NAOC Open IR
Insight-HXMT insight into switch of the accretion mode: The case of the X-ray pulsar 4U 1901+03
Tuo, Y. L.1,2; Ji, L.3; Tsygankov, S. S.4,5; Mihara, T.6; Song, L. M.1; Ge, M. Y.1; Nabizadeh, A.4; Tao, L.1; Qu, J. L.1; Zhang, Y.1,2; Zhang, S.1; Zhang, S. N.1; Bu, Q. C.1,3; Chen, L.7; Xu, Y. P.1,2; Cao, X. L.1; Chen, Y.1; Liu, C. Z.1; Cai, C.1,2; Chang, Z.1; Chen, G.1; Chen, T. X.1; Chen, Y. B.9; Chen, Y. P.1; Cui, W.8; Cui, W. W.1; Deng, J. K.9; Dong, Y. W.1; Du, Y. Y.1; Fu, M. X.9; 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.10; Kong, L. D.1,2; Li, B.1; Li, C. K.1; Li, G.1; Li, M. S.1; Li, T. P.1,2,8; 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.9; Liu, H. W.1; Liu, X. J.1; Liu, Y. N.10; Lu, B.1; Lu, F. 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; Sai, N.1,2; Shang, R. C.9; Song, X. Y.1; Sun, L.1; Tan, Y.1; Wang, C.2,11; Wang, G. F.1; Wang, J.1; Wang, W. S.1; 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, Y. J.1; Yi, Q. B.1,2; 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.1,2; Zhang, W. C.1; Zhang, W. Z.7; Zhang, Y. F.1; Zhang, Y. J.1; Zhang, Y. H.1,2; Zhang, Z.9,10; Zhang, Z. L.1; Zhao, H. S.1; Zhao, X. F.1,2; Zheng, S. J.1; Zheng, Y. G.1; Zhou, D. K.1,2; Zhou, J. F.10; Zhu, Y. X.1,2; Zhu, Y.1; Zhuang, R. L.10
2020-08-01
Source PublicationJOURNAL OF HIGH ENERGY ASTROPHYSICS
ISSN2214-4048
Volume27Pages:38-43
AbstractWe use the Insight-HXMT data collected during the 2019 outburst from X-ray pulsar 4U 1901+03 to complement the orbital parameters reported by Fermi/GBM. Using the Insight-HXMT, we examine the correlation between the derivative of the intrinsic spin frequency and bolometric flux based on accretion torque models. It was found that the pulse profiles significantly evolve during the outburst. The existence of two types of the profile's pattern discovered in the Insight-HXMT data indicates that this source experienced transition between a super-critical and a sub-critical accretion regimes during its 2019 outburst. Based on the evolution of the pulse profiles and the torque model, we derive the distance to 4U 1901+03 as 12.4 +/- 0.2 kpc. (C) 2020 Elsevier B.V. All rights reserved.
KeywordAccretion Accretion disk Pulsars: general Pulsars: individual(4U 1901+03)
Funding OrganizationChina National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Russian Science Foundation ; Russian Science Foundation ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Russian Science Foundation ; Russian Science Foundation ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Russian Science Foundation ; Russian Science Foundation ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Russian Science Foundation ; Russian Science Foundation
DOI10.1016/j.jheap.2020.03.003
WOS KeywordMAGNETIC NEUTRON-STARS ; PERIOD
Language英语
Funding ProjectChina National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST)[2016YFA0400801] ; Strategic Priority Research Program of the Chinese Academy of Sciences[XDB23040400] ; National Natural Science Foundation of China[11673023] ; National Natural Science Foundation of China[11733009] ; National Natural Science Foundation of China[U1838108] ; National Natural Science Foundation of China[U1838201] ; National Natural Science Foundation of China[U1838202] ; National Natural Science Foundation of China[U1938103] ; Russian Science Foundation[19-12-00423]
Funding OrganizationChina National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Russian Science Foundation ; Russian Science Foundation ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Russian Science Foundation ; Russian Science Foundation ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Russian Science Foundation ; Russian Science Foundation ; China National Space Administration (CNSA) ; China National Space Administration (CNSA) ; Chinese Academy of Sciences (CAS) ; Chinese Academy of Sciences (CAS) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; National Program on Key Research and Development Project from the Minister of Science and Technology of China (MOST) ; Strategic Priority Research Program of the Chinese Academy of Sciences ; Strategic Priority Research Program of the Chinese Academy of Sciences ; National Natural Science Foundation of China ; National Natural Science Foundation of China ; Russian Science Foundation ; Russian Science Foundation
WOS Research AreaAstronomy & Astrophysics
WOS SubjectAstronomy & Astrophysics
WOS IDWOS:000569885200005
PublisherELSEVIER
Citation statistics
Document Type期刊论文
Identifierhttp://ir.bao.ac.cn/handle/114a11/81307
Collection中国科学院国家天文台
Corresponding AuthorTuo, Y. L.; Song, L. M.
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.Univ Turku, Dept Phys & Astron, FI-20014 Turku, Finland
5.Russian Acad Sci, Space Res Inst, Profsoyuznaya Str 84-32, Moscow 117997, Russia
6.RIKEN, High Energy Astrophys Lab, Inst Phys & Chem Res, Wako, Saitama 3510198, Japan
7.Beijing Normal Univ, Dept Astron, Beijing 100088, Peoples R China
8.Tsinghua Univ, Dept Astron, Beijing 100084, Peoples R China
9.Tsinghua Univ, Dept Phys, Beijing 100084, Peoples R China
10.Tsinghua Univ, Dept Engn Phys, Beijing 100084, Peoples R China
11.Chinese Acad Sci, Natl Astron Observ, Key Lab Space Astron & Technol, Beijing 100012, Peoples R China
Recommended Citation
GB/T 7714
Tuo, Y. L.,Ji, L.,Tsygankov, S. S.,et al. Insight-HXMT insight into switch of the accretion mode: The case of the X-ray pulsar 4U 1901+03[J]. JOURNAL OF HIGH ENERGY ASTROPHYSICS,2020,27:38-43.
APA Tuo, Y. L..,Ji, L..,Tsygankov, S. S..,Mihara, T..,Song, L. M..,...&Zhuang, R. L..(2020).Insight-HXMT insight into switch of the accretion mode: The case of the X-ray pulsar 4U 1901+03.JOURNAL OF HIGH ENERGY ASTROPHYSICS,27,38-43.
MLA Tuo, Y. L.,et al."Insight-HXMT insight into switch of the accretion mode: The case of the X-ray pulsar 4U 1901+03".JOURNAL OF HIGH ENERGY ASTROPHYSICS 27(2020):38-43.
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