Line-driven disc wind in near-Eddington active galactic nuclei: decrease of mass accretion rate due to powerful outflow

Abstract

Based on recent X-ray observations, ultra-fast outflows from supermassive black holes are expected to have enough energy 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 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-$$10^{10}{M}_{\odot }$ accreting at $L/L_{\mathrm{Edd}}=0.5-$$0.9$. Our results open up the way for estimating the growth rate of supermassive black hole and evaluating the kinetic energy ejected into the inter stellar medium (active galactic nuclei feedback) based on a physical model of line-driven disc winds.

12 pages, 7 figures, accepted for publication in MNRAS

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