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Physical origin of the non-physical spin evolution of MAXI J1820+070
Guan, J.1; Tao, L.1; Qu, J. L.1,2; Zhang, S. N.1,2; Zhang, W.1,2; Zhang, S.1; Ma, R. C.1,2; Ge, M. Y.1; Song, L. M.1,2; Lu, F. J.1; Li, T. P.1,3; Xu, Y. P.1; Chen, Y.1; Cao, X. L.1; Liu, C. Z.1; Zhang, L.4; Wang, Y. N.4; Chen, Y. P.1; Bu, Q. C.1; Cai, C.1,2; Chang, Z.1; Chen, L.5; Chen, T. X.1; Chen, Y. B.3; Cui, W. W.1; Du, Y. Y.1; Gao, G. H.1,2; Gao, H.1,2; Gu, Y. D.1; Guo, C. C.1,2; Han, D. W.1; Huang, Y.1; Huo, J.1; Jia, S. M.1; Jiang, W. C.1; Jin, J.1; Kong, L. D.1; Li, B.1; Li, C. K.1; Li, G.1; Li, W.1; Li, X.1; Li, X. B.1; Li, X. F.1; Li, Z. W.1; Liang, X. H.1; Liao, J. Y.1; Liu, B. S.1; Liu, H. W.1; Liu, H. X.1; Liu, X. J.1; Lu, X. F.1; Luo, Q.1,2; Luo, T.1; Ma, X.1; Meng, B.1; Nang, Y.1,2; Nie, J. Y.1; Ou, G.1; Ren, X. Q.1,2; Sai, N.1,2; Song, X. Y.1; Sun, L.1; Tan, Y.1; Wang, C.2,6; Wang, L. J.1; Wang, P. J.1,2; Wang, W. S.1; Wang, Y. S.1; Wen, X. Y.1; Wu, B. B.1; Wu, B. Y.1,2; Wu, M.1; Xiao, G. C.1; Xiao, S.1,2; Xiong, S. L.1; Yang, R. J.7; Yang, S.1; Yang, Y. J.1; Yi, Q. B.1,2; Yin, Q. Q.1; You, Y.1; Zhang, F.1; Zhang, H. M.1; Zhang, J.1; Zhang, P.1; Zhang, W. C.1; Zhang, Y. F.1; Zhang, Y. H.1,2; Zhao, H. S.1; Zhao, X. F.1,2; Zheng, S. J.1; Zheng, Y. G.1,7; Zhou, D. K.1,2
2021-06-01
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
ISSN0035-8711
Volume504Issue:2Pages:2168-2180
AbstractWe report on the Insight-HXMT observations of the new black hole X-ray binary MAXI J1820+070 during its 2018 outburst. Detailed spectral analysis via the continuum fitting method shows an evolution of the inferred spin during its high soft sate. Moreover, the hardness ratio, the non-thermal luminosity and the reflection fraction also undergo an evolution, exactly coincident to the period when the inferred spin transition takes place. The unphysical evolution of the spin is attributed to the evolution of the inner disc, which is caused by the collapse of a hot corona due to condensation mechanism or may be related to the deceleration of a jet-like corona. The studies of the inner disc radius and the relation between the disc luminosity and the inner disc radius suggest that, only at a particular epoch, did the inner edge of the disc reach the innermost stable circular orbit and the spin measurement is reliable. We then constrain the spin of MAXI J1820 + 070 to be a(*) = 0.2(-0.3)(+0.2). Such a slowly spinning black hole possessing a strong jet suggests that its jet activity is driven mainly by the accretion disc rather than by the black hole spin.
Keywordaccretion, accretion discs black hole physics stars: individual (MAXI J1820+070) X-rays: binaries
Funding OrganizationChina National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; National Natural Science Foundation of China
DOI10.1093/mnras/stab945
WOS KeywordBLACK-HOLE SPIN ; CONTINUUM-FITTING METHOD ; X-RAY REFLECTION ; INNER-DISK ; ACCRETION DISK ; BACKGROUND MODEL ; HARD STATE ; ENERGY ; VARIABILITY ; JETS
Language英语
Funding ProjectChina National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China[2016YFA0400800] ; National Key Research and Development Program of China[2016YFA0400803] ; National Natural Science Foundation of China[U2038102] ; National Natural Science Foundation of China[U1838115] ; National Natural Science Foundation of China[U1838201] ; National Natural Science Foundation of China[11673023] ; National Natural Science Foundation of China[U1938104] ; National Natural Science Foundation of China[U1838111] ; National Natural Science Foundation of China[11473027] ; National Natural Science Foundation of China[U1838202] ; National Natural Science Foundation of China[11733009] ; National Natural Science Foundation of China[U1838104] ; National Natural Science Foundation of China[U1938101]
Funding OrganizationChina National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Key Research and Development Program of China ; National Key Research and Development Program of China ; National Natural Science Foundation of China ; National Natural Science Foundation of China
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000659453800044
PublisherOXFORD UNIV PRESS
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Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/76892
Collection中国科学院国家天文台
Corresponding AuthorGuan, J.; Tao, L.
Affiliation1.Chinese Acad Sci, Inst High Energy Phys, Key Lab Particle Astrophys, Beijing 100049, Peoples R China
2.Chinese Acad Sci, Univ Chinese Acad Sci, Beijing 100049, Peoples R China
3.Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China
4.Univ Southampton, Phys & Astron, Southampton SO17 1BJ, Hants, England
5.Beijing Normal Univ, Dept Astron, Beijing 100088, Peoples R China
6.Chinese Acad Sci, Natl Astron Observ, Key Lab Space Astron & Technol, Beijing 100012, Peoples R China
7.Hebei Univ, Coll Phys Sci & Technol, 180 Wusi Dong Rd, Baoding City 071002, Hebei, Peoples R China
Recommended Citation
GB/T 7714
Guan, J.,Tao, L.,Qu, J. L.,et al. Physical origin of the non-physical spin evolution of MAXI J1820+070[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2021,504(2):2168-2180.
APA Guan, J..,Tao, L..,Qu, J. L..,Zhang, S. N..,Zhang, W..,...&Zhou, D. K..(2021).Physical origin of the non-physical spin evolution of MAXI J1820+070.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,504(2),2168-2180.
MLA Guan, J.,et al."Physical origin of the non-physical spin evolution of MAXI J1820+070".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 504.2(2021):2168-2180.
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