期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 466, 期 2, 页码 1462-1476出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw2777
关键词
black hole physics; methods: numerical; galaxies: active; galaxies: haloes quasars: general
资金
- ISF [24/12, 1829/12]
- GIF [G-1052-104.7/2009]
- DIP
- I-CORE Program of the PBC
- NSF [AST-1010033, AST-1405962]
- E.C. through an ERC grant [StG-257720]
- GENCI [04-2192]
High-resolution simulations of supermassive black holes in isolated galaxies have suggested the importance of short (similar to 10 Myr) episodes of rapid accretion caused by interactions between the black hole and massive dense clouds within the host. Accretion of such clouds could potentially provide the dominant source for black hole growth in high-z galaxies, but it remains unresolved in cosmological simulations. Using a stochastic subgrid model calibrated by high-resolution isolated galaxy simulations, we investigate the impact that variability in black hole accretion rates has on black hole growth and the evolution of the host galaxy. We find this clumpy accretion to more efficiently fuel high-redshift black hole growth. This increased mass allows for more rapid accretion even in the absence of high-density clumps, compounding the effect and resulting in substantially faster overall black hole growth. This increased growth allows the black hole to efficiently evacuate gas from the central region of the galaxy, driving strong winds up to similar to 2500 km s(-1), producing outflows similar to 10 x stronger than the smooth accretion case, suppressing the inflow of gas on to the host galaxy, and suppressing the star formation within the galaxy by as much as a factor of 2. This suggests that the proper incorporation of variability is a key factor in the co-evolution between black holes and their hosts.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据