Dynamics of Line-driven Disk Winds in Active Galactic Nuclei. II. Effects of Disk Radiation

By D. Proga, T. R. K. Jila, U. Colorado, Boulder, Co., GSFC-NASA, Greenbelt, Md.. 2000

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We explore consequences of a radiation-driven disk wind model for mass outflows from active galactic nuclei (AGNs). We performed axisymmetric time-dependent hydrodynamic calculations using the same computational technique as Proga, Stone, and Kallman. We test the robustness of radiation launching and acceleration of the wind for relatively unfavorable conditions. In particular, we take into account the central engine radiation as a source of ionizing photons but neglect its contribution to the radiation force. In addition, we account for the attenuation of the X-ray radiation by computing the X-ray optical depth in the radial direction assuming that only electron scattering contributes to the opacity. Our new simulations confirm the main result from our previous work: the disk atmosphere can "shield" itself from external X-rays so that the local disk radiation can launch gas off the disk photosphere. We also find that the local disk force suffices to accelerate the disk wind to high velocities in the radial direction. This is true provided the wind does not significantly change the geometry of the disk radiation by continuum scattering and absorption processes; we discuss plausibility of this requirement. Synthetic profiles of a typical resonance ultraviolet line predicted by our models are consistent with observations of broad absorption line (BAL) QSOs.

Subfields: Astronomy and Astrophysics

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UNIFICATION OF LUMINOUS TYPE 1 QUASARS THROUGH C iv EMISSION (2010, background): “We emphasize that the rapid growth (and general acceptance) of the disk-wind model (e.g., Murray et al. 1995; Elvis 2000; Proga et al. 2000) postdates much of the work on the BELR (including Boroson & Green 1992).”
An Exploratory Chandra Survey of a Well-defined Sample of 35 Large Bright Quasar Survey Broad Absorption Line Quasars (2006, background): “The more complex hydrodynamic wind models presented in Proga et al. (2000) and Proga & Kallman (2004) do not make specific predictions for the relationship between absorption onset velocity and X-ray absorption column density (D. Proga, 2005, priv. comm.), and so it is unclear if they are…”
Accretion disk wind in the AGN broad-line region: Spectroscopically resolved line profile variations in Mrk 110 ? (2003, background): “They investigated radiatively-driven wind models (e.g. Murray & Chiang 1997; Proga et al. 2000) and/or magnetically-driven disk outflow models (Blandford & Payne 1982; Bottorff et al. 1997; Emmering et al. 1992; K¨onigl & Kartje 1994).”
A high-velocity ionized outflow and XUV photosphere in the narrow emission line quasar PG1211+143 (2003, background): “Models in which the BAL gas is launched more or less vertically off a disk and then accelerated by radiation pressure (Murray et al. 1995; Proga et al. 2000) are reasonably consistent with the UV data but have difficulty in accelerating the large columns of material seen in X-rays unless they are…”
Unusual Broad Absorption Line Quasars from the Sloan Digital Sky Survey (2002, background): “Stable disk winds are often invoked to explain the observed lack of velocity variability in BAL outflows, but disk winds may not be particularly stable (e.g., Proga et al. 2000).”
Multidimensional modelling of X-ray spectra for AGN accretion disc outflows (2008, background): “Hydrodynamical simulationshave demonstrated that such flows are plausible (e.g. Proga & Kallman 2004).”
Observations of feedback from radio-quiet quasars - I. Extents and morphologies of ionized gas nebulae (2013, background): “One option is that the gas is being expelled from the galaxy, presumably driven by the radiative pressure of the quasar itself (Murray et al. 1995; Proga et al. 2000).”
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).”
The physics of galactic winds driven by active galactic nuclei (2012, background): “In addition to radiation pressure on electrons and on dust, radiation pressure on UV lines (e.g., Murray et al. 1995; Proga et al. 2000), hydromagnetic processes (e.g., Emmering et al. 1992; Konigl & Kartje 1994), and Compton heating (e.g., Sazonov et al. 2005) may contribute to accelerating…”
FEEDBACK FROM CENTRAL BLACK HOLES IN ELLIPTICAL GALAXIES: TWO-DIMENSIONAL MODELS COMPARED TO ONE-DIMENSIONAL MODELS (2010, background): “These winds are launched by electromagnetic processes within a few hundred gravitational radii of the central BH (e.g., Proga et al. 2000), but by the time the wind galactic length scales, the energy is carried by the kinetic motion of the gas.”
Unification of X-ray winds in Seyfert galaxies: from ultra-fast outflows to warm absorbers (2012, background): “Thus, the UFOs are possibly directly identifiable, at least qualitatively, with accretion disc winds/outflows (King & Pounds 2003; Proga & Kallman 2004; Ohsuga et al. 2009; Sim et al. 2010; Fukumura et al. 2010) or the base of a possible weak jet (e.g. Ghisellini et al. 2004).”
The Compact, Conical, Accretion-Disk Warm Absorber of the Seyfert 1 Galaxy NGC 4051 and Its Implications for IGM-Galaxy Feedback Processes (2007, background): “We suggested, however, that we are not seeing the full terminal velocity of the wind (§8; Proga & Kallman 2004; Elvis 2000).”
Systematic effects in measurement of black hole masses by emission-line reverberation of active galactic nuclei: Eddington ratio and inclination (2006, background): “Key papers on the topic of disk winds are by Murray & Chiang (1995, 1998) and by Proga & Kallman (2004).”
Quasar outflows and AGN feedback in the extreme UV: HST/COS observations of HE 0238−1904 (2013, background): “…troughs of singly ionized species as Fe ii or Si ii (e.g. Korista et al. 2008; Moe et al. 2009; Dunn et al. 2010b), but they are 4+ orders of magnitude farther away than the assumed acceleration region (0.03–0.1 pc) of line driven winds in quasars (e.g. Murray et al. 1995; Proga et al. 2000).”
Quasar feedback and the origin of radio emission in radio-quiet quasars (2014, background): “Furthermore, the [OIII] width positively correlates with mid-infrared luminosity (Figure 11), which we take to suggest that the outflow is ultimately driven by the radiative pressure near the quasar (Murray et al. 1995; Proga et al. 2000).”
FEEDBACK IN LUMINOUS OBSCURED QUASARS (2011, background): “The velocities in broad absorption lines are high (∼ 10,000 km s−1), and they most likely emerge from a wind blown off of the accretion disk (e.g., Proga & Kallman 2004).”