{"@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/1360004239673137152.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/1538-4357/836/1/111"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/836/i=1/a=111/pdf"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/836/i=1/a=111?key=crossref.769ca54e0d41d44092821f3cbbcbf7ea"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/836/1/111"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/1538-4357/836/1/111/pdf"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"X-Ray Reflection and an Exceptionally Long Thermonuclear Helium Burst from IGR J17062-6143"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>Thermonuclear X-ray bursts from accreting neutron stars power brief but strong irradiation of their surroundings, providing a unique way to study accretion physics. We analyze <jats:italic>MAXI</jats:italic>/Gas Slit Camera and <jats:italic>Swift</jats:italic>/XRT spectra of a day-long flash observed from IGR J17062-6143 in 2015. It is a rare case of recurring bursts at a low accretion luminosity of 0.15% Eddington. Spectra from <jats:italic>MAXI</jats:italic>, <jats:italic>Chandra</jats:italic>, and <jats:italic>NuSTAR</jats:italic> observations taken between the 2015 burst and the previous one in 2012 are used to determine the accretion column. We find it to be consistent with the burst ignition column of 5 × 10<jats:sup>10</jats:sup> g cm<jats:sup>−2</jats:sup>, which indicates that it is likely powered by burning in a deep helium layer. The burst flux is observed for over a day, and decays as a straight power law: <jats:italic>F</jats:italic> ∝ <jats:italic>t</jats:italic>\n                  <jats:sup>−1.15</jats:sup>. The burst and persistent spectra are well described by thermal emission from the neutron star, Comptonization of this emission in a hot optically thin medium surrounding the star, and reflection off the photoionized accretion disk. At the burst peak, the Comptonized component disappears, when the burst may dissipate the Comptonizing gas, and it returns in the burst tail. The reflection signal suggests that the inner disk is truncated at ∼10<jats:sup>2</jats:sup> gravitational radii before the burst, but may move closer to the star during the burst. At the end of the burst, the flux drops below the burst cooling trend for 2 days, before returning to the pre-burst level.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004239673137542","@type":"Researcher","foaf:name":[{"@value":"L. Keek"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239673137408","@type":"Researcher","foaf:name":[{"@value":"W. Iwakiri"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239673137410","@type":"Researcher","foaf:name":[{"@value":"M. Serino"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239673137537","@type":"Researcher","foaf:name":[{"@value":"D. R. Ballantyne"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239673137418","@type":"Researcher","foaf:name":[{"@value":"J. J. M. in’t Zand"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004239673137282","@type":"Researcher","foaf:name":[{"@value":"T. E. Strohmayer"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"0004637X"},{"@type":"EISSN","@value":"15384357"}],"prism:publicationName":[{"@value":"The Astrophysical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2017-02-10","prism:volume":"836","prism:number":"1","prism:startingPage":"111"},"reviewed":"false","dcterms:accessRights":"http://purl.org/coar/access_right/c_abf2","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/836/i=1/a=111/pdf"},{"@id":"http://stacks.iop.org/0004-637X/836/i=1/a=111?key=crossref.769ca54e0d41d44092821f3cbbcbf7ea"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/836/1/111"},{"@id":"https://iopscience.iop.org/article/10.3847/1538-4357/836/1/111/pdf"}],"createdAt":"2017-02-13","modifiedAt":"2024-01-10","project":[{"@id":"https://cir.nii.ac.jp/crid/1040282256900875520","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"16K17717"},{"@type":"JGN","@value":"JP16K17717"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16K17717/"}],"notation":[{"@language":"ja","@value":"MAXI-NICER連携で解き明かすX線スーパーバーストにおける元素合成"},{"@language":"en","@value":"Observational study of nucleosynthesis in X-ray superburst using the MAXI-NICER cooperation"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050564287772262400","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"ja","@value":"The Burst Alert Telescope (BAT) on the SWIFT Midex Mission"}]},{"@id":"https://cir.nii.ac.jp/crid/1360002217650647040","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Gas Slit Camera (GSC) onboard MAXI on ISS"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004234733678336","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"In-Orbit Performance of MAXI Gas Slit Camera (GSC) on ISS"}]},{"@id":"https://cir.nii.ac.jp/crid/1360011144105031168","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"RELATIVISTIC LINES AND REFLECTION 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