A Comprehensive Chandra Study of the Disk Wind in the Black Hole Candidate 4U 1630-472

Trueba, Nicolas; Miller, J. M.; Kaastra, J. S.; Zoghbi, A.; Fabian, A. C.; Proga, Daniel; Raymond, J. C.

doi:10.3847/1538-4357/ab4f70

Cited by 28 publications

(32 citation statements)

References 66 publications

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“…to see that a smooth wind with a density profile of the form n(r) = n 0 (r/r 0 ) −p implies p = (2α + 1)/(α + 1), corresponding to the range of 1 < ∼ p < ∼ 1.23, which is in fact broadly consistent with other independent work on X-ray absorbers (e.g. F10; Detmers et al 2011;Fukumura et al 2015;F17;Fukumura et al 2018;Trueba et al 2019;Laha et al 2016).…”

Section: Introductionsupporting

confidence: 88%

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: Introductionsupporting

confidence: 88%

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

Fukumura,

Kazanas,

Shrader

et al. 2021

Preprint

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“…The AMD characterizes the distribution of the hydrogen column density along the line of sight as a function of logξ and is defined in Holczer et al 2007 as AMD = dN H /d(logξ). This can be re-cast (see Trueba et al 2019) into expressions of the form n ∝ r −α , where α is a simple index, not the magnetic stress term from Shakura & Sunyaev 1973. A spherically symmetric, mass-conserving flow would have a value of α = 2, for instance.…”

Section: Resultsmentioning

confidence: 99%

Swift Spectroscopy of the Accretion Disk Wind in the Black Hole GRO J1655–40

Balakrishnan

Miller

Trueba

et al. 2020

ApJ

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Chandra obtained two High Energy Transmission Grating (HETG) spectra of the stellar-mass black hole GRO J1655−40 during its 2005 outburst, revealing a rich and complex disk wind. Soon after its launch, the Neil Gehrels Swift Observatory began monitoring the same outburst. Some X-ray Telescope (XRT) observations were obtained in a mode that makes it impossible to remove strong Mn calibration lines, so the Fe Kα line region in the spectra was previously neglected. However, these lines enable a precise calibration of the energy scale, facilitating studies of the absorption-dominated disk wind and its velocity shifts. Here, we present fits to 15 Swift/XRT spectra, revealing variability and evolution in the outflow. The data strongly point to a magnetically driven disk wind: both the higher velocity (e.g., v ≃ 10 4 km s −1 ) and lower velocity (e.g., v ≃ 10 3 km s −1 ) wind components are typically much faster than is possible for thermally driven outflows (v ≤ 200 km s −1 ), and photoionization modeling yields absorption radii that are two orders of magnitude below the Compton radius that defines the typical inner extent of thermal winds. Moreover, correlations between key wind parameters yield an average absorption measure distribution (AMD) that is consistent with magnetohydrodynamic wind models. We discuss our results in terms of recent observational and theoretical studies of black hole accretion disks and outflows, and future prospects.

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“…gas , where Ω is the opening angle ( p W = 2 is assumed), μ is the average molecular weight of the gas (m = 1.23 is assumed as in some other black hole systems; e.g., Janiuk et al 2015;Trueba et al 2019), m p is the mass of a proton, and v is the outflow velocity. The mass accretion rate is roughly estimated as…”

Section: Spectral Analysismentioning

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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A Comprehensive Chandra Study of the Disk Wind in the Black Hole Candidate 4U 1630-472

Cited by 28 publications

References 66 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

Swift Spectroscopy of the Accretion Disk Wind in the Black Hole GRO J1655–40

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

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