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Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity
Wang, P. J.1,2; Kong, L. D.1,2; Zhang, S.1; Chen, Y. P.1; Zhang, S. N.1,2; Qu, J. L.1,2; Ji, L.3; Tao, L.1; Ge, M. Y.1; Lu, F. J.1; Chen, L.4; Song, L. M.1,2; Li, T. P.1,2,5; Xu, Y. P.1,2; Cao, X. L.1; Chen, Y.1; Liu, C. Z.1; Bu, Q. C.1,3; Cai, C.1,2; Chang, Z.1; Chen, G.1; Chen, T. X.1; Chen, Y. B.6; Cui, W.5; Cui, W. W.1; Deng, J. K.6; Dong, Y. W.1; Du, Y. Y.1; Fu, M. X.6; Gao, G. H.1,2; Gao, H.1,2; Gao, M.1; Gu, Y. D.1; Guan, J.1; Guo, C. C.1,2; Han, D. W.1; Huang, Y.1,2; Huo, J.1; Jia, S. M.1,2; Jiang, L. H.1; Jiang, W. C.1; Jin, J.1; Jin, Y. J.7; Li, B.1; Li, C. K.1; Li, G.1; Li, M. S.1; Li, W.1; Li, X.1; Li, X. B.1; Li, X. F.1; Li, Y. G.1; Li, Z. W.1; Liang, X. H.1; Liao, J. Y.1; Liu, B. S.1; Liu, G. Q.6; Liu, H. W.1; Liu, X. J.1; Liu, Y. N.7; Lu, B.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.8; Sai, N.1,2; Shang, R. C.6; Song, X. Y.1; Sun, L.1; Tan, Y.1; Tuo, Y. L.1,2; Wang, C.2,9; Wang, G. F.1; Wang, J.1; Wang, L. J.1; Wang, W. S.10; Wang, Y. S.1; Wen, X. Y.1; Wu, B. Y.1,2; Wu, B. B.1; Wu, M.1; Xiao, G. C.1,2; Xiao, S.1,2; Xiong, S. L.1; Yang, J. W.1; Yang, S.1; Yang, Yan Ji1; Yang, Yi Jung1; Yi, Q. B.1,10; Yin, Q. Q.1; You, Y.1,2; Zhang, A. M.1; Zhang, C. M.1; Zhang, F.1; Zhang, H. M.1; Zhang, J.1; Zhang, T.1; Zhang, W. C.1; Zhang, W.1,2; Zhang, W. Z.4; Zhang, Y.1; Zhang, Y. F.1; Zhang, Y. J.1; Zhang, Y.1,2; Zhang, Zhao6; Zhang, Zhi7; Zhang, Z. L.1; Zhao, H. S.1; Zhao, X. F.1,2; Zheng, S. J.1; Zheng, Y. G.1,11; Zhou, D. K.1,2; Zhou, J. F.7; Zhu, Y. X.1,12; Zhu, Y.1; Zhuang, R. L.7
2020-10-01
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
ISSN0035-8711
Volume497Issue:4Pages:5498-5506
AbstractBased on Insight-HXMT data, we report on the pulse fraction evolution during the 2017-2018 outburst of the newly discovered first Galactic ultraluminous X-ray (ULX) source Swift J0243.6+6124. The pulse fractions of 19 observation pairs selected in the rising and fading phases with similar luminosity are investigated. The results show a general trend of the pulse fraction increasing with luminosity and energy at supercritical luminosity. However, the relative strength of the pulsation between each pair evolves strongly with luminosity. The pulse fraction in the rising phase is larger at luminosity below 7.71 x 10(38) erg s(-1), but smaller at above. A transition luminosity is found to be energy independent. Such a phenomenon is first confirmed by Insight-HXMT observations and we speculate that it may have relation with the radiation-pressure-dominated accretion disc.
Keywordstars: neutron pulsars: individual: Swift J0243.6+6124 X-rays: binaries
Funding OrganizationNational Key R&D Program of China ; National Key R&D 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 R&D Program of China ; National Key R&D 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 R&D Program of China ; National Key R&D 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 R&D Program of China ; National Key R&D 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)
DOI10.1093/mnras/staa2448
WOS KeywordX-RAY SOURCE ; ACCRETION LUMINOSITY ; COHERENT PULSATIONS ; NEUTRON-STARS ; DISCOVERY
Language英语
Funding ProjectNational Key R&D Program of China[2016YFA0400800] ; National Natural Science Foundation of China[U1838201] ; National Natural Science Foundation of China[U1838202] ; National Natural Science Foundation of China[U1938101] ; National Natural Science Foundation of China[11733009] ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS)
Funding OrganizationNational Key R&D Program of China ; National Key R&D 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 R&D Program of China ; National Key R&D 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 R&D Program of China ; National Key R&D 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 R&D Program of China ; National Key R&D 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)
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000587739300108
PublisherOXFORD UNIV PRESS
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/80685
Collection中国科学院国家天文台
Corresponding AuthorWang, P. J.; Kong, L. D.; Zhang, S.
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.Eberhard Karls Univ Tubingen, Kepler Ctr Astro & Particle Phys, Inst Astron & Astrophys, D-72076 Tubingen, Germany
4.Beijing Normal Univ, Dept Astron, Beijing 100088, Peoples R China
5.Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China
6.Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China
7.Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China
8.Hebei Univ, Coll Phys Sci & Technol, Baoding 071002, Hebei, Peoples R China
9.Xiangtan Univ, Sch Phys & Optoelect, Xiangtan 411105, Peoples R China
10.Chinese Acad Sci, Natl Astron Observ, Key Lab Space Astron & Technol, Beijing 100012, Peoples R China
11.Chinese Acad Sci, Inst High Energy Phys, Comp Div, Beijing 100049, Peoples R China
12.Jilin Univ, Coll Phys, Changchun 130012, Peoples R China
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GB/T 7714
Wang, P. J.,Kong, L. D.,Zhang, S.,et al. Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2020,497(4):5498-5506.
APA Wang, P. J..,Kong, L. D..,Zhang, S..,Chen, Y. P..,Zhang, S. N..,...&Zhuang, R. L..(2020).Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,497(4),5498-5506.
MLA Wang, P. J.,et al."Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 497.4(2020):5498-5506.
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