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	Forming supermassive black holes by accreting dark and baryon matter
	Hu, J ; Shen, Y ; Lou, YQ ; Zhang, SN
	2010-05-06 ; 2010-05-06
关键词	accretion, accretion discs black hole physics galaxies : formation quasars : general cosmology : theory dark matter BH-SIGMA RELATION ACTIVE GALACTIC NUCLEI BULGE MASS RELATION DIGITAL SKY SURVEY HIGH-REDSHIFT HOST GALAXY GROWTH QUASARS CONSTRAINTS DISCOVERY Astronomy & Astrophysics
中文摘要	Given a large-scale mixture of self-interacting dark matter (SIDM) particles and baryon matter distributed in the early Universe, we advance here a two-phase accretion scenario for forming supermassive black holes (SMBHs) with masses around similar to 10(9) M-. at high redshifts z(greater than or similar to 6). The first phase is conceived to involve a rapid quasi-spherical and quasi-steady Bondi accretion of mainly SIDM particles embedded with baryon matter on to seed black holes (BHs) created at redshifts z less than or similar to 30 by the first generation of massive Population III stars; this earlier phase rapidly gives birth to significantly enlarged seed BH masses of M-BH, t(1) similar or equal to 1.4 x 10(6) M-. sigma(0)/( 1 cm(2) g(-1))(C-s/30 km s(-1))(4) during z similar to 20 - 15, where sigma(0) is the cross-section per unit mass of SIDM particles and C-s is the velocity dispersion in the SIDM halo referred to as an effective 'sound speed'. The second phase of BH mass growth is envisaged to proceed primarily via baryon accretion, eventually leading to SMBH masses of M-BH similar to 10(9) M-.; such SMBHs may form either by z similar to 6 for a sustained accretion at the Eddington limit or later at lower z for sub-Eddington mean accretion rates. In between these two phases, there is a transitional yet sustained diffusively limited accretion of SIDM particles which in an eventual steady state would be much lower than the accretion rates of the two main phases. We intend to account for the reported detections of a few SMBHs at early epochs, e. g. Sloan Digital Sky Survey (SDSS) 1148+ 5251 and so forth, without necessarily resorting to either super-Eddington baryon accretion or very frequent BH merging processes. Only extremely massive dark SIDM haloes associated with rare peaks of density fluctuations in the early Universe may harbour such early SMBHs or quasars. Observational consequences are discussed. During the final stage of accumulating a SMBH mass, violent feedback in circumnuclear environs of a galactic nucleus leads to the central bulge formation and gives rise to the familiar empirical M-BH - sigma(b) correlation inferred for nearby normal galaxies with sigma(b) being the stellar velocity dispersion in the galactic bulge; in our scenario, the central SMBH formation precedes that of the galactic bulge.
语种	英语 ; 英语
出版者	BLACKWELL PUBLISHING ; OXFORD ; 9600 GARSINGTON RD, OXFORD OX4 2DQ, OXON, ENGLAND
内容类型	期刊论文
源URL	[http://hdl.handle.net/123456789/15157]
专题	清华大学
推荐引用方式 GB/T 7714	Hu, J,Shen, Y,Lou, YQ,et al. Forming supermassive black holes by accreting dark and baryon matter[J],2010, 2010.
APA	Hu, J,Shen, Y,Lou, YQ,&Zhang, SN.(2010).Forming supermassive black holes by accreting dark and baryon matter..
MLA	Hu, J,et al."Forming supermassive black holes by accreting dark and baryon matter".(2010).

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