Insight-HXMT observations of thermonuclear X-ray bursts in 4U 1636-53
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| Main Authors: | , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866913202337480704 |
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| author | Yan, Zhe Zhang, Guobao Chen, Yu-Peng Zhang, Shu Méndez, Mariano Peng, Jingqiang Zhang, Shuang-Nan Qu, Jinlu Lyu, Ming Mao, Jirong Ge, Mingyu Wang, Jiancheng |
| author_facet | Yan, Zhe Zhang, Guobao Chen, Yu-Peng Zhang, Shu Méndez, Mariano Peng, Jingqiang Zhang, Shuang-Nan Qu, Jinlu Lyu, Ming Mao, Jirong Ge, Mingyu Wang, Jiancheng |
| contents | We conducted an analysis of 45 bursts observed from 4U 1636$-$53. To investigate the mechanism behind the light curve profiles and the impact of thermonuclear X-ray bursts on the accretion environment in accreting neutron star low-mass X-ray binaries. This analysis employed both light curve and time-resolved spectroscopy methodologies, with data collected by the \textit{Insight}-HXMT instrument. We found that 30 bursts exhibited similar light curve profiles and were predominantly in the hard state, and two photospheric radius expansion (PRE) bursts were in the soft state. The light curves of most bursts did not follow a single exponential decay but displayed a dual-exponential behavior. The initial exponent had a duration of approximately 6 s. We utilized both the standard method and the `$f_{\rm a}$' method to fit the burst spectra. The majority of the `$f_{\rm a}$' values exceeded 1, indicating an enhancement of the persistent emission during the burst. Under the two comptonization components assumption, we suggest that the scattering of burst photons by the inner corona may mainly contribute to the persistent emission enhancement. We also observed an inverse correlation between the maximum $f_{\rm a}$ and the persistent emission flux in the non-PRE burst. This anti-correlation suggests that when the accretion rate is lower, there is a greater enhancement of persistent emission during the burst peak. The prediction based on Poynting-Robertson drag (P-R drag) aligns with this observed anti-correlation. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2401_11172 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Insight-HXMT observations of thermonuclear X-ray bursts in 4U 1636-53 Yan, Zhe Zhang, Guobao Chen, Yu-Peng Zhang, Shu Méndez, Mariano Peng, Jingqiang Zhang, Shuang-Nan Qu, Jinlu Lyu, Ming Mao, Jirong Ge, Mingyu Wang, Jiancheng High Energy Astrophysical Phenomena We conducted an analysis of 45 bursts observed from 4U 1636$-$53. To investigate the mechanism behind the light curve profiles and the impact of thermonuclear X-ray bursts on the accretion environment in accreting neutron star low-mass X-ray binaries. This analysis employed both light curve and time-resolved spectroscopy methodologies, with data collected by the \textit{Insight}-HXMT instrument. We found that 30 bursts exhibited similar light curve profiles and were predominantly in the hard state, and two photospheric radius expansion (PRE) bursts were in the soft state. The light curves of most bursts did not follow a single exponential decay but displayed a dual-exponential behavior. The initial exponent had a duration of approximately 6 s. We utilized both the standard method and the `$f_{\rm a}$' method to fit the burst spectra. The majority of the `$f_{\rm a}$' values exceeded 1, indicating an enhancement of the persistent emission during the burst. Under the two comptonization components assumption, we suggest that the scattering of burst photons by the inner corona may mainly contribute to the persistent emission enhancement. We also observed an inverse correlation between the maximum $f_{\rm a}$ and the persistent emission flux in the non-PRE burst. This anti-correlation suggests that when the accretion rate is lower, there is a greater enhancement of persistent emission during the burst peak. The prediction based on Poynting-Robertson drag (P-R drag) aligns with this observed anti-correlation. |
| title | Insight-HXMT observations of thermonuclear X-ray bursts in 4U 1636-53 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2401.11172 |