Accretion disc atmospheres and winds in low‐mass X‐ray binaries

Trigo, María Díaz; Boirin, L.

doi:10.1002/asna.201612315

Cited by 114 publications

(80 citation statements)

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“…Low ionized state plasma, with log ξ ∼ 1.8 − 2.5, has been identified in BH and NS LMXBs in the past (see Table 1 in Díaz Trigo & Boirin 2016). However, we caution that none of these studies included in their models the warmhot component associated to the ISM (but note that van Peet et al (2009) included both a collisionally ionised and a photo-ionised plasma).…”

Section: Discussionmentioning

confidence: 99%

“…The crucial question of why the wind is absent during the hard accretion state remains unanswered. Some possibilities include thermal in-E-mail: efraingatuzz@gmail.com stabilities (Chakravorty et al 2013;Bianchi et al 2017), full ionization of the plasma (Ueda et al 2010;Díaz Trigo et al 2012, 2014Díaz Trigo & Boirin 2016), density changes in the wind (Miller et al 2012), geometrical changes in the system (Ueda et al 2010) or mass depletion between winds and jets (Neilsen & Lee 2009).…”

Section: Introductionmentioning

confidence: 99%

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

Gatuzz¹,

Trigo²,

Miller-Jones

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present a detailed analysis of three XMM-Newton observations of the black hole low-mass X-ray binary IGR J17091-3624 taken during its 2016 outburst. Radio observations obtained with the Australia Telescope Compact Array (ATCA) indicate the presence of a compact jet during all observations. From the best X-ray data fit results we concluded that the observations were taken during a transition from a hard accretion state to a hard-intermediate accretion state. For Observations 1 and 2 a local absorber can be identified in the EPIC-pn spectra but not in the RGS spectra, preventing us from distinguishing between absorption local to the source and that from the hot ISM component. For Observation 3, on the other hand, we have identified an intrinsic ionized static absorber in both EPIC-pn and RGS spectra. The absorber, observed simultaneously with a compact jet emission, is characterized by an ionization parameter of 1.96 < log ξ < 2.05 and traced mainly by Ne x, Mg xii, Si xiii and Fe xviii.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Gatuzz¹,

Trigo²,

Miller-Jones

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…Strong photoionization can fully ionize a wind, resulting in the disappearance of absorption lines Díaz Trigo & Boirin 2016).…”

Section: Discussionmentioning

confidence: 99%

“…Radio observations of jet outflows have revealed that they are highly collimated, often relativistic, and are launched close to the compact object (Fomalont et al 2001a(Fomalont et al , 2001bFender 2006;Fender & Gallo 2014). Disk winds are typically studied via narrow line features in X-ray spectra; they have a more equatorial geometry, are much slower, and are formed further out (Neilsen 2013;Díaz Trigo & Boirin 2016). Observed behavior in the black hole (BH) LMXB H1743-332 suggested that jets and disk winds are causally related (Miller et al 2006); later, Neilsen & Lee (2009) found that in the BH LMXB GRS 1915+105 the jet outflows are typically quenched when strong disk winds are present (see also Miller et al 2008).…”

Section: Introductionmentioning

confidence: 99%

Evidence for Simultaneous Jets and Disk Winds in Luminous Low-Mass X-Ray Binaries

Homan

Neilsen

Allen

et al. 2016

ApJL

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Recent work on jets and disk winds in low-mass X-ray binaries (LMXBs) suggests that they are to a large extent mutually exclusive, with jets observed in spectrally hard states and disk winds observed in spectrally soft states. In this paper we use existing literature on jets and disk winds in the luminous neutron star (NS) LMXB GX 13+1, in combination with archival Rossi X-ray Timing Explorer data, to show that this source is likely able to produce jets and disk winds simultaneously. We find that jets and disk winds occur in the same location on the source's track in its X-ray color-color diagram. A further study of literature on other luminous LMXBs reveals that this behavior is more common, with indications for simultaneous jets and disk winds in the black hole LMXBs V404 Cyg and GRS 1915+105 and the NS LMXBs Sco X-1 and Cir X-1. For the three sources for which we have the necessary spectral information, we find that simultaneous jets/winds all occur in their spectrally hardest states. Our findings indicate that in LMXBs with luminosities above a few tens of percent of the Eddington luminosity, jets and disk winds are not mutually exclusive, and the presence of disk winds does not necessarily result in jet suppression.

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“…Bjerkeli et al 2016) through to stellar mass compact objects (both black holes and neutron stars) in X-ray binaries (e.g. Ponti et al 2012;Díaz Trigo & Boirin 2016) and the supermassive black holes in active galactic nuclei (AGN) at the centre of galaxies (e.g. Nardini et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The thermal-radiative wind in low-mass X-ray binary H1743−322 – II. Iron line predictions from Monte Carlo radiation transfer

Tomaru

Done

Ohsuga

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We show the best current simulations of the absorption and emission features predicted from thermal-radiative winds produced from X-ray illumination of the outer accretion disc in binary systems. We use the density and velocity structure derived from a radiation hydrodynamic code as input to a Monte-Carlo radiation transport calculation. The initial conditions are matched to those of the black hole binary system H1743-322 in its soft, disc dominated state, where wind features are seen in Chandra grating data. Our simulation fits well to the observed line profile, showing that these physical wind models can be the origin of the absorption features seen, rather than requiring a magnetically driven wind. We show how the velocity structure is key observable discriminator between magnetic and thermal winds. Magnetic winds are faster at smaller radii, whereas thermal winds transition to a static atmosphere at smaller radii. New data from XRISM (due for launch Jan 2022) will give an unprecedented view of the physics of the wind launch and acceleration processes, but the existence of static atmospheres in small disc systems already rules out magnetic winds which assume self-similar magnetic fields from the entire disc as the origin of the absorption features seen.

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Accretion disc atmospheres and winds in low‐mass X‐ray binaries

Cited by 114 publications

References 100 publications

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

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

Evidence for Simultaneous Jets and Disk Winds in Luminous Low-Mass X-Ray Binaries

The thermal-radiative wind in low-mass X-ray binary H1743−322 – II. Iron line predictions from Monte Carlo radiation transfer

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