Vol 21, No 3 (2021) / Liu

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Timing analysis of the black hole candidate EXO 1846–031 with Insight-HXMT monitoring

He-Xin Liu, Yue Huang, Guang-Cheng Xiao, Qing-Cui Bu, Jin-Lu Qu, Shu Zhang, Shuang-Nan Zhang, Shu-Mei Jia, Fang-Jun Lu, Xiang Ma, Lian Tao, Wei Zhang, Li Chen, Li-Ming Song, Ti-Pei Li, Yu-Peng Xu, Xue-Lei Cao, Yong Chen, Cong-Zhan Liu, Ce Cai, Zhi Chang, Gang Chen, Tian-Xiang Chen, Yi-Bao Chen, Yu-Peng Chen, Wei Cui, Wei-Wei Cui, Jing-Kang Deng, Yong-Wei Dong, Yuan-Yuan Du, Min-Xue Fu, Guan-Hua Gao, He Gao, Min Gao, Ming-Yu Ge, Yu-Dong Gu, Ju Guan, Cheng-Cheng Guo, Da-Wei Han, Jia Huo, Lu-Hua Jiang, Wei-Chun Jiang, Jing Jin, Yong-Jie Jin, Ling-Da Kong, Bing Li, Cheng-Kui Li, Gang Li, Mao-Shun Li, Wei Li, Xian Li, Xiao-Bo Li, Xu-Fang Li, Yang-Guo Li, Zheng-Wei Li, Xiao-Hua Liang, Jing-Yuan Liao, Bai-Sheng Liu, Guo-Qing Liu, Hong-Wei Liu, Xiao-Jing Liu, Yi-Nong Liu, Bo Lu, Xue-Feng Lu, Qi Luo, Tao Luo, Bin Meng, Yi Nang, Jian-Yin Nie, Ge Ou, Na Sai, Ren-Cheng Shang, Xin-Ying Song, Liang Sun, Ying Tan, You-Li Tuo, Chen Wang, Juan Wang, Ling-Jun Wang, Weng-Shuai Wang, Yu-Sa. Wang, Xiang-Yang Wen, Bai-Yang Wu, Bo-Bing Wu, Mei Wu, Shuo Xiao, Shao-Lin Xiong, He Xu, Jia-Wei Yang, Sheng Yang, Yan-Ji Yang, Yi-Jung Yang, Qi-Bin Yi, Qian-Qing Yin, Yuan You, Ai-Mei Zhang, Cheng-Mo Zhang, Fan Zhang, Hong-Mei Zhang, Juan Zhang, Tong Zhang, Wan-Chang Zhang, Wen-Zhao Zhang, Yi Zhang, Yi-Fei Zhang, Yong-Jie Zhang, Yuan-Hang Zhang, Yue Zhang, Zhao Zhang, Zhi Zhang, Zi-Liang Zhang, Hai-Sheng Zhao, Xiao-Fan Zhao, Shi-Jie Zheng, Yao-Guang Zheng, Deng-Ke Zhou, Jian-Feng Zhou, Yu-Xuan Zhu, Ren-Lin Zhuang, Yue Zhu

Abstract

We present the observational results from a detailed timing analysis of the black hole candidate EXO 1846–031 during its outburst in 2019 with the observations of Insight-HXMT, NICER and MAXI. This outburst can be classified roughly into four different states. Type-C quasi-periodic oscillations (QPOs) observed by NICER (about 0.1–6 Hz) and Insight-HXMT (about 0.7–8 Hz) are also reported in this work. Meanwhile, we study various physical quantities related to QPO frequency. The QPO rms–frequency relationship in the energy band 1–10 keV indicates that there is a turning pointing in frequency around 2 Hz, which is similar to that of GRS 1915+105. A possible hypothesis for the relationship above may be related to the inclination of the source, which may require a high inclination to explain it. The relationships between QPO frequency and QPO rms, hardness, total fractional rms and count rate have also been found in other transient sources, which can indicate that the origin of type–C QPOs is non-thermal.

Keywords


X-ray binaries — black hole candidate — QPO — EXO 1846–031

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DOI: https://doi.org/10.1088/1674-4527/21/3/70

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