Qwind code release. A non-hydrodynamical approach to modelling line-driven winds in active galactic nuclei. (arXiv:2001.04720v1 [astro-ph.HE])

Qwind code release. A non-hydrodynamical approach to modelling line-driven winds in active galactic nuclei. (arXiv:2001.04720v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Quera_Bofarull_A/0/1/0/all/0/1">Arnau Quera-Bofarull</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Done_C/0/1/0/all/0/1">Chris Done</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lacey_C/0/1/0/all/0/1">Cedric Lacey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McDowell_J/0/1/0/all/0/1">Jonathan C. McDowell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Risaliti_G/0/1/0/all/0/1">Guido Risaliti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Elvis_M/0/1/0/all/0/1">Martin Elvis</a>

UV line driven winds may be an important part of the AGN feedback process,
but understanding their impact is hindered by the complex nature of the
radiation hydrodynamics. Instead, we have taken the approach pioneered by
Risaliti & Elvis, calculating only ballistic trajectories from radiation forces
and gravity, but neglecting gas pressure. We have completely re-written their
QWIND code using more robust algorithms, and can now quickly model the
acceleration phase of these winds for any AGN spectral energy distribution
spanning UV and X-ray wavebands. We demonstrate the code using an AGN with
black hole mass $10^8, M_odot$ emitting at half the Eddington rate and show
that this can effectively eject a wind with velocities $simeq (0.1-0.2), c$.
The mass loss rates can be up to $simeq 0.3 M_odot$ per year, consistent with
more computationally expensive hydrodynamical simulations, though we highlight
the importance of future improvements in radiation transfer along the multiple
different lines of sight illuminating the wind. The code is fully public, and
can be used to quickly explore the conditions under which AGN feedback can be
dominated by accretion disc winds.

UV line driven winds may be an important part of the AGN feedback process,
but understanding their impact is hindered by the complex nature of the
radiation hydrodynamics. Instead, we have taken the approach pioneered by
Risaliti & Elvis, calculating only ballistic trajectories from radiation forces
and gravity, but neglecting gas pressure. We have completely re-written their
QWIND code using more robust algorithms, and can now quickly model the
acceleration phase of these winds for any AGN spectral energy distribution
spanning UV and X-ray wavebands. We demonstrate the code using an AGN with
black hole mass $10^8, M_odot$ emitting at half the Eddington rate and show
that this can effectively eject a wind with velocities $simeq (0.1-0.2), c$.
The mass loss rates can be up to $simeq 0.3 M_odot$ per year, consistent with
more computationally expensive hydrodynamical simulations, though we highlight
the importance of future improvements in radiation transfer along the multiple
different lines of sight illuminating the wind. The code is fully public, and
can be used to quickly explore the conditions under which AGN feedback can be
dominated by accretion disc winds.

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