The 2018 failed outburst of H 1743 – 322: <i>Insight-HXMT, NuSTAR</i>, and <i>NICER</i> views

Wang, P J; Kong, L. D.; Chen, Y P; Zhang, S; Zhang, S N; Soria, Roberto; Ji, Long; Qu, J. L.; Huang, Y.; Tao, Lian; Ge, Ming-Yu; Chen, Liang; Li, T P; Xu, YP; Cao, X. L.; Liu, C Z; Bu, Q. C.; Cai, C.; Chang, Zhi; Chen, T X; Chen, Y B; Cui, Wei; Du, Yan-Qi; Gao, G. H.; Gu, Y. D.; Guan, J.; Guo, Chengcheng; Han, Danxiang; Jia, Haiqiang; Jia, S. M.; Jiang, Weichun; Jin, J.; Li, B; Li, C K; Li, G; Li, W; Li, X; Li, Z W; Liang, X. H.; Liao, J. Y.; Liu, B S; Liu, H X; Liu, X J; Lu, Xiao-Meng; Luo, Q.; Luo, T.; C, R; Ma, Xiang; Meng, Bin; Nang, Y.; Nie, J. Y.; Ou, G.; Ren, Xiaokang; Sai, N.; Song, Liming; Song, X. Y.; Sun, Liang; Tan, Ying; Tuo, You-Li; Wang, Chunling; Wang, L. J.; Wang, W S; Wang, Y S; Wen, Xiang-Yang; Wu, Bai-Yang; Wu, Mei‐Hwan; Xiao, G. C.; Xiao, Shuo; Xiong, S. L.; Yang, Rong-Jia; Yang, S.; Yang, Yun-Cheng; Yang, Yi; Yi, Q. B.; Yin, Q. Q.; You, Y.; Zhang, F; Zhang, H M; Zhang, J; Zhang, Peng; Zhang, W C; Zhang, W; Zhang, Y F; Zhang, Y H; Zhao, H. S.; Zhao, X. F.; Zheng, S.; Zheng, Y. G.; Zhou, D. K.

doi:10.1093/mnras/stac773

Cited by 11 publications

(9 citation statements)

References 97 publications

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“…The most recent failed-transition outburst of H1743-322, monitored by Insight-HXMT in 2018, has been reported by Wang et al (2022). Different from the outbursts presented above, this outburst remained in the LHS and never showed a significant hysteresis trace in the HID throughout the observed stage (see Figure 10(a)).…”

Section: Possible Relations Between Rms Differences and Hysteresis Ef...mentioning

confidence: 69%

“…Type C QPOs usually appear in the HIMS, a stage that shows the significant transition in both the timing and spectral domains Remillard & McClintock 2006), where the properties of the type C QPO, like central frequency and fractional rms, evolve in a large value range. Previous studies have presented that the fractional rms of type C QPOs varies with the frequency (see Motta et al 2015;van Doesburgh & van der Klis 2020;Zhang et al 2020;Wang et al 2022). Here, we analyze a number of type C QPO samples across different outbursts of H1743-322 and present the QPO fractional rms dependence on fundamental frequency in both the rise and decay phases in Figure 5(a) for comparisons.…”

Section: Qpo Rms Dependence On Frequencymentioning

confidence: 97%

“…Recently, Aneesha & Mandal (2020) systematically analyzed the spectral evolution of the outbursts of H1743-322 in the RXTE era. In the post-RXTE era, there were outbursts in 2012, 2014, 2016, and 2018 monitored by other instruments (Shidatsu et al 2014;Stiele & Yu 2016;Chand et al 2020;Williams et al 2020;Wang et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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Tracing the Accretion Geometry of H1743-322 with Type C Quasiperiodic Oscillations in Multiple Outbursts

Shui

Zhang²,

Chen³

et al. 2023

ApJ

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We present a systematic analysis of type C quasiperiodic oscillation (QPO) observations of H1743-322 throughout the Rossi X-ray Timing Explorer era. We find that, while different outbursts have significant flux differences, they show consistent positive correlations between the QPO fractional rms amplitude and nonthermal fraction of the emission, which indicate an independence of the intrinsic QPO rms on individual outburst brightnesses in H1743-322. However, the dependence of the QPO rms on frequency is different between the outburst rise and decay phases, where the QPO fractional rms of the decay phase is significantly lower than that of the rise phase at low frequencies. The spectral analysis also reveals different ranges of coronal temperature between the two outburst stages. A semiquantitative analysis shows that the Lense–Thirring precession model could be responsible for the QPO rms differences, requiring a variable coronal geometric shape. However, the variable-Comptonization model could also account for the findings. The fact that the rms differences and the hysteresis traces in the hardness–intensity diagram accompany each other indicates a connection between the two phenomena. By correlating the findings with QPO phase lags and the quasi-simultaneous radio flux previously published, we propose there could be corona-jet transitions in H1743-322 similar to those that have been recently reported in GRS 1915+105.

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Section: Possible Relations Between Rms Differences and Hysteresis Ef...mentioning

confidence: 69%

Section: Qpo Rms Dependence On Frequencymentioning

confidence: 97%

See 1 more Smart Citation

Tracing the Accretion Geometry of H1743-322 with Type C Quasiperiodic Oscillations in Multiple Outbursts

Shui

Zhang²,

Chen³

et al. 2023

ApJ

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show abstract

“…In this model, the multiplicative constant is used to quantify the cross-calibration uncertainties between the three instruments of Insight-HXMT. The component thcomp is a novel thermal Comptonization convolution model to describe the broadband X-ray power-law continuum, which is presented as a replacement for the nthcomp model (Zdziarski et al 1996(Zdziarski et al , 2020Dziełak et al 2021;Wang et al 2022). To use the thcomp convolution model, we extend the energy grid from 0.1 keV to 500 keV with the XSPEC command ENERGIES to treat the limited response matrices at high or low energies.…”

Section: Spectral Changes During the Transitions Between Different Ki...mentioning

confidence: 99%

An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47

Yang

Zhang

Huang

et al. 2022

ApJ

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Here we report the spectral-timing results of the black hole X-ray binary 4U 1630–47 during its 2021 outburst using observations from the Hard X-ray Modulation Telescope (Insight-HXMT). Type C quasi-periodic oscillations (QPOs) in ∼1.6–4.2 Hz and quasi-regular modulation (QRM) near 60 mHz are detected during the outburst. The mHz QRM has a fractional rms of ∼10%–16% in the 8–35 keV energy band with a Q factor (frequency/width) of ∼2–4. Benefiting from the broad energy band of Insight-HXMT, we study the energy dependence of the ∼60 mHz QRM in 1–100 keV for the first time. We find that the fractional rms of the mHz QRM increases with photon energy, while the time lags of the mHz QRM are soft and decrease with photon energy. Fast recurrence of the mHz QRM, in a timescale of less than 1 hr, has been observed during the outburst. During this period, the corresponding energy spectra moderately change when the source transitions from the QRM state to the non-QRM state. The QRM phenomenon also shows a dependence with the accretion rate. We suggest that the QRM could be caused by an unknown accretion instability aroused from the corona.

show abstract

“…In this model, the multiplicative constant is used to quantify the cross-calibration uncertainties between the three instruments of Insight-HXMT. The component thcomp is a novel thermal Comptonization convolution model to describe the broadband X-ray power-law continuum, which is presented as a replacement for the nthcomp model (Zdziarski et al 1996(Zdziarski et al , 2020Dziełak et al 2021;Wang et al 2022). To use the thcomp convolution model, we extend the energy grid from 0.1 keV to 500 keV with the XSPEC command ENERGIES to treat with the limited response matrices at high or low energies.…”

Section: Spectral Changes During the Transitions Between Different Ki...mentioning

confidence: 99%

An Insight-HXMT view of the mHz quasi-regular modulation phenomenon in the black hole X-ray binary 4U 1630-47

Yang¹,

Zhang²,

Huang³

et al. 2022

Preprint

View full text Add to dashboard Cite

Here we report the spectral-timing results of the black hole X-ray binary 4U 1630-47 during its 2021 outburst using observations from the Hard X-ray Modulation Telescope (Insight-HXMT). Type-C quasi-periodic oscillations (QPOs) in ∼1.6-4.2 Hz and quasi-regular modulation (QRM) near 60 mHz are detected during the outburst. The mHz QRM has a fractional rms of ∼10%-16% in the 8-35 keV energy band with a Q factor (frequency/width) of ∼2-4. Benefiting from the broad energy band of Insight-HXMT, we study the energy dependence of the ∼60 mHz QRM in 1-100 keV for the first time. We find that the fractional rms of the mHz QRM increases with photon energy, while the time lags of the mHz QRM are soft and decrease with photon energy. Fast recurrence of the mHz QRM, in a timescale of less than one hour, has been observed during the outburst. During this period, the corresponding energy spectra moderately change when the source transitions from the QRM state to the non-QRM state. The QRM phenomena also shows a dependence with the accretion rate. We suggest that the QRM could be caused by an unknown accretion instability aroused from the corona.

show abstract

The 2018 failed outburst of H 1743 – 322: Insight-HXMT, NuSTAR, and NICER views

Cited by 11 publications

References 97 publications

Tracing the Accretion Geometry of H1743-322 with Type C Quasiperiodic Oscillations in Multiple Outbursts

Tracing the Accretion Geometry of H1743-322 with Type C Quasiperiodic Oscillations in Multiple Outbursts

An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630–47

An Insight-HXMT view of the mHz quasi-regular modulation phenomenon in the black hole X-ray binary 4U 1630-47

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