http://arxiv.org/abs/1811.01966
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.
M. Nomura, K. Ohsuga and C. Done
Wed, 7 Nov 18
53/94
Comments: 8 pages, 6 figures, submitted to MNRAS
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