Timing analysis of 2S 1417-624 observed with NICER and insight-HXMT

Ji, L. and Doroshenko, V. and Santangelo, A. and Güngör, Can and Zhang, S. and Ducci, L. and Zhang, S. N. and Ge, M. Y. and Qu, L. J. and Chen, Y. P. and Bu, Q. C. and Cai, C. and Cao, X. L. and Chang, Z. and Chen, G. and Chen, L. and Chen, T. X. and Chen, Y. and Chen, Y. B. and Cui, W. and Cui, W. W. and deng, J. K. and Dong, Y. W. and Du, Y. Y. and Fu, M. X. and Gao, G. H. and Gao, H. and Gao, M. and Gu, Y. D. and Guan, J. and Guo, C. C. and Han, D. W. and Huang, Y. and Huo, J. and Jia, S. M. and Jiang, L. H. and Jiang, W. C. and Jin, J. and Kong, L. D. and Li, B. and Li, C. K. and Li, G. and Li, M. S. and Li, T. P. and Li, W. and Li, X. and Li, X. B. and Li, X. F. and Li, Y. G. and Li, Z. W. and Liang, X. H. and Liao, J. Y. and Liu, C. Z. and Liu, G. Q. and Liu, H. W. and Liu, X. J. and Liu, Y. N. and Lu, B. and Lu, F. J. and Lu, X. F. and Luo, Q. and Luo, T. and Ma, X. and Meng, B. and Nang, Y. and Nie, J. Y. and Ou, G. and Sai, N. and Song, L. M. and Song, X. Y. and Sun, L. and Tan, Y. and Tao, L. and Tuo, Y. L. and Wang, C. and Wang, G. F. and Wang, J. and Wang, W. S. and Wang, Y. S. and Wen, X. Y. and Wu, B. B. and Wu, B. Y. and Wu, M. and Xiao, G. C. and Xiao, S. and Xiong, S. L. and Xu, Y. P. and Yang, Y. J. and Yang, J. W. and Yang, S. and Yang, Y. J. and Yi, Q. B. and Yin, Q. Q. and You, Y. and Zhang, A. M. and Zhang, C. M. and Zhang, F. and Zhang, H. M. and Zhang, J. and Zhang, T. and Zhang, W. and Zhang, W. C. and Zhang, W. Z. and Zhang, Y. and Zhang, Y. and Zhang, Y. F. and Zhang, Y. J. and Zhang, Z. and Zhang, Z. L. and Zhao, H. S. and Zhao, X. F. and Zheng, S. J. and Zhou, D. K. and Zhou, J. F. and Zhu, Y. and Zhu, Y. X. (2020) Timing analysis of 2S 1417-624 observed with NICER and insight-HXMT. Monthly Notices of the Royal Astronomical Society, 491 (2). pp. 1851-1856. ISSN 0035-8711 (Print) 1365-2966 (Online)

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We present a study of timing properties of the accreting pulsar 2S 1417-624 observed during its 2018 outburst, based on Swift/BAT, Fermi/GBM, Insight-HXMT, and NICER observations. We report a dramatic change of the pulse profiles with luminosity. The morphology of the profile in the range 0.2-10.0 keV switches from double to triple peaks at ∼2.5 × 1037D 210 erg s-1and from triple to quadruple peaks at ∼7×1037D 210 erg s-1. The profile at high energies (25-100 keV) shows significant evolutions as well. We explain this phenomenon according to existing theoretical models. We argue that the first change is related to the transition from the sub to the supercritical accretion regime, while the second to the transition of the accretion disc from the gas-dominated to the radiation pressure-dominated state. Considering the spin-up as well due to the accretion torque, this interpretation allows to estimate the magnetic field self-consistently at ∼7 × 1012 G.
Item Type: Article
Uncontrolled Keywords: Stars: magnetic field; Stars: neutron; X-rays: binaries; X-rays: individual: 2S 1417-624
Divisions: Faculty of Engineering and Natural Sciences
Depositing User: Can Güngör
Date Deposited: 31 Jul 2023 21:34
Last Modified: 31 Jul 2023 21:34
URI: https://research.sabanciuniv.edu/id/eprint/46682

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