학술논문
Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity
Document Type
Working Paper
Author
Wang, P. J.; Kong, L. D.; Zhang, S.; Chen, Y. P.; Zhang, S. N.; Qu, J. L.; Ji, L.; Tao, L.; Ge, M. Y.; Lu, F. J.; Chen, L.; Song, L. M.; Li, T. P.; Xu, Y. P.; Cao, X. L.; Chen, Y.; Liu, C. Z.; Bu, Q. C.; Cai, C.; Chang, Z.; Chen, G.; Chen, T. X.; Chen, Y. B.; Cui, W.; Cui, W. W.; Deng, J. K.; Dong, Y. W.; Du, Y. Y.; Fu, M. X.; Gao, G. H.; Gao, H.; Gao, M.; Gu, Y. D.; Guan, J.; Guo, C. C.; Han, D. W.; Huang, Y.; Huo, J.; Jia, S. M.; Jiang, L. H.; Jiang, W. C.; Jin, J.; Jin, Y. J.; Li, B.; Li, C. K.; Li, G.; Li, M. S.; Li, W.; Li, X.; Li, X. B.; Li, X. F.; Li, Y. G.; Li, Z. W.; Liang, X. H.; Liao, J. Y.; Liu, B. S.; Liu, G. Q.; Liu, H. W.; Liu, X. J.; Liu, Y. N.; Lu, B.; Lu, X. F.; Luo, Q.; Luo, T.; Ma, X.; Meng, B.; Nang, Y.; Nie, J. Y.; Ou, G.; Sai, N.; Shang, R. C.; Song, X. Y.; Sun, L.; Tan, Y.; Tuo, Y. L.; Wang, C.; Wang, G. F.; Wang, J.; Wang, L. J.; Wang, W. S.; Wang, Y. S.; Wen, X. Y.; Wu, B. Y.; Wu, B. B.; Wu, M.; Xiao, G. C.; Xiao, S.; Xiong, S. L.; Yang, J. W.; Yang, S.; Yang, Yan Ji; Yang, Yi Jung; Yi, Q. B.; Yin, Q. Q.; You, Y.; Zhang, A. M.; Zhang, C. M.; Zhang, F.; Zhang, H. M.; Zhang, J.; Zhang, T.; Zhang, W. C.; Zhang, W.; Zhang, W. Z.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. J.; Zhang, Zhao; Zhang, Zhi; Zhang, Z. L.; Zhao, H. S.; Zhao, X. F.; Zheng, S. J.; Zheng, Y. G.; Zhou, D. K.; Zhou, J. F.; Zhu, Y. X.; Zhu, Y.; Zhuang, R. L.
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Abstract
Based 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 source (ULX) 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 super-critical 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 $7.71\times10^{38}$~erg~s$^{-1}$, but smaller at above. A transition luminosity is found to be energy independent. Such a phenomena is firstly confirmed by Insight-HXMT observations and we speculate it may have relation with the radiation pressure dominated accretion disk.