Black hole winds

By A. King, K. H. U. O. Leicester, UK., H. C. F. Astrophysics, Cambridge, Ma, Usa. 2003

314 citations recorded by the source corpus.

Also available at http://www.blackwell-synergy.com/doi/abs/10.1046/j.1365-8711.2003.06980.x. The definitive version is available at www.blackwell-synergy.com.

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Citations in the corpus

UNLEASHING POSITIVE FEEDBACK: LINKING THE RATES OF STAR FORMATION, SUPERMASSIVE BLACK HOLE ACCRETION, AND OUTFLOWS IN DISTANT GALAXIES (2013, background): “…4πR2dc = fEGMBHΣd Mdκ , (3) where the Eddington luminosity is LE = 4πGcMBH κ , (4) the Eddington accretion rate (or the black hole growth rate at Eddington luminosity) is ṀE = ṀBH/fE = LE ηc2 = 4π GMBH cηκ , (5) and the wind outflow rate from the AGN disk is (King & Pounds 2003) Ṁw = fE LE vwc .”
Black Hole Outflows (2009, methodology): “As expected, using this value of v in the mass conservation equation Ṁout = 4πbR2vρ(R), (9) where ρ(R) is the mass density, self-consistently shows that the optical depth τ of the wind is ∼1 (cf. King & Pounds 2003, equation 4).”
Heating cooling flows with jets (2003, background): “While these outflows are suggestive, they are not directly relevant to the systems of interest here because they are observed in objects with comparable photon luminosities and they may be radiatively driven (King & Pounds 2003).”
DISCOVERY OF ULTRA-FAST OUTFLOWS IN A SAMPLE OF BROAD-LINE RADIO GALAXIES OBSERVED WITH SUZAKU (2010, background): “These two sources are emitting closer to their Eddington limits and therefore are more capable of producing powerful outflows/ejecta that would eventually leave the system (e.g., King & Pounds 2003; King 2010).”
On why the iron K-shell absorption in AGN is not a signature of the local warm/hot intergalactic medium (2008, background): “Its high velocity means that its kinetic energy can be comparable to the bolometric radiated luminosity of the AGN (King & Pounds 2003; Pounds et al 2003; Pounds & Reeves 2007), yet its high ionisation means that it is effectively invisible in all other wavebands.”
Multidimensional modelling of X-ray spectra for AGN accretion disc outflows (2008, background): “However, we notethat the wind model does clearly lead to an excess of emission below ∼ 1 keV suggesting that reprocessing by the fast flow may account for a modest fraction of the excess soft-energy emission (c.f. King & Pounds 2003).”
EVIDENCE FOR ULTRA-FAST OUTFLOWS IN RADIO-QUIET ACTIVE GALACTIC NUCLEI. II. DETAILED PHOTOIONIZATION MODELING OF Fe K-SHELL ABSORPTION LINES (2011, background): “The electron temperature of kT∼100 eV (see §2.2) then suggests the continuum emission might be mainly in the soft Xrays (e.g., King & Pounds 2003; Pounds & Reeves 2007; Sim et al. 2008; Sim et al. 2010 and references therein).”
Unification of X-ray winds in Seyfert galaxies: from ultra-fast outflows to warm absorbers (2012, background): “The alternative scenario in which radiation pressure could provide significant acceleration to this material even if it is highly ionized is then through Compton scattering (e.g., King & Pounds 2003; King 2010a, b).”
Evidence for ultra-fast outflows in radio-quiet AGNs - I. Detection and statistical incidence of Fe K-shell absorption lines (2010, background): “Detailed theoretical studies of accretion disk winds in AGNs showed that the inner regions of the outflowing material can be highly ionized by the intense nuclear radiation and can have large outflow velocities (e.g., King & Pounds 2003; Proga & Kallman 2004; Ohsuga et al. 2009; King 2010).”
A high-velocity ionized outflow and XUV photosphere in the narrow emission line quasar PG1211+143 (2003, background): “A wide angle outflow is indicated by the strength and low projected velocity of the OVII emission line (Section 4.1), corresponding to case 1 in King and Pounds 2003, where the flow geometry limits the leakage of photons from the side of the cone.”
The Suzaku View of Highly Ionized Outflows in AGN. 1; Statistical Detection and Global Absorber Properties (2012, background): “…and their energetic output are of vital importance when it comes to studying how the interplay between the accretion and ejection flows at small radii can affect the host galaxy on larger scales (e.g. Ferrarese & Merritt 2000; King & Pounds 2003; Sazonov et al. 2005; Ciotti, Ostriker & Proga 2009).”
The multi-phase winds of Markarian 231: from the hot, nuclear, ultra-fast wind to the galaxy-scale, molecular outflow (2015, background): “The momentum load of the nuclear wind, ṖUFO/(Lbol,AGN/c) = 0.2 − 1.6, agrees with the predictions for radiatively accelerated winds with scattering optical depth ∼ 1 (King & Pounds 2003).”
Evidence of a high-velocity ionized outflow in a second narrow-line quasar PG 0844+349 (2003, methodology): “…implications of the observed high-velocity outflow, which we assess below in terms of a physical model of winds from black holes accreting at or above the Eddington limit (King & Pounds 2003, hereafter KP03), are a significant mass loss and substantial kinetic energy associated with the outflow.”
Chandra/High Energy Transmission Grating Spectrometer Spectroscopy of the Galactic Black Hole GX 339–4: A Relativistic Iron Emission Line and Evidence for a Seyfert-like Warm Absorber (2003, unknown): “In contrast to a recent model for AGN spectra that relies on an optically thick outflow (King & Pounds 2003); it is clear that any disk-driven outflow in GX 339 4 and XTE J1650 500 must be optically thin.”
XMM–Newton observations of the brightest ultraluminous X-ray sources (2006, background): “The physical motivation for the soft component comes from the suggestion that optically-thick outflowing winds from BHs accreting at or above the Eddington limit could explain ultrasoft components in ULXs (King & Pounds 2003).”
The physics of galactic winds driven by active galactic nuclei (2012, background): “The electron scattering optical depth around black holes accreting near the Eddington limit is furthermore naturally τes ∼ 1 (e.g., King & Pounds 2003).”
CLEARING OUT A GALAXY (2012, background): “With mass rate Ṁw ∼ ṀEdd, where ṀEdd = LEdd/ηc 2 is the Eddington accretion rate and η is the accretion efficiency, 2 a wide–angle wind has scattering optical depth ∼ 1 (King & Pounds 2003), assuming that the covering factor of absorbing gas is close to unity (see the discussion below eqn 2).”
Powerful Outflows and Feedback from Active Galactic Nuclei (2015, background): “The observed distributions of velocity, ionization parameter and column density are compatible with Eddington winds launched from close to the black hole, where the optical depth τes ∼ 1, and carrying the local escape velocity (King & Pounds 2003).”
Supercritically accreting stellar mass black holes as ultraluminous X-ray sources (2006, background): “Because the outflow is optically thick at most radii and the radiation is partially trapped (see below), it isenergy-driven (not momentum-driven as was assumed by King & Pounds 2003), and its kinetic luminosity can exceedLEdd.”