Line-driven disc wind in near-Eddington active galactic nuclei: decrease of mass accretion rate due to powerful outflow. (arXiv:1811.01966v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Nomura_M/0/1/0/all/0/1">Mariko Nomura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ohsuga_K/0/1/0/all/0/1">Ken Ohsuga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Done_C/0/1/0/all/0/1">Chris Done</a>
Ultrafast winds from supermassive black holes are observed to be powerful
enough to dramatically affect their host galaxy but their launch and
acceleration mechanisms are not well understood. We perform two-dimensional
radiation hydrodynamics simulations of UV line-driven disc winds in order to
calculate the mass loss rates and kinetic power in these models. We develop a
new iterative technique which self consistently reduces the mass accretion rate
through the inner disc in response to the wind mass loss. This makes the inner
disc is less UV bright, reducing the wind power compared to previous
simulations which assumed a constant accretion rate with radius. The
line-driven winds in our simulations are still extremely powerful, with around
half the supplied mass accretion rate being ejected in the wind for black holes
with mass $10^8$-$10^{10},M_odot$ accreting at $L/L_{rm Edd}=0.5$-$0.9$. Our
results open up the way for a physical rather than phenomenological model for
active galactic nuclei feedback via UV line-driven winds.
Ultrafast winds from supermassive black holes are observed to be powerful
enough to dramatically affect their host galaxy but their launch and
acceleration mechanisms are not well understood. We perform two-dimensional
radiation hydrodynamics simulations of UV line-driven disc winds in order to
calculate the mass loss rates and kinetic power in these models. We develop a
new iterative technique which self consistently reduces the mass accretion rate
through the inner disc in response to the wind mass loss. This makes the inner
disc is less UV bright, reducing the wind power compared to previous
simulations which assumed a constant accretion rate with radius. The
line-driven winds in our simulations are still extremely powerful, with around
half the supplied mass accretion rate being ejected in the wind for black holes
with mass $10^8$-$10^{10},M_odot$ accreting at $L/L_{rm Edd}=0.5$-$0.9$. Our
results open up the way for a physical rather than phenomenological model for
active galactic nuclei feedback via UV line-driven winds.
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