Phase-resolved spectral analysis of the 11 mHz quasi-periodic oscillation in the black hole candidate H1743–322

Cheng, Zheng; Méndez, Mariano; Altamirano, D.; Beri, Aru; Wang, Yanan

doi:10.1093/mnras/sty2695

Cited by 6 publications

(6 citation statements)

References 70 publications

(85 reference statements)

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“…In addition, the fractional rms amplitude of the ∼11 mHz QPO is significantly lower (3.1% ± 0.4%). Meanwhile, its energy-dependent properties also seems to be different from that found in 4U 1630-47 (Altamirano & Strohmayer 2012;Cheng et al 2019). Therefore, it is not clear whether the two mHz signals have a similar physical origin or not.…”

Section: Appearance Of the Mhz Qrmmentioning

confidence: 76%

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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

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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 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.

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Section: Appearance Of the Mhz Qrmmentioning

confidence: 76%

“…Apart from the comparison with the 1998 outburst, we also compare this mHz QRM with the ∼11 mHz QPO detected in H 1743-322 (Altamirano & Strohmayer 2012;Cheng et al 2019). Altamirano & Strohmayer (2012) reported the detection of a ∼11 mHz QPO in H 1743-322 at the beginning of the 2010 and 2011 outbursts.…”

Section: Appearance Of the Mhz Qrmmentioning

confidence: 88%

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

show abstract

“…In addition, the fractional rms amplitude of the ∼11 mHz QPO is significantly lower (3.1% ± 0.4%). Meanwhile, its energydependent properties also seem to be different from those found in 4U 1630-47 (Altamirano & Strohmayer 2012;Cheng et al 2019). Therefore, it is not clear whether the two mHz signals have a similar physical origin or not.…”

Section: Appearance Of the Mhz Qrmmentioning

confidence: 82%

“…Apart from the comparison with the 1998 outburst, we also compare this mHz QRM with the ∼11 mHz QPO detected in H1743-322 (Altamirano & Strohmayer 2012;Cheng et al 2019). Altamirano & Strohmayer (2012) reported the detection of a ∼11 mHz QPO in H1743-322 at the beginning of the 2010 and 2011 outbursts.…”

Section: Appearance Of the Mhz Qrmmentioning

confidence: 88%

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

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 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.

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“…Over the past several years there has been an increasing consensus on the geometrical origin of the type C quasi-periodic oscillations (QPOs; Ingram & Done 2009, 2011. The precessing hot flow model explains the dynamic origin of the QPOs quite well (Ingram & van der Klis 2015;Cheng et al 2019). You et al (2018) carried out extensive simulations under the framework of the Lense-Thirring precession model to predict the fractional variability spectrum during different states of an outburst and for various physical parameters.…”

Section: Discussionmentioning

confidence: 99%

Revisiting the Galactic X-Ray Binary MAXI J1631–479: Implications for High Inclination and a Massive Black Hole

Rout

Vadawale

Garcia

et al. 2023

ApJ

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X-ray spectroscopy of Galactic black hole binaries serves as a powerful tool to gain an overall understanding of the system. Not only can the properties of the accretion disk be studied in detail, the fundamental properties of the black hole such as spin and mass can also be measured. In this work we carry out a comprehensive spectral analysis of the X-ray binary MAXI J1631–479 using data from NICER and NuSTAR observatories. We trace the evolution of the accretion disk properties, such as density, ionization, and Fe abundance, as the source transitions from a disk-dominated soft state to a power-law-dominated hard intermediate state. As expected the disc ionization increased with hardness while the density and abundance (at solar values) remained unchanged. We provide strong constraints on the spin of the black hole (a > 0.996) and the inclination of the inner disk (50°–70°). We also use the soft-state NICER observations to constrain the black hole mass using distance estimates from optical observations. We find the probable mass of the black hole to be much higher than its X-ray binary counterparts with a conservative lower limit of 15 M ⊙ at 4.5 kpc.

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Phase-resolved spectral analysis of the 11 mHz quasi-periodic oscillation in the black hole candidate H1743–322

Cited by 6 publications

References 70 publications

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

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

Revisiting the Galactic X-Ray Binary MAXI J1631–479: Implications for High Inclination and a Massive Black Hole

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