期刊
ASTROPHYSICAL JOURNAL
卷 754, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/754/2/125
关键词
accretion, accretion disks; black hole physics; galaxies: active; galaxies: nuclei; galaxies: starburst; quasars: general
资金
- NSF [AST-0707505]
- DFG cluster of excellence Origin and Structure of the Universe
- Samsung Scholarship foundation
- University of Helsinki
- DFG [SPP1177]
- Direct For Mathematical & Physical Scien
- Division Of Mathematical Sciences [1040196] Funding Source: National Science Foundation
We study the growth of black holes (BHs) in galaxies using three-dimensional smoothed particle hydrodynamic simulations with new implementations of the momentum mechanical feedback, and restriction of accreted elements to those that are gravitationally bound to the BH. We also include the feedback from the X-ray radiation emitted by the BH, which heats the surrounding gas in the host galaxies, and adds radial momentum to the fluid. We perform simulations of isolated galaxies and merging galaxies and test various feedback models with the new treatment of the Bondi radius criterion. We find that overall the BH growth is similar to what has been obtained by earlier works using the Springel, Di Matteo, & Hernquist algorithms. However, the outflowing wind velocities and mechanical energy emitted by winds are considerably higher (upsilon(w) similar to 1000-3000 km s(-1)) compared to the standard thermal feedback model (upsilon(w) similar to 50-100 km s(-1)). While the thermal feedback model emits only 0.1% of BH released energy in winds, the momentum feedback model emits more than 30% of the total energy released by the BH in winds. In the momentum feedback model, the degree of fluctuation in both radiant and wind output is considerably larger than in standard treatments. We check that the new model of BH mass accretion agrees with analytic results for the standard Bondi problem.
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