期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 440, 期 2, 页码 1551-1561出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stu357
关键词
methods: numerical; galaxies: formation; cosmology: theory; early Universe
资金
- Deutsche Forschungsgemeinschaft (DFG) [SFB 963/1]
- HLRN [nip00029]
- DFG via the Schwerpunktprogram [SPP 1573, SCHL 1964/1 - 1]
Observations of quasars at z > 6 report the existence of a billion solar mass black holes. Comprehending their formation in such a short time-scale is a matter of ongoing research. One of the most promising scenarios to assemble supermassive black holes is a monolithic collapse of protogalactic gas clouds in atomic cooling haloes with T-vir >= 10(4) K. In this paper, we study the amplification and impact of magnetic fields during the formation of seed black holes in massive primordial haloes. We perform high-resolution cosmological magnetohydrodynamic simulations for four distinct haloes and follow their collapse for a few free-fall times until the simulations reach a peak density of 7 x 10(-10) g cm(-3). Our findings show that irrespective of the initial seed field, the magnetic field strength reaches a saturated state in the presence of strong accretion shocks. Under such conditions, the growth time becomes very short and amplification occurs rapidly within a small fraction of the free-fall time. We find that the presence of such strong magnetic fields provides additional support against gravity and helps in suppressing fragmentation. Massive clumps of a few hundred solar masses are formed at the end of our simulations and high accretion rates of 1 M-circle dot yr(-1) are observed. We expect that in the presence of such accretion rates, the clumps will grow to form supermassive stars of similar to 10(5) M-circle dot. Overall, the role of the magnetic fields seems supportive for the formation of massive black holes.
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