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

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

doi:10.48550/arxiv.2009.10956

Cited by 3 publications

(2 citation statements)

References 31 publications

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“…The behaviour of the parameters with the count rate is just the opposite: the frequency and the FWHM increase while the fractional rms amplitude slightly decreases as count rate increases. A similar behaviour of 𝜈 𝐿𝐹 with count rate was found in other BH systems: e.g., GRS 1915+105 (Trudolyubov et al 1999;Reig et al 2000), GRS 1739-278 (Wĳnands et al 2001), XTE J1859+226 (Casella et al 2005b), XTE J1650-500 (Xiao et al 2018), XTE J1550-564 (Heil et al 2011), Swift J1842.5-1124(Zhao et al 2016) and EXO 1846-031 (Liu et al 2020). The QPO frequency of GRS 1739-278, on the contrary, increases with the hardness ratio (Wĳnands et al 2001).…”

Section: Evolution Of the Parameters Of The Qpo During The Reflaresupporting

confidence: 69%

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348–630 with NICER

Alabarta

Méndez

García

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We study the properties of the type-C quasi-periodic oscillation (type-C QPO) of MAXI J1348–630 during its 2019 outburst and reflare with NICER. This is the first time that the evolution of the properties of type-C QPOs are studied during an outburst reflare. We found that the properties of the type-C QPO during the reflare are similar to those of type-C QPOs observed in other black hole systems during outburst. This suggests that the physical processes responsible for type-C QPOs are the same in a reflare and in an outburst. We also found that the FWHM of a high-frequency broadband component observed during the reflare changes significantly with energy. We studied the energy-dependent fractional rms amplitude and phase lags of the type-C QPO from 0.5 keV to 12 keV. We found that the fractional rms amplitude increases up to 2–3 keV and then remains approximately constant above this energy, and the lag spectra of the type-C QPO are hard. We discuss the dependence of the fractional rms amplitude and phase lags with energy in the context of Comptonisation as the radiative mechanism driving the QPO rms and lag spectra.

show abstract

Section: Evolution Of the Parameters Of The Qpo During The Reflaresupporting

confidence: 69%

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348–630 with NICER

Alabarta

Méndez

García

et al. 2022

Monthly Notices of the Royal Astronomical Society

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show abstract

“…Remillard & McClintock 2006;Belloni 2010;Muñoz-Darias et al 2011). Liu et al (2020) conducted a timing analysis of EXO 1846-031 in the same outburst with HXMT and Neutron star Interior Composition Explorer (NICER). Based on the relative changes in the hardness ratio diagram and the fractional rms integrated in the 2 −5 − 32 Hz, they classify the entire outburst into four spectral states, i.e.…”

Section: Analysis and Resultsmentioning

confidence: 99%

A variable ionized disk wind in the black-hole candidate EXO 1846-031

Wang,

Ji,

Garcia

et al. 2020

Preprint

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After 34 years, the black-hole candidate EXO 1846-031 went into outburst again in 2019. We investigate its spectral properties in the hard intermediate and the soft states with NuSTAR and Insight-HXMT. A reflection component has been detected in the two spectral states but possibly originating from different illumination spectra: in the intermediate state, the illuminating source is attributed to a hard coronal component, which has been commonly observed in other X-ray binaries, whereas in the soft state the reflection is probably produced by the disk self-irradiation. Both cases support EXO 1846-031 as a low inclination system of ∼ 40 • . An absorption line is clearly detected at ∼ 7.2 keV in the hard intermediate state, corresponding to a highly ionized disk wind (log ξ > 6.1) with a velocity up to 0.06c. Meanwhile, quasi-simultaneous radio emissions have been detected before and after the X-rays, implying the co-existence of disk winds and jets in this system. Additionally, the observed wind in this source is potentially driven by magnetic forces. The absorption line disappeared in the soft state and a narrow emission line appeared at ∼ 6.7 keV on top of the reflection component, which may be evidence for disk winds, but data with the higher spectral resolution are required to examine this.

show abstract

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348-630 with NICER

Alabarta,

Méndez,

García

et al. 2022

Preprint

View full text Add to dashboard Cite

We study the properties of the type-C quasi-periodic oscillation (type-C QPO) of MAXI J1348-630 during its 2019 outburst and reflare with NICER. This is the first time that the evolution of the properties of type-C QPOs are studied during an outburst reflare. We found that the properties of the type-C QPO during the reflare are similar to those of type-C QPOs observed in other black-hole systems during outburst. This suggests that the physical processes responsible for type-C QPOs are the same in a reflare and in an outburst. We also found that the FWHM of a high-frequency broadband component observed during the reflare changes significantly with energy. We studied the energy-dependent fractional rms amplitude and phase lags of the type-C QPO from 0.5 keV to 12 keV. We found that the fractional rms amplitude increases up to 2-3 keV and then remains approximately constant above this energy, and the lag spectra of the type-C QPO are hard. We discuss the dependence of the fractional rms amplitude and phase lags with energy in the context of Comptonisation as the radiative mechanism driving the QPO rms and lag spectra.

show abstract

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

Cited by 3 publications

References 31 publications

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348–630 with NICER

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348–630 with NICER

A variable ionized disk wind in the black-hole candidate EXO 1846-031

Variability and phase lags of the type-C quasi-periodic oscillation of MAXI J1348-630 with NICER

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