{"@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/1361131644404281216.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4357/ab6bc8"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/ab6bc8/pdf"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/ab6bc8"}},{"identifier":{"@type":"DOI","@value":"10.3929/ethz-b-000463462"}},{"identifier":{"@type":"HANDLE","@value":"20.500.11850/463462"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Serial Flaring in an Active Region: Exploring Why Only One Flare Is Eruptive"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>Over a four hour period between 2014 June 12–13 a series of three flares were observed within AR 12087. This sequence of flares started with a non-eruptive M-class flare, followed by a non-eruptive C-class flare, and finally ended with a second C-class flare that had an associated filament eruption. In this paper we combine spectroscopic analysis of <jats:italic>Interface Region Imaging Spectrometer</jats:italic> observations of the Si <jats:sc>iv</jats:sc> line during the three flares along with a series of nonlinear force-free field (NLFFF) extrapolations in order to investigate the conditions that lead the final flare to be eruptive. From this analysis it is found to be unlikely that the eruption was triggered by either kink instability or by tether-cutting reconnection, allowing the flux rope to rise into a region where it would be susceptible to the torus instability. The NLFFF modeling does, however, suggest that the overlying magnetic field has a fan-spine topology, raising the possibility that breakout reconnection occurring during the first two flares weakened the overlying field, allowing the flux rope to erupt in the subsequent third flare.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1381131644404281223","@type":"Researcher","foaf:name":[{"@value":"Magnus M. Woods"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131644404281219","@type":"Researcher","foaf:name":[{"@value":"Satoshi Inoue"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131644404281344","@type":"Researcher","foaf:name":[{"@value":"Louise K. Harra"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131644404281092","@type":"Researcher","foaf:name":[{"@value":"Sarah A. Matthews"}]},{"@id":"https://cir.nii.ac.jp/crid/1381131644404281346","@type":"Researcher","foaf:name":[{"@value":"Kanya Kusano"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"0004637X"},{"@type":"EISSN","@value":"15384357"}],"prism:publicationName":[{"@value":"The Astrophysical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2020-02-10","prism:volume":"890","prism:number":"1","prism:startingPage":"84"},"reviewed":"false","dc:rights":["http://creativecommons.org/licenses/by/4.0/","https://iopscience.iop.org/info/page/text-and-data-mining"],"url":[{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/ab6bc8/pdf"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/ab6bc8"}],"createdAt":"2020-02-14","modifiedAt":"2024-01-12","foaf:topic":[{"@id":"https://cir.nii.ac.jp/all?q=Solar%20physics","dc:title":"Solar physics"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20active%20region%20filaments","dc:title":"Solar active region filaments"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20flare%20spectra","dc:title":"Solar flare spectra"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20activity","dc:title":"Solar activity"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20active%20region%20magnetic%20fields","dc:title":"Solar active region magnetic fields"},{"@id":"https://cir.nii.ac.jp/all?q=520","dc:title":"520"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20active%20regions","dc:title":"Solar active regions"},{"@id":"https://cir.nii.ac.jp/all?q=Solar%20flares","dc:title":"Solar flares"}],"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"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050845763736005760","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Double Arc Instability in the Solar Corona"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011142929920000","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Helioseismic and Magnetic Imager (HMI) Vector Magnetic Field Pipeline: SHARPs – Space-Weather HMI Active Region Patches"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011142937650304","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Helioseismic and Magnetic Imager (HMI) Investigation for the Solar Dynamics Observatory (SDO)"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011142941271040","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Torus Instability"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011145337808896","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Two Episodes of Magnetic Reconnections during a Confined Circular-ribbon Flare"}]},{"@id":"https://cir.nii.ac.jp/crid/1360285714652218752","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Triggering of the 2014 March 29 Filament Eruption"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292617917560448","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO)"}]},{"@id":"https://cir.nii.ac.jp/crid/1360298754843615616","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Polarization calibration of the Tandem Etalon Magnetograph of the Solar Magnetic Activity Research Telescope at Hida Observatory"}]},{"@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/1360565165385340288","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Characteristics of Solar X-Class Flares and CMEs: A Paradigm for Stellar Superflares and Eruptions?"}]},{"@id":"https://cir.nii.ac.jp/crid/1360565167378412160","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"NONLINEAR FORCE-FREE EXTRAPOLATION OF THE CORONAL MAGNETIC FIELD BASED ON THE MAGNETOHYDRODYNAMIC RELAXATION METHOD"}]},{"@id":"https://cir.nii.ac.jp/crid/1360565170737870336","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"MAGNETIC PROPERTIES OF SOLAR ACTIVE REGIONS THAT GOVERN LARGE SOLAR FLARES AND ERUPTIONS"}]},{"@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/1360574095790804992","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A Model for Solar Coronal Mass Ejections"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855567864468480","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Hyperbolic Divergence Cleaning for the MHD Equations"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855567866467456","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Confined and Ejective Eruptions of Kink-unstable Flux Ropes"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855567870539136","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Onset of the Magnetic Explosion in Solar Flares and Coronal Mass Ejections"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855569962968064","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Filament Eruption in the 3B Flare of July 29, 1973: Onset and Magnetic Field Configuration"}]},{"@id":"https://cir.nii.ac.jp/crid/1360855570760796032","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Recurrent flares in active region NOAA 11283"}]},{"@id":"https://cir.nii.ac.jp/crid/1360861704787522048","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"An Evolution and Eruption of the Coronal Magnetic Field through a Data-driven MHD Simulation"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137045078646144","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Recurrent flare/CME events from an emerging flux region"}]},{"@id":"https://cir.nii.ac.jp/crid/1361137045769099520","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Formation and eruption of solar prominences"}]},{"@id":"https://cir.nii.ac.jp/crid/1361699994276766336","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"RELATIONSHIP BETWEEN CHROMOSPHERIC EVAPORATION AND MAGNETIC FIELD TOPOLOGY IN AN M-CLASS SOLAR FLARE"}]},{"@id":"https://cir.nii.ac.jp/crid/1361981469776823424","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Evidence for the Flare Trigger Site and Three‐Dimensional Reconnection in Multiwavelength Observations of a Solar Flare"}]},{"@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/1362262945559092352","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The Topology and Evolution of the Bastille Day Flare"}]},{"@id":"https://cir.nii.ac.jp/crid/1362544418619475072","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"FORMATION AND ERUPTION OF A SMALL FLUX ROPE IN THE CHROMOSPHERE OBSERVED BY NST,<i>IRIS</i>, AND<i>SDO</i>"}]},{"@id":"https://cir.nii.ac.jp/crid/1362544421010111360","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"THE NATURE OF FLARE RIBBONS IN CORONAL NULL-POINT TOPOLOGY"}]},{"@id":"https://cir.nii.ac.jp/crid/1362825893283630464","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Green's function methods for potential magnetic fields"}]},{"@id":"https://cir.nii.ac.jp/crid/1362825896101779712","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"COMBINED<i>STEREO/RHESSI</i>STUDY OF CORONAL MASS EJECTION ACCELERATION AND PARTICLE ACCELERATION IN SOLAR FLARES"}]},{"@id":"https://cir.nii.ac.jp/crid/1363388843633370112","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Observations and Modelling of the Pre-flare Period of the 29 March 2014 X1 Flare"}]},{"@id":"https://cir.nii.ac.jp/crid/1363388844973937920","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Evidence from the Extreme-Ultraviolet Imaging Spectrometer for Axial Filament Rotation before a Large Flare"}]},{"@id":"https://cir.nii.ac.jp/crid/1363670319315208064","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"A prototype discovery environment for analyzing and visualizing terascale turbulent fluid flow simulations"}]},{"@id":"https://cir.nii.ac.jp/crid/1363951793387115520","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Interactive desktop analysis of high resolution simulations: application to turbulent plume dynamics and current sheet formation"}]},{"@id":"https://cir.nii.ac.jp/crid/1363951794234463104","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Flare Energy Release in the Lower Solar Atmosphere near the Magnetic Field Polarity Inversion Line"}]},{"@id":"https://cir.nii.ac.jp/crid/1371131644404281101","@type":"Product","relationType":["references"]},{"@id":"https://cir.nii.ac.jp/crid/2050307416982588672","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Magnetohydrodynamics modeling of coronal magnetic field and solar eruptions based on the photospheric magnetic field"}]}],"dataSourceIdentifier":[{"@type":"CROSSREF","@value":"10.3847/1538-4357/ab6bc8"},{"@type":"KAKEN","@value":"PRODUCT-22828493"},{"@type":"OPENAIRE","@value":"doi_dedup___::729c925dd4ee8564caab1a089cd3bf2f"},{"@type":"CROSSREF","@value":"10.1093/pasj/psac072_references_DOI_8CF3JfgTzlvekJJg6Z054A6Ht5f"},{"@type":"CROSSREF","@value":"10.3847/1538-4357/ac9eaa_references_DOI_8CF3JfgTzlvekJJg6Z054A6Ht5f"}]}