELERATED ENERGETIC ELECTRONS IN THE LOW SOLAR ATMOSPHERE"}]},{"@id":"https://cir.nii.ac.jp/crid/2050588891959340160","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The first super geomagnetic storm of solar cycle 24 : \"The St. Patrick's day event (17 March 2015)\""}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.1007/s11207-020-01602-6"},{"@type":"KAKEN","@value":"PRODUCT-23421772"},{"@type":"KAKEN","@value":"PRODUCT-23121060"},{"@type":"OPENAIRE","@value":"doi_dedup___::d66c6f5094b097b90f698577cc458705"},{"@type":"CROSSREF","@value":"10.1007/s11214-025-01153-x_references_DOI_5kglrOiuigS0YZVsrrKaLTWLMsv"}]}