The appearance of a compact jet in the soft–intermediate state of 4U 1543−47

Russell, D. M.; Casella, P.; Kalemci, Emrah; Vahdat, Armin; Saikia, Payaswini; Pirbhoy, Saarah F.; Maitra, D.

doi:10.1093/mnras/staa1182

Cited by 20 publications

(21 citation statements)

References 90 publications

(163 reference statements)

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“…Although no comprehensive model has been proposed for the type-B QPOs, there is growing evidence suggesting that they may originate in a jet-like structure. The most striking observational evidence is the fact that the launch of discrete jet ejection (or the resulting radio flare) occurs close in time to the appearance of the type-B QPO, which has been found in a few BHBs (Soleri et al 2008;Fender et al 2009;Russell et al 2019a;Homan et al 2020;Russell et al 2020). However, the precise association between the ejection event and the type-B QPO is not clear, as the type-B QPO sometimes appears before and sometimes after the inferred jet ejection.…”

Section: Origin Of the Type-b Qpomentioning

confidence: 99%

“…The physical origin of these two types of QPOs is less clear. Hints of a connection between the appearance of type-B QPO and the launch of discrete jet ejection have been found in several BHBs (e.g., Soleri et al 2008;Fender et al 2009;Russell et al 2019a;Homan et al 2020;Russell et al 2020), pointing to a jet-based origin of type-B QPOs. In this work, we will focus our study on the type-B QPOs.…”

Section: Introductionmentioning

confidence: 99%

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NICER uncovers the transient nature of the type-B quasi-periodic oscillation in the black hole candidate MAXI J1348−630

Zhang

Altamirano

Uttley

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We present a systematic spectral-timing analysis of a fast appearance/disappearance of a type-B quasi-periodic oscillation (QPO), observed in four NICER observations of MAXI J1348−630. By comparing the spectra of the period with and without the type-B QPO, we found that the main difference appears at energy bands above ∼2 keV, suggesting that the QPO emission is dominated by the hard Comptonised component. During the transition, a change in the relative contribution of the disk and Comptonised emission was observed. The disk flux decreased while the Comptonised flux increased from non-QPO to type-B QPO. However, the total flux did not change too much in the NICER band. Our results reveal that the type-B QPO is associated with a redistribution of accretion power between the disk and Comptonised emission. When the type-B QPO appears, more accretion power is dissipated into the Comptonised region than in the disk. Our spectral fits give a hint that the increased Comptonised emission may come from an additional component that is related to the base of the jet.

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Section: Origin Of the Type-b Qpomentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

NICER uncovers the transient nature of the type-B quasi-periodic oscillation in the black hole candidate MAXI J1348−630

Zhang

Altamirano

Uttley

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Fast transitions can occur between different states, associated with rapid changes between the type-B QPO and other types of QPOs in the PDS (e.g., Takizawa et al 1997;Nespoli et al 2003;Belloni et al 2005). These transitions can be accompanied by discrete jet ejections observed in radio (e.g., Fender et al 2004), suggesting a possible connection between the type-B QPO and the relativistic jet (e.g., Fender et al 2009;Homan et al 2020;Russell et al 2020).…”

Section: Introductionmentioning

confidence: 99%

A two-component Comptonization model for the type-B QPO in MAXI J1348−630

García

Méndez

Καρπούζας

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Spectral-timing analysis of the fast variability observed in X-rays is a powerful tool to study the physical and geometrical properties of the accretion/ejection flows in black hole (BH) binaries. The origin of type-B quasi-periodic oscillations (QPO), predominantly observed in BH candidates in the soft-intermediate state, has been linked to emission arising from the relativistic jet. In this state, the X-ray spectrum is characterized by a soft-thermal blackbody-like emission due to the accretion disc, an iron emission line (in the 6–7 keV range), and a power-law-like hard component due to inverse-Compton scattering of the soft-photon source by hot electrons in a corona or the relativistic jet itself. The spectral-timing properties of MAXI J1348−630 have been recently studied using observations obtained with the NICER observatory. The data show a strong type-B QPO at ∼4.5 Hz with increasing fractional rms amplitude with energy and positive lags with respect to a reference band at 2–2.5 keV. We use a variable-Comptonization model that assumes a sinusoidal coherent oscillation of the Comptonized X-ray flux and the physical parameters of the corona at the QPO frequency, to fit simultaneously the energy-dependent fractional rms amplitude and phase lags of this QPO. We show that two physically connected Comptonization regions can successfully explain the radiative properties of the QPO in the full 0.8–10 keV energy range.

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“…During the rise of an outburst, a compact jet is always seen in the first three states. By the soft intermediate state, a jet had previously been suspected to be present but it is confirmed that it has been observed (Russell et al 2020). In the soft state, the jet disappears.…”

Section: Introductionmentioning

confidence: 56%

A quantitative explanation of the type-B QPOs in GX 339-4

Kylafis,

Reig,

Papadakis

2020

Preprint

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Context. Type-B quasi periodic oscillations (QPOs) in black-hole X-ray binaries (BHXRBs) are a class of low-frequency QPOs that are observed in the soft intermediate state in the rising and the declining phases of an outburst. They are suspected to result from the precession of the jet that is ejected from the source. Aims. The objective of the present work is to investigate in detail the emissivity of the jet in hard X-rays and to see whether the type-B QPOs from GX 339-4, which is the best studied black-hole transient, can be explained quantitatively with a precessing jet. Methods. We used our simple jet model, which invokes Comptonization in the jet, and examined the angular dependence of the upscattered photons that emerge from the jet and their energy distribution, which is a power law. Results. Due to the elongation of the jet, assisted by the bulk motion of the electrons, the angular distribution of the emerging hard Xray photons from the jet is not isotropic. More importantly, the photon-number spectral index, Γ, is an increasing function of the polar angle, θ, with respect to the axis of the jet. If the jet is fixed, then an observer at infinity sees the photon index, Γ, which corresponds to this specific observational direction. However, if the jet is precessing, then the observer sees a periodic variation of Γ with the precession period. Such a periodic variation of Γ has been observed in GX 339-4 and in this work, we reproduce it quantitatively, using our model. Conclusions. Our jet model nicely explains through quantitative means the type-B QPOs seen in GX 339-4 as originating from a precessing jet. The given model has previously explained several observed correlations thus far.

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The appearance of a compact jet in the soft–intermediate state of 4U 1543−47

Cited by 20 publications

References 90 publications

NICER uncovers the transient nature of the type-B quasi-periodic oscillation in the black hole candidate MAXI J1348−630

NICER uncovers the transient nature of the type-B quasi-periodic oscillation in the black hole candidate MAXI J1348−630

A two-component Comptonization model for the type-B QPO in MAXI J1348−630

A quantitative explanation of the type-B QPOs in GX 339-4

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