Characteristics of the High-frequency Humps in the Black hole X-ray Binary Swift J1727.8--1613
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| Main Authors: | , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2026
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| _version_ | 1866914348114378752 |
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| author | Li, Ze-Xi Zhang, Liang Tao, Lian Yang, Zi-Han Zhao, Qing-Chang Zhao, Shu-Jie Ma, Rui-Can Yang, Zi-Xu Li, Pan-Ping Ma, Xiang Huang, Yue Jia, Shu-Mei Zhang, Shuang-Nan Feng, Hua Qu, Jin-Lu Zhang, Shu |
| author_facet | Li, Ze-Xi Zhang, Liang Tao, Lian Yang, Zi-Han Zhao, Qing-Chang Zhao, Shu-Jie Ma, Rui-Can Yang, Zi-Xu Li, Pan-Ping Ma, Xiang Huang, Yue Jia, Shu-Mei Zhang, Shuang-Nan Feng, Hua Qu, Jin-Lu Zhang, Shu |
| contents | We present a detailed timing analysis of the two high-frequency humps observed in the power density spectrum of Swift J1727.8--1613 up to 100 keV, using data from the Hard X-ray Modulation Telescope (Insight-HXMT). Our analysis reveals that the characteristic frequencies of the humps increase with energy up to $\sim30$ keV, followed by a plateau at higher energies. The fractional rms amplitudes of the humps increase with energy, reaching approximately 15\% in the 50-100 keV band. The lag spectrum of the hump is characterized primarily by a soft lag that varies with energy. Our results suggest that the high-frequency humps originate from a corona close to the black hole. Additionally, by applying the relativistic precession model, we constrain the mass of Swift J1727.8--1613 to $2.84 < M / M_{\odot} < 120.01$ and the spin to $0.14 < a < 0.43$ from the full-energy band dataset, using triplets composed of a type-C quasi-periodic oscillation and two high-frequency humps. When considering only the high-energy bands with stable characteristic frequencies, we derive additional constraints of $2.84 < M/M_{\odot} < 13.98$ and $0.14 < a < 0.40$. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2601_03696 |
| institution | arXiv |
| publishDate | 2026 |
| record_format | arxiv |
| spellingShingle | Characteristics of the High-frequency Humps in the Black hole X-ray Binary Swift J1727.8--1613 Li, Ze-Xi Zhang, Liang Tao, Lian Yang, Zi-Han Zhao, Qing-Chang Zhao, Shu-Jie Ma, Rui-Can Yang, Zi-Xu Li, Pan-Ping Ma, Xiang Huang, Yue Jia, Shu-Mei Zhang, Shuang-Nan Feng, Hua Qu, Jin-Lu Zhang, Shu High Energy Astrophysical Phenomena We present a detailed timing analysis of the two high-frequency humps observed in the power density spectrum of Swift J1727.8--1613 up to 100 keV, using data from the Hard X-ray Modulation Telescope (Insight-HXMT). Our analysis reveals that the characteristic frequencies of the humps increase with energy up to $\sim30$ keV, followed by a plateau at higher energies. The fractional rms amplitudes of the humps increase with energy, reaching approximately 15\% in the 50-100 keV band. The lag spectrum of the hump is characterized primarily by a soft lag that varies with energy. Our results suggest that the high-frequency humps originate from a corona close to the black hole. Additionally, by applying the relativistic precession model, we constrain the mass of Swift J1727.8--1613 to $2.84 < M / M_{\odot} < 120.01$ and the spin to $0.14 < a < 0.43$ from the full-energy band dataset, using triplets composed of a type-C quasi-periodic oscillation and two high-frequency humps. When considering only the high-energy bands with stable characteristic frequencies, we derive additional constraints of $2.84 < M/M_{\odot} < 13.98$ and $0.14 < a < 0.40$. |
| title | Characteristics of the High-frequency Humps in the Black hole X-ray Binary Swift J1727.8--1613 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2601.03696 |