Radiation hydrodynamic simulations of line-driven disk winds for ultra-fast outflows

Nomura, Munehiro; Ohsuga, Ken; Takahashi, Hiroyuki R.; Wada, Keiichi; Yoshida, Tessei

doi:10.1093/pasj/psv124

Cited by 77 publications

(67 citation statements)

References 36 publications

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“…UV lines are especially effective, as they can absorb enough momentum to accelerate the material so that the line is shifted from resonance, so there is new continuum to absorb. Such UV line driven disc winds can be extremely powerful even for sub-Eddington flows (Proga et al 2000;Proga & Kallman 2004;Risaliti & Elvis 2010;Nomura et al 2013Nomura et al , 2016, and are also supported by some observations (e.g. Matzeu et al 2017).…”

supporting

confidence: 72%

UV line-driven disc wind as the origin of UltraFast Outflows in AGN

Mizumoto

Nomura

Done

et al. 2021

Monthly Notices of the Royal Astronomical Society

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UltraFast Outflows (UFO) are observed in some active galactic nuclei (AGN), with blueshifted and highly ionised Fe-K absorption features. AGN typically have a UV bright accretion flow, so UV line driving is an obvious candidate for launching these winds. However this mechanism requires material with UV opacity, in apparent conflict with the observed high ionisation state of the wind. In this paper we synthesise the X-ray energy spectra resulting from different lines of sight through a state of the art radiation hydrodynamics UV line driven disc wind simulation. We demonstrate that there are some lines of sight which only intercept highly ionised and fast outflowing material. The cooler material required for the UV line driving acceleration is out of the line of sight, close to the disc, shielded from the X-rays by a failed wind. We fit these simulated wind spectra to data from the archetypal UFO source PG 1211+143 and show that they broadly reproduce the depth and velocity of the iron absorption lines seen. This directly demonstrates that UV line driving is a viable mechanism to launch even the fastest UFOs. We simulate microcalorimeter observations of this wind and show that their high energy resolution can resolve the detailed structure in the wind and recover the wind energetics when combined with models which correctly estimate the line formation radius of the wind. New data from microcalorimeters will pave the way for physical predictions of AGN wind feedback in cosmological simulations.

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supporting

confidence: 72%

UV line-driven disc wind as the origin of UltraFast Outflows in AGN

Mizumoto

Nomura

Done

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…Simulations predict that the winds launched by accretion discs should be largely equatorial (e.g. Proga, Stone & Kallman 2000;Proga & Kallman 2004;Nomura et al 2016); there is clear evidence that this is the case for X-ray binaries (Ponti et al 2012), and there is also some evidence that AGN outflow properties are inclination dependent (Parker et al 2018). As the inclination inferred from the reflection spectrum is fairly modest here, the true outflow velocity could yet be slightly larger owing to projection effects.…”

Section: Ionised Absorptionmentioning

confidence: 76%

A full characterization of the supermassive black hole in IRAS 09149–6206

Walton

Alston

Kosec

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present new broadband X-ray observations of the type-I Seyfert galaxy IRAS 09149–6206, taken in 2018 with XMM-Newton, NuSTAR and Swift. The source is highly complex, showing a classic ‘warm’ X-ray absorber, additional absorption from highly ionised iron, strong relativistic reflection from the innermost accretion disc and further reprocessing by more distant material. By combining X-ray timing and spectroscopy, we have been able to fully characterise the supermassive black hole in this system, constraining both its mass and – for the first time – its spin. The mass is primarily determined by X-ray timing constraints on the break frequency seen in the power spectrum, and is found to be log [MBH/M⊙] = 8.0 ± 0.6 (1σ uncertainties). This is in good agreement with previous estimates based on the Hα and Hβ line widths, and implies that IRAS 09149–6206 is radiating at close to (but still below) its Eddington luminosity. The spin is constrained via detailed modelling of the relativistic reflection, and is found to be $a^* = 0.94^{+0.02}_{-0.07}$ (90% confidence), adding IRAS 09149–6206 to the growing list of radio-quiet AGN that host rapidly rotating black holes. The outflow velocities of the various absorption components are all relatively modest (vout ≲ 0.03c), implying these are unlikely to drive significant galaxy-scale AGN feedback.

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“…This geometry is widely used in geometric unification and BAL outflow models (e.g. Murray et al 1995;de Kool & Begelman 1995;Elvis 2000;Proga et al 2000;Risaliti & Elvis 2010;Proga & Kallman 2004;Borguet & Hutsemékers 2010;Higginbottom et al 2013;Nomura et al 2013Nomura et al , 2016.…”

Section: Resultsmentioning

confidence: 99%

Quasar emission lines as probes of orientation: implications for disc wind geometries and unification

Matthews

Knigge

Long

2017

Mon. Not. R. Astron. Soc.

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The incidence of broad absorption lines (BALs) in quasar samples is often interpreted in the context of a geometric unification model consisting of an accretion disc and an associated outflow. We use the the Sloan Digital Sky Survey (SDSS) quasar sample to test this model by examining the equivalent widths (EWs) of C iv 1550Å, Mg ii 2800Å, [O iii] 5007Å and C iii] 1909Å. We find that the emission line EW distributions in BAL and non-BAL quasars are remarkably similar -a property that is inconsistent with scenarios in which a BAL outflow rises equatorially from a geometrically thin, optically thick accretion disc. We construct simple models to predict the distributions from various geometries; these models confirm the above finding and disfavour equatorial geometries. We show that obscuration, line anisotropy and general relativistic effects on the disc continuum are unlikely to hide an EW inclination dependence. We carefully examine the radio and polarisation properties of BAL quasars. Both suggest that they are most likely viewed (on average) from intermediate inclinations, between type 1 and type 2 AGN. We also find that the low-ionization BAL quasars in our sample are not confined to one region of 'Eigenvector I' parameter space. Overall, our work leads to one of the following conclusions, or some combination thereof: (i) the continuum does not emit like a geometrically thin, optically thick disc; (ii) BAL quasars are viewed from similar angles to non-BAL quasars, i.e. low inclinations; (iii) geometric unification does not explain the fraction of BALs in quasar samples.

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Radiation hydrodynamic simulations of line-driven disk winds for ultra-fast outflows

Cited by 77 publications

References 36 publications

UV line-driven disc wind as the origin of UltraFast Outflows in AGN

UV line-driven disc wind as the origin of UltraFast Outflows in AGN

A full characterization of the supermassive black hole in IRAS 09149–6206

Quasar emission lines as probes of orientation: implications for disc wind geometries and unification

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