{"@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/1360004234734799488.json","@type":"Article","productIdentifier":[{"identifier":{"@type":"DOI","@value":"10.1093/pasj/psw048"}},{"identifier":{"@type":"URI","@value":"https://academic.oup.com/pasj/article-pdf/68/4/50/54680700/pasj_68_4_50.pdf"}}],"resourceType":"学術雑誌論文(journal article)","dc:title":[{"@value":"Hard-tail emission in the soft state of low-mass X-ray binaries and their relation to the neutron star magnetic field"}],"description":[{"type":"abstract","notation":[{"@value":"<jats:title>Abstract</jats:title>\n               <jats:p>Average hard-tail X-ray emission in the soft state of nine bright Atoll low-mass X-ray binaries containing a neutron star (NS-LMXBs) are investigated by using the light curves of MAXI/GSC (Gas Slit Camera) and Swift/BAT (Burst Alert Telescope). Two sources (4U 1820−30 and 4U 1735−44) exhibit a large hardness ratio (15–50 keV/2–10 keV: HR &gt;0.1), while the other sources distribute at HR ≲ 0.1. In either case, HR does not depend on the 2–10 keV luminosity. Therefore the difference of HR is due to the 15–50 keV luminosity, which is Comptonized emission. The Compton cloud is assumed to be around the neutron star. The size of the Compton cloud would affect the value of HR. Although the magnetic field of an NS-LMXB is weak, we could expect a larger Alfvén radius than the innermost stable circular orbit or the neutron star radius in some sources. In such cases, the accretion inflow is stopped at the Alfvén radius and would create a relatively large Compton cloud. This would result in the observed larger Comptonized emission. By attributing the difference of the size of Compton cloud to the Alfvén radius, we can estimate the magnetic fields of neutron stars. The obtained lower/upper limits are consistent with the previous results.</jats:p>"}]}],"creator":[{"@id":"https://cir.nii.ac.jp/crid/1380004234734799361","@type":"Researcher","foaf:name":[{"@value":"Kazumi Asai"}],"jpcoar:affiliationName":[{"@value":"MAXI team, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004234734799360","@type":"Researcher","foaf:name":[{"@value":"Tatehiro Mihara"}],"jpcoar:affiliationName":[{"@value":"MAXI team, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1380004234734799488","@type":"Researcher","foaf:name":[{"@value":"Masaru Mastuoka"}],"jpcoar:affiliationName":[{"@value":"MAXI team, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan"}]},{"@id":"https://cir.nii.ac.jp/crid/1420864424379814656","@type":"Researcher","personIdentifier":[{"@type":"KAKEN_RESEARCHERS","@value":"00469933"},{"@type":"NRID","@value":"1000000469933"},{"@type":"NRID","@value":"9000380969659"},{"@type":"NRID","@value":"9000244901376"},{"@type":"NRID","@value":"9000402479500"},{"@type":"NRID","@value":"9000257176670"},{"@type":"NRID","@value":"9000244901667"},{"@type":"NRID","@value":"9000244901809"},{"@type":"NRID","@value":"9000376939655"},{"@type":"NRID","@value":"9000388530055"}],"foaf:name":[{"@value":"Mutsumi Sugizaki"}],"jpcoar:affiliationName":[{"@value":"MAXI team, RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan"}]}],"publication":{"publicationIdentifier":[{"@type":"EISSN","@value":"2053051X"},{"@type":"PISSN","@value":"00046264"}],"prism:publicationName":[{"@value":"Publications of the Astronomical Society of Japan"}],"dc:publisher":[{"@value":"Oxford University Press (OUP)"}],"prism:publicationDate":"2016-05-31","prism:volume":"68","prism:number":"4"},"reviewed":"false","url":[{"@id":"https://academic.oup.com/pasj/article-pdf/68/4/50/54680700/pasj_68_4_50.pdf"}],"createdAt":"2016-06-02","modifiedAt":"2023-12-21","project":[{"@id":"https://cir.nii.ac.jp/crid/1040000781898907264","@type":"Project","projectIdentifier":[{"@type":"KAKEN","@value":"16H03965"},{"@type":"JGN","@value":"JP16H03965"},{"@type":"URI","@value":"https://kaken.nii.ac.jp/grant/KAKENHI-PROJECT-16H03965/"}],"notation":[{"@language":"ja","@value":"ＭＡＸＩ即時連携で解明するＭＡＸＩ未同定短時間トランジェント"},{"@language":"en","@value":"Revealing MAXI unidentified short transient by prompt 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