Radiation hydrodynamics simulations of line-driven AGN disc winds: Metallicity dependence and black hole growth

Mariko Nomura, Kazuyuki Omukai, Ken Ohsuga

研究成果: ジャーナルへの寄稿学術論文査読

3 被引用数 (Scopus)

抄録

Growth of the black holes (BHs) from the seeds to supermassive BHs (SMBHs, ∼109M⊙) is not understood, but the mass accretion must have played an important role. We performed 2D radiation hydrodynamics simulations of line-driven disc winds considering the metallicity dependence in a wide range of the BH mass, and investigated the reduction of the mass accretion rate due to the wind mass-loss. Our results show that denser and faster disc winds appear at higher metallicities and larger BH masses. The accretion rate is suppressed to ∼0.4-0.6 times the mass supply rate to the disc for the BH mass of MBH ≳ 105M⊙ in high-metallicity environments of Z ≳ Z⊙, while the wind mass-loss is negligible when the metallicity is subsolar (∼0.1Z⊙). By developing a semi-analytical model, we found that the metallicity dependence of the line force and the BH mass dependence of the surface area of the wind launch region are the cause of the metallicity dependence (∝ Z2/3) and BH mass dependencies (∝M4/3BH for MBH ≤ 106M⊙ and ∝ MBH for MBH ≥ 106M⊙) of the mass-loss rate. Our model suggests that the growth of BHs by the gas accretion effectively slows down in the regime ≳ 105M⊙ in metal-enriched environments ≳ Z⊙. This means that the line-driven disc winds may have an impact on late evolution of SMBHs.

本文言語英語
ページ(範囲)904-913
ページ数10
ジャーナルMonthly Notices of the Royal Astronomical Society
507
1
DOI
出版ステータス出版済み - 2021 10月 1

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