| Autor: |
Ju Guan, Yuan-Hang Zhang, Wei Zhang, Yue Zhang, W. C. Jiang, Y. G. Zheng, Cheng-Cheng Guo, Cheng-Kui Li, R. C. Shang, W. S. Wang, Shaolin Xiong, GuoQing Liu, Yongwei Dong, Tian-Xiang Chen, Yupeng Xu, Jian-Feng Zhou, Yu-Dong Gu, Qian-Qing Yin, Wei Li, Jianyin Nie, Wei Cui, X. L. Cao, Qingcui Bu, Yongjie Zhang, J. W. Yang, Jing-Yuan Liao, XiangYang Wen, Xiang Ma, Bing Li, Wen-Zhao Zhang, B. B. Wu, Tong Zhang, Zhao Zhang, Lian Tao, X. Y. Song, Zheng-Wei Li, Jing Jin, Zhi Chang, Mao-Shun Li, Yue Zhu, Jia Huo, Wei-Wei Cui, Xian Li, Hongwei Liu, Y. G. Li, Sheng Yang, Bo Lu, ShiJie Zheng, Jin-Lu Qu, H. W. Liu, Da-Wei Han, Wan-Chang Zhang, C. Cai, HongMei Zhang, Gang Li, Luhua Jiang, Yuan-Yuan Du, Min-Xue Fu, Yue Huang, He Xu, Juan Zhang, Xiaobo Li, Min Gao, Shuang-Nan Zhang, Zhi Zhang, Yu-Sa Wang, Li-Ming Song, Xufang Li, Liang Sun, Aimei Zhang, Tao Luo, Yu-Peng Chen, S. Xiao, Fangjun Lu, Li Chen, Shu Zhang, Guan-Hua Gao, Xiao-Fan Zhao, Ling-Jun Wang, N. Sai, He Gao, Q. Luo, Yifei Zhang, Bin Meng, Fan Zhang, Y. P. Chen, Mei Wu, Yu-Xuan Zhu, B. S. Liu, D. K. Zhou, Shu-Mei Jia, Ming-Yu Ge, Xiao-Jing Liu, Juan Wang, Xue-Feng Lu, Ge Ou, Chengmo Zhang, R. L. Zhuang, Hai-Sheng Zhao, C. X. Liu, Gang Chen, Yong Chen, Y. N. Liu, Y. Nang, Guang-Cheng Xiao, G. F. Wang, Jing-Kang Deng, Xiaohua Liang, Yuan You, Youli Tuo, Qi-Bin Yi, Bobing Wu, Ti-Pei Li, Y. J. Yang, Ying Tan, Zi-Liang Zhang, YongJie Jin, Yanji Yang, Yi Zhang, L. D. Kong, Chen Wang |
| Jazyk: |
angličtina |
| Rok vydání: |
2020 |
| Předmět: |
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| Popis: |
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. |
| Databáze: |
OpenAIRE |
| Externí odkaz: |
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