{"@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/1360002217650874752.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1093/pasj/psw116"}},{"identifier":{"@type":"URI","@value":"https://academic.oup.com/pasj/article-pdf/69/1/12/54677906/pasj_69_1_12.pdf"}},{"identifier":{"@type":"DOI","@value":"10.48550/arxiv.1611.03659"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Spectroscopic observations of active solar-analog stars with high X-ray luminosity, as a proxy of superflare stars"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>Recent studies of solar-type superflare stars have suggested that even old slowly rotating stars similar to the Sun can have large starspots and superflares. We conducted high-dispersion spectroscopy of 49 nearby solar-analog stars (G-type main-sequence stars with Teff ≈ 5600–6000 K) identified as ROSAT soft X-ray sources, which are not binary stars from previous studies. We expected that these stars could be used as a proxy of bright solar-analog superflare stars, since superflare stars are expected to show strong X-ray luminosity. More than half (37) of the 49 target stars show no evidence of binarity, and their atmospheric parameters (temperature, surface gravity, and metallicity) are within the range of ordinary solar-analog stars. We measured the intensity of Ca ii 8542 and Hα lines, which are good indicators of the stellar chromospheric activity. The intensity of these lines indicates that all the target stars have large starspots. We also measured v sin i (projected rotational velocity) and lithium abundance for the target stars. Li abundance is a key to understanding the evolution of the stellar convection zone, which reflects the stellar age, mass and rotational history. We confirmed that many of the target stars rapidly rotate and have high Li abundance, compared with the Sun, as suggested by many previous studies. There are, however, also some target stars that rotate slowly (v sin i = 2–3 km s−1) and have low Li abundance like the Sun. These results support that old and slowly rotating stars similar to the Sun could have high activity levels and large starspots. This is consistent with the results of our previous studies of solar-type superflare stars. In the future, it is important to conduct long-term monitoring observations of these active solar-analog stars in order to investigate detailed properties of large starspots from the viewpoint of stellar dynamo theory.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380847870790537985","@type":"Researcher","foaf:name":[{"@value":"Yuta Notsu"}],"jpcoar:affiliationName":[{"@value":"1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1420564276171782400","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"20425408"},{"@type":"NRID","@value":"1000020425408"},{"@type":"NRID","@value":"9000248219272"},{"@type":"NRID","@value":"9000002596396"},{"@type":"NRID","@value":"9000003394539"},{"@type":"NRID","@value":"9000290358469"},{"@type":"NRID","@value":"9000244901779"},{"@type":"NRID","@value":"9000242546866"},{"@type":"NRID","@value":"9000250471627"},{"@type":"NRID","@value":"9000244901434"},{"@type":"NRID","@value":"9000016865590"},{"@type":"NRID","@value":"9000323844369"},{"@type":"NRID","@value":"9000346921244"},{"@type":"NRID","@value":"9000010083794"},{"@type":"NRID","@value":"9000002214063"},{"@type":"NRID","@value":"9000346921348"},{"@type":"NRID","@value":"9000023738902"},{"@type":"NRID","@value":"9000237870355"},{"@type":"NRID","@value":"9000315143732"},{"@type":"NRID","@value":"9000001815898"},{"@type":"NRID","@value":"9000237870896"},{"@type":"NRID","@value":"9000014152172"},{"@type":"NRID","@value":"9000250750334"},{"@type":"NRID","@value":"9000003804692"},{"@type":"NRID","@value":"9000398834551"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/hondast"}],"foaf:name":[{"@value":"Satoshi Honda"}],"jpcoar:affiliationName":[{"@value":"2Center for Astronomy, University of Hyogo, 407-2 Nishigaichi, Sayo-cho, Sayo, Hyogo 679-5313, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1420564276185218048","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"40456851"},{"@type":"NRID","@value":"1000040456851"},{"@type":"ORCID","@value":"0000-0003-0332-0811"},{"@type":"NRID","@value":"9000249538160"},{"@type":"NRID","@value":"9000323844365"},{"@type":"NRID","@value":"9000250750216"},{"@type":"NRID","@value":"9000237870922"},{"@type":"NRID","@value":"9000244902160"},{"@type":"NRID","@value":"9000310465778"},{"@type":"NRID","@value":"9000019229102"},{"@type":"NRID","@value":"9000403553662"},{"@type":"NRID","@value":"9000285477513"},{"@type":"NRID","@value":"9000399527262"},{"@type":"NRID","@value":"9000403553716"},{"@type":"NRID","@value":"9000237870991"},{"@type":"NRID","@value":"9000244901889"},{"@type":"NRID","@value":"9000253678536"},{"@type":"NRID","@value":"9000246809119"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/h.maehara"}],"foaf:name":[{"@value":"Hiroyuki Maehara"}],"jpcoar:affiliationName":[{"@value":"3Okayama Astrophysical Observatory, National Astronomical Observatory of Japan, 3037-5 Honjo, Kamogata, Asakuchi, Okayama 719-0232, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380847870790537984","@type":"Researcher","foaf:name":[{"@value":"Shota Notsu"}],"jpcoar:affiliationName":[{"@value":"1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380847870790537990","@type":"Researcher","foaf:name":[{"@value":"Kosuke Namekata"}],"jpcoar:affiliationName":[{"@value":"1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1420282801206033536","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"20332728"},{"@type":"NRID","@value":"1000020332728"},{"@type":"ORCID","@value":"0000-0001-9588-1872"},{"@type":"NRID","@value":"9000000122293"},{"@type":"NRID","@value":"9000237871111"},{"@type":"NRID","@value":"9000242546870"},{"@type":"NRID","@value":"9000237871074"},{"@type":"NRID","@value":"9000323844370"},{"@type":"NRID","@value":"9000279644560"},{"@type":"NRID","@value":"9000237871072"},{"@type":"NRID","@value":"9000237871300"},{"@type":"NRID","@value":"9000262347417"},{"@type":"NRID","@value":"9000401948763"},{"@type":"NRID","@value":"9000237871073"},{"@type":"NRID","@value":"9000000122110"},{"@type":"NRID","@value":"9000237870989"},{"@type":"NRID","@value":"9000313618294"},{"@type":"NRID","@value":"9000305623653"},{"@type":"NRID","@value":"9000290358365"},{"@type":"NRID","@value":"9000014145387"},{"@type":"NRID","@value":"9000244901817"},{"@type":"NRID","@value":"9000237871157"},{"@type":"NRID","@value":"9000275831899"},{"@type":"NRID","@value":"9000237871327"},{"@type":"NRID","@value":"9000250750332"},{"@type":"NRID","@value":"9000237871274"},{"@type":"NRID","@value":"9000237870356"},{"@type":"NRID","@value":"9000341541965"},{"@type":"NRID","@value":"9000000122412"},{"@type":"NRID","@value":"9000237871112"},{"@type":"NRID","@value":"9000237871178"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/read0069959"}],"foaf:name":[{"@value":"Daisaku Nogami"}],"jpcoar:affiliationName":[{"@value":"1Department of Astronomy, Kyoto University, Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto, Kyoto 606-8502, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1420564276176857728","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"70144178"},{"@type":"NRID","@value":"1000070144178"},{"@type":"CINII_AUTHOR_ID","@value":"DA10967417"},{"@type":"URI","@value":"https://ci.nii.ac.jp/author/DA10967417#entity"},{"@type":"URI","@value":"https://viaf.org/viaf/NII%7CDA10967417"},{"@type":"NRID","@value":"9000364778126"},{"@type":"NRID","@value":"9000297477012"},{"@type":"NRID","@value":"9000014144869"},{"@type":"NRID","@value":"9000006350908"},{"@type":"NRID","@value":"9000401948532"},{"@type":"NRID","@value":"9000346921254"},{"@type":"NRID","@value":"9000255727956"},{"@type":"NRID","@value":"9000364773944"},{"@type":"NRID","@value":"9000014152488"},{"@type":"NRID","@value":"9000310741718"},{"@type":"NRID","@value":"9000401946454"},{"@type":"NRID","@value":"9000022832447"},{"@type":"NRID","@value":"9000244901587"},{"@type":"NRID","@value":"9000000512875"},{"@type":"NRID","@value":"9000017677107"},{"@type":"NRID","@value":"9000244901876"},{"@type":"NRID","@value":"9000014143665"},{"@type":"NRID","@value":"9000014151472"},{"@type":"NRID","@value":"9000341541964"},{"@type":"NRID","@value":"9000017677126"},{"@type":"NRID","@value":"9000401948682"},{"@type":"RESEARCHMAP","@value":"https://researchmap.jp/read0049257"}],"foaf:name":[{"@value":"Kazunari Shibata"}],"jpcoar:affiliationName":[{"@value":"4Kwasan and Hida Observatories, Kyoto University, 17 Ohmine-cho Kita Kazan, Yamashina-ku, Kyoto, Kyoto 607-8471, Japan"}]}],"publication":{"publicationIdentifier":[{"@type":"PISSN","@value":"00046264"},{"@type":"EISSN","@value":"2053051X"}],"prism:publicationName":[{"@value":"Publications of the Astronomical Society of Japan"}],"dc:publisher":[{"@value":"Oxford University Press (OUP)"}],"prism:publicationDate":"2017-01-24","prism:volume":"69","prism:number":"1","prism:startingPage":"12"},"reviewed":"false","url":[{"@id":"https://academic.oup.com/pasj/article-pdf/69/1/12/54677906/pasj_69_1_12.pdf"}],"createdAt":"2016-11-17","modifiedAt":"2023-12-21","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/1040000781898888704","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"16H03955"},{"@type":"JGN","@value":"JP16H03955"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16H03955/"}],"notation":[{"@language":"ja","@value":"太陽白色光フレアの解析に基づく、スーパーフレア星の磁気活動機構の解明"},{"@language":"en","@value":"Solving the Mechanism of Magnetic Activity of Supeflare Stars based on the Analysis of White Light Solar Flares"}]},{"@id":"https://cir.nii.ac.jp/crid/1040000781905215488","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"16J06887"},{"@type":"JGN","@value":"JP16J06887"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16J06887/"}],"notation":[{"@language":"ja","@value":"原始惑星系円盤・系外惑星大気の化学構造研究から迫る、普遍的な惑星形成理論"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282256880745984","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"16J00320"},{"@type":"JGN","@value":"JP16J00320"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16J00320/"}],"notation":[{"@language":"ja","@value":"スーパーフレア星の観測から迫る、太陽型恒星の磁気活動とダイナモ理論"},{"@language":"en","@value":"Magnetic activities of solar-type stars and dynamo theory investigated through the observations of superflare stars"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282257274126976","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"26400231"},{"@type":"JGN","@value":"JP26400231"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-26400231/"}],"notation":[{"@language":"ja","@value":"スーパーフレア星の化学組成から探る元素合成の研究"},{"@language":"en","@value":"Nucleosynthesis studies from the chmical abundances of superflare stars"}]},{"@id":"https://cir.nii.ac.jp/crid/1040282257293082624","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"26800096"},{"@type":"JGN","@value":"JP26800096"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-26800096/"}],"notation":[{"@language":"ja","@value":"広視野測光サーベイとアーカイブデータの活用による活動的な太陽型星の探査"},{"@language":"en","@value":"Survey of active solar-type stars with the wide-filed photometric observations and archival data"}]}],"relatedProduct":[{"@id":"https://cir.nii.ac.jp/crid/1050282810809482624","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Statistical properties of superflares on solar-type stars based on 1-min cadence data"}]},{"@id":"https://cir.nii.ac.jp/crid/1050578283037622656","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["isReferencedBy"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Self-Consistent Picture of the Mass Ejection from a One Second Long Binary Neutron Star Merger Leaving a Short-Lived Remnant in a General-Relativistic Neutrino-Radiation Magnetohydrodynamic Simulation"}]},{"@id":"https://cir.nii.ac.jp/crid/1050856893077653760","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@language":"en","@value":"Coalescence of black hole–neutron star binaries"},{"@value":"Solar flares: 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XI - A survey of CA II lambda 8542 line profiles in late-type stars of differing chromospheric activity"}]},{"@id":"https://cir.nii.ac.jp/crid/1360292621040297088","@type":"Article","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"Lithium abundances of nearby young solar-type stars based on optical high-resolution spectroscopy"}]},{"@id":"https://cir.nii.ac.jp/crid/1360565167604188672","@type":"Article","resourceType":"学術雑誌論文(journal article)","relationType":["references"],"jpcoar:relatedTitle":[{"@value":"High dispersion spectroscopy of solar-type superflare stars. II. 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