Forming supermassive black holes by accreting dark and baryon matter
Hu, J; Shen, Y; Lou, YQ; Zhang, SN; Zhang SN(张双南)
刊名MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
2006
卷号365期号:1页码:345-351
关键词accretion, accretion discs black hole physics galaxies : formation quasars : general cosmology : theory dark matter
学科分类Astronomy & Astrophysics
DOI10.1111/j.1365-2966.2005.09712.x
通讯作者Tsing Hua Univ, Dept Phys, Beijing 100084, Peoples R China ; Tsing Hua Univ, Tsinghua Ctr Astrophys, Beijing 100084, Peoples R China ; Chinese Acad Sci, Inst High Energy Phys, Beijing 100039, Peoples R China ; Natl Space Sci & Technol Ctr, Huntsville, AL 35805 USA ; Univ Alabama, Dept Phys, Huntsville, AL 35899 USA ; Princeton Univ, Dept Astrophys Sci, Princeton, NJ 08544 USA ; Chinese Acad Sci, Natl Astron Observ China, Beijing 100012, Peoples R China ; Univ Chicago, Dept Astron & Astrophys, Chicago, IL 60637 USA ; CNRS, CPM, Inst Natl Phys Nucl & Phys Particules, F-13288 Marseille 09, France ; Univ Mediterrannee Aix Marseille II, F-13288 Marseille 09, France
文章类型Article
英文摘要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.
类目[WOS]Astronomy & Astrophysics
研究领域[WOS]Astronomy & Astrophysics
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语种英语
WOS记录号WOS:000234853400037
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被引频次:23[WOS]   [WOS记录]     [WOS相关记录]
文献类型期刊论文
条目标识符http://ir.ihep.ac.cn/handle/311005/237076
专题中国科学院高能物理研究所_粒子天体物理中心_期刊论文
作者单位中国科学院高能物理研究所
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Hu, J,Shen, Y,Lou, YQ,et al. Forming supermassive black holes by accreting dark and baryon matter[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2006,365(1):345-351.
APA Hu, J,Shen, Y,Lou, YQ,Zhang, SN,&张双南.(2006).Forming supermassive black holes by accreting dark and baryon matter.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,365(1),345-351.
MLA Hu, J,et al."Forming supermassive black holes by accreting dark and baryon matter".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 365.1(2006):345-351.
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