학술논문
GECAM detection of a bright type-I X-ray burst from 4U 0614+09: confirmation its spin frequency at 413 Hz
Document Type
Working Paper
Author
Chen, Y. P.; Li, J.; Xiong, S. L.; Ji, L.; Zhang, S.; Peng, W. X.; Qiao, R.; Li, X. Q.; Wen, X. Y.; Song, L. M.; Zheng, S. J.; Song, X. Y.; Zhao, X. Y.; Huang, Y.; Lu, F. J.; Zhang, S. N.; Xiao, S.; Cai, C.; Zhang, B. X.; An, Z. H.; Chen, C.; Chen, G.; Chen, W.; Dai, G. Q.; Du, Y. Q.; Gao, M.; Gong, K.; Guo, D. Y.; Guo, Z. W.; He, J. J.; Li, B.; Li, C.; Li, C. Y.; Li, G.; Li, J. H.; Li, L.; Li, Q. X.; Li, X. B.; Li, Y. G.; Liang, J.; Liang, X. H.; Liao, J. Y.; Liu, J. C.; Liu, X. J.; Liu, Y. Q.; Luo, Q.; Ma, X.; Meng, B.; Ou, G.; Shi, D. L.; Shi, F.; Shi, J. Y.; Sun, G. X.; Sun, X. L.; Tuo, Y. L.; Wang, C. W.; Wang, H.; Wang, H. Y.; Wang, J.; Wang, J. Z.; Wang, P.; Wang, Y. S.; Wang, Y. X.; Wen, X.; Wu, H.; Xie, S. L.; Xu, Y. B.; Xu, Y. P.; Xue, W. C.; Yang, S.; Yao, M.; Ye, J. Y.; Yi, Q. B.; Zhang, C. M.; Zhang, C. Y.; Zhang, D. L.; Zhang, Fan; Zhang, Fei; Zhang, H. M.; Zhang, K.; Zhang, P.; Zhang, X. L.; Zhang, Y. Q.; Zhang, Z.; Zhao, G. Y.; Zhao, S. Y.; Zhao, Y.; Zheng, C.; Zhou, X.; Zhu, Y.
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Abstract
One month after launching Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM), a bright thermonuclear X-ray burst from 4U~0614+09, was observed on January 24, 2021. We report the time-resolved spectroscopy of the burst and a burst oscillation detection at 413 Hz with a fractional amplitude 3.4\% (rms). This coincides with the burst oscillation previously discovered with \textit{Swift}/BAT \citep{Strohmayer2008}, and therefore confirms the spin frequency of this source. This burst is the brightest one in the normal bursts (except the superburst) ever detected from 4U~0614+09, which leads to an upper limit of distance estimation as 3.1 kpc. The folded light curve during the burst oscillation shows a multi-peak structure, which is the first case observed during a single burst oscillation in nonpulsating sources. The multi-peak profile could be due to additional harmonics of the burst oscillation, which is corresponding to several brighter/fainter spots at the stellar surface.