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Physical origin of the non-physical spin evolution of MAXI J1820 + 070
Guan, J.; Tao, L.; Qu, J. L.; Zhang, S. N.; Zhang, W.; Zhang, S.; Ma, R. C.; Ge, M. Y.; Song, L. M.; Lu, F. J.; Li, T. P.; Xu, Y. P.; Chen, Y.; Cao, X. L.; Liu, C. Z.; Zhang, L.; Wang, Y. N.; Chen, Y. P.; Bu, Q. C.; Cai, C.; Chang, Z.; Chen, L.; Chen, T. X.; Chen, Y. B.; Cui, W. W.; Du, Y. Y.; Gao, G. H.; Gao, H.; Gu, Y. D.; Guo, C. C.; Han, D. W.; Huang, Y.; Huo, J.; Jia, S. M.; Jiang, W. C.; Jin, J.; Kong, L. D.; Li, B.; Li, C. K.; Li, G.; Li, W.; Li, X.; Li, X. B.; Li, X. F.; Li, Z. W.; Liang, X. H.; Liao, J. Y.; Liu, B. S.; Liu, H. W.; Liu, H. X.; Liu, X. J.; Lu, X. F.; Luo, Q.; Luo, T.; Ma, X.; Meng, B.; Nang, Y.; Nie, J. Y.; Ou, G.; Ren, X. Q.; Sai, N.; Song, X. Y.; Sun, L.; Tan, Y.; Wang, C.; Wang, L. J.; Wang, P. J.; Wang, W. S.; Wang, Y. S.; Wen, X. Y.; Wu, B. B.; Wu, B. Y.; Wu, M.; Xiao, G. C.; Xiao, S.; Xiong, S. L.; Yang, R. J.; Yang, S.; Yang, Y. J.; Yang, Y. J.; Yi, Q. B.; Yin, Q. Q.; You, Y.; Zhang, F.; Zhang, H. M.; Zhang, J.; Zhang, P.; Zhang, W. C.; Zhang, Y. F.; Zhang, Y. H.; Zhao, H. S.; Zhao, X. F.; Zheng, S. J.; Zheng, Y. G.; Zhou, D. K.
2021
Source PublicationMonthly Notices of the Royal Astronomical Society
ISSN0035-8711
Volume504Pages:2168
SubtypeJournal Article
Abstract

We 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 Astrophysics - High Energy Astrophysical Phenomena 83C57
DOI10.1093/mnras/stab945
WOS IDWOS:000659453800044
ADS Bibcode2021MNRAS.504.2168G
ADS URLhttps://ui.adsabs.harvard.edu/abs/2021MNRAS.504.2168G
Citation statistics
Cited Times:12 [ADS]
Document Type期刊论文
Identifierhttp://ir.ihep.ac.cn/handle/311005/289767
Collection粒子天体物理中心
硬X射线调制望远镜卫星
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,2021,504:2168.
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,504,2168.
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(2021):2168.
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