Astronomy and Astrophysics – Astrophysics – Cosmology and Extragalactic Astrophysics
Scientific paper
2009-11-05
Astronomy and Astrophysics
Astrophysics
Cosmology and Extragalactic Astrophysics
15 pages, 9 figures. Accepted for publication in Astronomy & Astrophysics
Scientific paper
We present a study of the acceleration phase of line-driven winds in AGNs, in order to examine the physical conditions for the existence of such winds for a wide variety of initial conditions. We built a simple and fast non-hydrodynamic model, QWIND, where we assume that a wind is launched from the accretion disc at supersonic velocities of the order of a few 10^2 km/s and we concentrate on the subsequent supersonic phase. We show that this model can produce a wind with terminal velocities of the order of 10^4 km/s. There are three zones in the wind, only the middle one of which can launch a wind: in the inner zone the wind is too ionized and so experiences only the Compton radiation force which is not effective in accelerating gas. This inner failed wind however plays an important role in shielding the next zone, lowering the ionization parameter there. In the middle zone the lower ionization of the gas leads to a much larger radiation force and the gas achieves escape velocity This middle zone is quite thin (about 100 gravitational radii). The outer, third, zone is shielded from the UV radiation by the central wind zone and so does not achieve a high enough acceleration to reach escape velocity. We also describe a simple analytic approximation of our model, based on neglecting the effects of gravity during the acceleration phase. This analytic approach is in agreement with the results of the numerical code, and is a powerful way to check whether a radiation driven wind can be accelerated with a given set of initial parameters. Our analytical analysis and the fast QWIND model are in agreement with more complex hydrodynamical models, and allow an exploration of the dependence of the wind properties for a wide set of initial parameters: black hole mass, Eddington ratio, initial density profile, X-ray to UV ratio.
Elvis Martin
Risaliti Guido
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