{"@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/1360848664600611968.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.3847/0004-637x/816/2/91"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/816/i=2/a=91/pdf"}},{"identifier":{"@type":"URI","@value":"http://stacks.iop.org/0004-637X/816/i=2/a=91?key=crossref.45c2bde7d86507d9b512491636197e78"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/0004-637X/816/2/91"}},{"identifier":{"@type":"URI","@value":"https://iopscience.iop.org/article/10.3847/0004-637X/816/2/91/pdf"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1511.08991"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"CHROMOSPHERIC SUNSPOTS IN THE MILLIMETER RANGE AS OBSERVED BY THE NOBEYAMA RADIOHELIOGRAPH"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>ABSTRACT</jats:title>\n               <jats:p>We investigate the upper chromosphere and the transition region of the sunspot umbra using the radio brightness temperature at 34 GHz (corresponding to 8.8 mm observations) as observed by the Nobeyama Radioheliograph (NoRH). Radio free–free emission in the longer millimeter range is generated around the transition region, and its brightness temperature yields the region's temperature and density distribution. We use the NoRH data at 34 GHz by applying the Steer-CLEAN image synthesis. These data and the analysis method enable us to investigate the chromospheric structures in the longer millimeter range with high spatial resolution and sufficient visibilities. We also perform simultaneous observations of one sunspot using the NoRH and the Nobeyama 45 m telescope operating at 115 GHz. We determine that 115 GHz emission mainly originates from the lower chromosphere while 34 GHz emission mainly originates from the upper chromosphere and transition region. These observational results are consistent with the radio emission characteristics estimated from current atmospheric models of the chromosphere. On the other hand, the observed brightness temperature of the umbral region is almost the same as that of the quiet region. This result is inconsistent with current sunspot models, which predict a considerably higher brightness temperature of the sunspot umbra at 34 GHz. This inconsistency suggests that the temperature of the region at which the 34 GHz radio emission becomes optically thick should be lower than that predicted by the models.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380848664600611972","@type":"Researcher","foaf:name":[{"@value":"Kazumasa Iwai"}]},{"@id":"https://cir.nii.ac.jp/crid/1380848664600611968","@type":"Researcher","foaf:name":[{"@value":"Hideki Koshiishi"}]},{"@id":"https://cir.nii.ac.jp/crid/1380848664600611970","@type":"Researcher","foaf:name":[{"@value":"Kiyoto Shibasaki"}]},{"@id":"https://cir.nii.ac.jp/crid/1380848664600611840","@type":"Researcher","foaf:name":[{"@value":"Satoshi Nozawa"}]},{"@id":"https://cir.nii.ac.jp/crid/1380848664600612096","@type":"Researcher","foaf:name":[{"@value":"Shun Miyawaki"}]},{"@id":"https://cir.nii.ac.jp/crid/1380848664600611971","@type":"Researcher","foaf:name":[{"@value":"Takuro Yoneya"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"0004637X"},{"@type":"EISSN","@value":"15384357"}],"prism:publicationName":[{"@value":"The Astrophysical Journal"}],"dc:publisher":[{"@value":"American Astronomical Society"}],"prism:publicationDate":"2016-01-10","prism:volume":"816","prism:number":"2","prism:startingPage":"91"},"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/816/i=2/a=91/pdf"},{"@id":"http://stacks.iop.org/0004-637X/816/i=2/a=91?key=crossref.45c2bde7d86507d9b512491636197e78"},{"@id":"https://iopscience.iop.org/article/10.3847/0004-637X/816/2/91"},{"@id":"https://iopscience.iop.org/article/10.3847/0004-637X/816/2/91/pdf"}],"createdAt":"2016-01-15","modifiedAt":"2024-01-09","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/1040282256813933568","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"15J09524"},{"@type":"JGN","@value":"JP15J09524"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-15J09524/"}],"notation":[{"@language":"ja","@value":"電波観測を用いたリアルタイム宇宙天気予報システムの構築"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050001338805863936","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"ALMA Discovery of Solar Umbral Brightness Enhancement at λ=3mm"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004231434523520","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"The Brightness Temperature of the Quiet Solar Chromosphere at 2.6 mm"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004233713225344","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"First analysis of solar structures in 1.21 mm full-disc ALMA image of the Sun"}]},{"@id":"https://cir.nii.ac.jp/crid/1360004239674359040","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@value":"Solar ALMA Observations: Constraining the Chromosphere above Sunspots"}]},{"@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/1360292618916212608","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Solar atmospheric model with spicules  applied to radio observation"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292619590428288","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Semiempirical Models of Solar Magnetic Structures"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292620517166976","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Soft X‐Ray and Gyroresonance Emission above Sunspots"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292621429560448","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"The center-to-limb brightness variation of the sun at lambda = 850 microns"}]},{"@id":"https://cir.nii.ac.jp/crid/1360565165385260032","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Hinode Flare Catalogue"}]},{"@id":"https://cir.nii.ac.jp/crid/1360574093692727680","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Structure of the solar chromosphere. 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