The energy dependence of the three types of low-frequency quasi-periodic oscillations in the black hole candidate H1743−322

Li, Z. B.; Zhang, S.; Qu, J. L.; Gao, He; Zhao, Huabiao; Huang, Chunping; Song, Liming

doi:10.1093/mnras/stt737

Cited by 29 publications

(18 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…In addition, it is also interesting to consider the inclination dependence of differences in the Type-C QPO cen-troid frequency in different energy bands. Such frequency differences have been reported in GRS 1915+105 (Qu et al 2010;Yan et al 2012), XTE J1550-564 (Li et al 2013a) and H1743-322 (Li et al 2013b). Van den Eijnden et al (2016) found that the observed differences in QPO centroid frequency in GRS 1915+105 correspond to a systematic evolution of phase lags while the QPO decoheres on timescales of seconds.…”

Section: Introductionsupporting

confidence: 70%

Inclination dependence of QPO phase lags in black hole X-ray binaries

Eijnden

Ingram

Uttley

et al. 2016

Mon. Not. R. Astron. Soc.

108

View full text Add to dashboard Cite

Quasi-periodic oscillations (QPOs) with frequencies from ∼ 0.05-30 Hz are a common feature in the X-ray emission of accreting black hole binaries. As the QPOs originate from the innermost accretion flow, they provide the opportunity to probe the behaviour of matter in extreme gravity. In this paper, we present a systematic analysis of the inclination dependence of phase lags associated with both Type-B and Type-C QPOs in a sample of 15 Galactic black hole binaries. We find that the phase lag at the Type-C QPO frequency strongly depends on inclination, both in evolution with QPO frequency and sign. Although we find that the Type-B QPO soft lags are associated with high inclination sources, the source sample is too small to confirm this as a significant inclination dependence. These results are consistent with a geometrical origin of Type-C QPOs and a different origin for Type-B and Type-C QPOs. We discuss the possibility that the phase lags originate from a pivoting spectral power law during each QPO cycle, while the inclination dependence arises from differences in dominant relativistic effects. We also search for energy dependences in the Type-C QPO frequency. We confirm this effect in the three known sources (GRS 1915+105, H1743-322 and XTE J1550-564) and newly detect it in XTE J1859+226. Lastly, our results indicate that the unknown inclination sources XTE J1859+226 and MAXI J1543-564 are most consistent with a high inclination.

show abstract

Section: Introductionsupporting

confidence: 70%

Inclination dependence of QPO phase lags in black hole X-ray binaries

Eijnden

Ingram

Uttley

et al. 2016

Mon. Not. R. Astron. Soc.

108

View full text Add to dashboard Cite

show abstract

“…In addition to MAXI J1535-571, similar energy dependence relations for the type-C QPO were found in GRS 1915+015 (Rodriguez et al 2004;Yan et al 2012Yan et al , 2013Yadav et al 2016), H1743-322 (Li et al 2013b), XTE J1859+226 (Casella et al 2004) and XTE J1550-564 (Li et al 2013a), in which a corona origin of type-C QPOs is considered. For GRS 1915+105, HEXTE results showed that the QPO rms decreases above 20 keV (Tomsick and Kaaret 2001).…”

Section: Energy Dependence Of Qpo Parameterssupporting

confidence: 59%

“…For energies < 20 keV, this relation in GRS 1915+105 (Qu et al 2010;Yan et al 2012Yan et al , 2018 and XTE J1550-564 (Li et al 2013a) evolves from a negative correlation to a positive one when the QPO frequency increases, but with a different turn-over QPO frequency. The pattern in H1743-322 shows no apparent turn-over frequency, which might be due to the lack of observational data for the hard state (Li et al 2013b). The energy dependence of the QPO frequency could be caused by differential precession of the inner accretion flow (van den Eijnden et al 2016).…”

Section: Energy Dependence Of Qpo Parametersmentioning

confidence: 99%

INSIGHT-HXMT Observations of the New Black Hole Candidate MAXI J1535−571: Timing Analysis

Huang

Qu²,

Zhang

et al. 2018

ApJ

Self Cite

View full text Add to dashboard Cite

We present the X-ray timing results of the new black hole candidate (BHC) MAXI J1535-571 during its 2017 outburst from Hard X-ray Modulation Telescope (Insight -HXMT) observations taken from 2017 September 6 to 23. Following the definitions given by Belloni (2010), we find that the source exhibits state transitions from Low/Hard state (LHS) to Hard Intermediate state (HIMS) and eventually to Soft Intermediate state (SIMS). Quasi-periodic oscillations (QPOs) are found in the intermediate states, which suggest different types of QPOs. With the large effective area of Insight -HXMT at high energies, we are able to present the energy dependence of the QPO amplitude and centroid frequency up to 100 keV which is rarely explored by previous satellites. We also find that the phase lag at the type-C QPOs centroid frequency is negative (soft lags) and strongly correlated with the centroid frequency. By assuming a geometrical origin of type-C QPOs, the source is consistent with being a high inclination system.

show abstract

“…However, below ∼ 3.3 Hz no variations with energy were observed. Li et al (2013b) reported comparable behaviour in the QPO in H1743-322, also exclusively showing frequency increases with photon energy. GRS 1915+105 is thus the only source to systematically show decreases of QPO frequency with energy.…”

Section: Introductionmentioning

confidence: 69%

Probing the origin of quasi-periodic oscillations: the short-time-scale evolution of phase lags in GRS 1915+105

Eijnden

Ingram

Uttley

2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We present a model-independent analysis of the short-timescale energy dependence of low frequency quasi-periodic oscillations (QPOs) in the X-ray flux of GRS 1915+105. The QPO frequency in this source has previously been observed to depend on photon energy, with the frequency increasing with energy for observations with a high ( 2 Hz) QPO frequency, and decreasing with energy for observations with a low ( 2 Hz) QPO frequency. As this observed energy dependence is currently unexplained, we investigate if it is intrinsic to the QPO mechanism by tracking phase lags on (sub)second timescales. We find that the phase lag between two broad energy bands systematically increases for 5 -10 QPO cycles, after which the QPO becomes decoherent, the phase lag resets and the pattern repeats. This shows that the band with the higher QPO frequency is running away from the other band on short timescales, providing strong evidence that the energy dependence of the QPO frequency is intrinsic. We also find that the faster the QPO decoheres, the faster the phase lag increases, suggesting that the intrinsic frequency difference contributes to the decoherence of the QPO. We interpret our results within a simple geometric QPO model, where different radii in the inner accretion flow experience Lense-Thirring precession at different frequencies, causing the decoherence of the oscillation. By varying the spectral shape of the inner accretion flow as a function of radius, we are able to qualitatively explain the energy-dependent behaviour of both QPO frequency and phase lag.

show abstract

The energy dependence of the three types of low-frequency quasi-periodic oscillations in the black hole candidate H1743−322

Cited by 29 publications

References 26 publications

Inclination dependence of QPO phase lags in black hole X-ray binaries

Inclination dependence of QPO phase lags in black hole X-ray binaries

INSIGHT-HXMT Observations of the New Black Hole Candidate MAXI J1535−571: Timing Analysis

Probing the origin of quasi-periodic oscillations: the short-time-scale evolution of phase lags in GRS 1915+105

Contact Info

Product

Resources

About