Simultaneous detection of an intrinsic absorber and a compact jet emission in the X-ray binary IGR J17091−3624 during a hard accretion state

Gatuzz, E.; Trigo, María Díaz; Miller-Jones, J. C. A.; Migliari, S.

doi:10.1093/mnras/stz3385

Cited by 12 publications

(6 citation statements)

References 53 publications

(70 reference statements)

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“…V404 Cyg and IGR J17091-3624) (e.g. Homan et al 2016;Gatuzz et al 2020). Such a persistent existence of optical disk-winds in XRBs even during hard state is in fact consistent with our X-ray wind model; its spectroscopic appearance changes between the two states due to the intrinsic change in an internal physical condition of the wind such as (p, n 17 ) as well as photoionization balance, as found in this work.…”

Section: Summary and Discussionsupporting

confidence: 90%

Modeling Magnetic Disk-Wind State Transitions in Black Hole X-ray Binaries

Fukumura,

Kazanas,

Shrader

et al. 2021

Preprint

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We analyze three prototypical black hole (BH) X-ray binaries (XRBs), 4U1630-472, GRO J1655-40 and H1743-322, in an effort to systematically understand the intrinsic state transition of the observed accretion-disk winds between wind-on and wind-off states by utilizing state-of-the-art Chandra/HETGS archival data from multi-epoch observations. We apply our magnetically-driven wind models in the context of magnetohydrodynamic (MHD) calculations to constrain their (1) global density slope (p), (2) their density (n 17 ) at the foot point of the innermost launching radius and (3) the abundances of heavier elements (A Fe,S,Si ). Incorporating the MHD winds into xstar photoionization calculations in a self-consistent manner, we create a library of synthetic absorption spectra given the observed X-ray continua. Our analysis clearly indicates a characteristic bi-modal transition of multi-ion X-ray winds; i.e. the wind density gradient is found to steepen (from p ∼ 1.2 − 1.4 to ∼ 1.4 − 1.5) while its density normalization declines as the source transitions from wind-on to wind-off state. The model implies that the ionized wind remains physically present even in wind-off state, despite its absent appearance in the observed spectra. Super-solar abundances for heavier elements are also favored. Our global multi-ion wind models, taking into account soft X-ray ions as well as Fe K absorbers, show that the internal wind condition plays an important role in wind transitions besides photoionization changes. Simulated XRISM/Resolve and Athena/X-IFU spectra are presented to demonstrate a high fidelity of the multi-ion wind model for better understanding of these powerful ionized winds in the coming decades.

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Section: Summary and Discussionsupporting

confidence: 90%

Modeling Magnetic Disk-Wind State Transitions in Black Hole X-ray Binaries

Fukumura,

Kazanas,

Shrader

et al. 2021

Preprint

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“…There is evidence for an anticorrelation between jets and disk winds in LMXBs: jets are present in the hard state and disk winds are present in the soft state (e.g., Miller et al 2006bMiller et al , 2008. However, some studies show that jets and disk winds can coexist in the hard state (e.g., Homan et al 2016;Gatuzz et al 2020). Moreover, Homan et al (2016) suggested that disk winds and jets do not need to be mutually exclusive in LMXBs when a source luminosity is higher than a few tens of percent of the Eddington luminosity.…”

Section: Disk Wind In the Hard Intermediate Statementioning

confidence: 99%

A Variable Ionized Disk Wind in the Black Hole Candidate EXO 1846–031

Wang

Ji²,

Garcia

et al. 2020

ApJ

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After 34 yr, 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 disk selfirradiation. 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 (x > log 6.1) with a velocity of up to 0.06c. Meanwhile, quasi-simultaneous radio emissions have been detected before and after the X-rays, implying the coexistence of disk winds and jets in this system. If only the high-flux segment of the NuSTAR observation is considered, the observed wind appears to be magnetically driven. 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 higher spectral resolution are required to examine this.

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“…To study the transition of the source towards quiescence we selected archived Chandra (Weisskopf 1999) and XMM-Newton (Barré, Nye & Janin 1999) observations performed within June -October of 2013. These data, presented here for the first time, correspond to the five last months of the 2011-2013 outburst (for further information about the behaviour of the source in outburst we refer to Gatuzz, et al 2020;Radhika, et al 2018;Xu, et al 2017;Court et al 2017;Grinberg et al 2016 and references therein).…”

Section: Observationsmentioning

confidence: 88%

Swift/XRT, Chandra, and XMM–Newton observations of IGR J17091–3624 as it returns into quiescence

Pereyra

Altamirano

Court

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Abstract IGR J17091-3624 is a low mass X-ray binary (LMXB) which received wide attention from the community thanks to its similarities with the bright black hole system GRS 1915+105. Both systems exhibit a wide range of highly structured X-ray variability during outburst, with time scales from few seconds to tens of minutes, which make them unique in the study of mass accretion in LMXBs. In this work we present a general overview into the long-term evolution of IGR J17091-3624, using Swift/XRT observations from the onset of the 2011–2013 outburst in February 2011 to the end of the last bright outburst in November 2016. We found 4 re-flares during the decay of the 2011 outburst, but no similar re-flares appear to be present in the latter one. We studied in detail the period with the lowest flux observed in the last 10 years, just at the tail end of the 2011-2013 outburst, using Chandra and XMM-Newton observations. We observed changes in flux as high as a factor of 10 during this period of relative quiescence, without strong evidence of softening in the spectra. This result suggests that the source has not been observed at its true quiescence so far. By comparing the spectral properties at low luminosities of IGR J17091–3624 and those observed for a well studied population of LMXBs, we concluded that IGR J17091–3624 is most likely to host a black hole as a compact companion rather than a neutron star.

show abstract

Simultaneous detection of an intrinsic absorber and a compact jet emission in the X-ray binary IGR J17091−3624 during a hard accretion state

Cited by 12 publications

References 53 publications

Modeling Magnetic Disk-Wind State Transitions in Black Hole X-ray Binaries

Modeling Magnetic Disk-Wind State Transitions in Black Hole X-ray Binaries

A Variable Ionized Disk Wind in the Black Hole Candidate EXO 1846–031

Swift/XRT, Chandra, and XMM–Newton observations of IGR J17091–3624 as it returns into quiescence

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