Formation of Massive Black Holes in an Early Universe and Cosmological Consequences

研究了宇宙重组后不久宇宙背景辐射（CBR）对早期形成天体辐射力的影响。CBR辐射力的计算是通过求解辐射传递方程，包括汤姆逊散射，假设一个磁盘是局部近似为一个平面平行介质的纵向运动。结果表明，即使辐射扩散有效，CBR提取角动量的效率也随光学深度呈指数下降。由于目前的影响，早期形成的盘的自旋概率分布可能会在强CBR的存在下显着修改。此外，CBR力可能有助于增强剪切粘度的影响，从而使种子黑洞的形式在z>10解释类星体的形成。此外，我们已经检查了一个人口的遗迹大质量黑洞，也许构成了一个重要的COM ...更多信息 暗物质的组成部分，可以通过它们偶尔对遥远的外部星系中个别发光恒星的非常强的引力透镜效应间接检测到。对于合理的，在某些方面保守的，相关的物理参数的值，我们表明，这样的事件可能会被检测到，无论是在大面积的调查达到常规CCD星等限制（如斯隆数字巡天）或在小领域，非常深的图像（如HDF）。因此，探测或限制大质量黑洞遗迹的数量将是一项具有挑战性但并非不可能的任务。此外，我们提出了一种新的活动星系核（AGN）燃料机制，即，辐射雪崩，这是质量吸积驱动的辐射阻力所施加的恒星辐射从环核星暴地区。如果旋转气体盘的表面层受到强烈的星光照射，那么它可能会通过辐射阻力失去角动量，从而导致层的雪崩是不可避免的结果。分析表明，在光学厚区，通过辐射雪崩产生的质量吸积率不仅与吸收光子物质的消光系数有关，而且与星盘的密度分布有关，最大质量吸积率可简单地表示为M-L_m/c^2，其中L_m为星暴的热光度。在目前的背景下，辐射雪崩的强度决定了一个星暴星系是否注定要成为活动星系核。目前的模型提供了一个坚实的物理机制推导出的第一性原理，占星爆活动和活动星系核之间的可能联系，这已经提出了一些观测。少

The effects of radiation force by the cosmic background radiation (CBR) on early-formed objects shortly after the cosmological recombination have been explored. The radiation force by the CBR is calculated by solving radiative transfer equation with including Thomson scattering, under an assumption that a disk is locally approximated to be a plane-parallel medium in longitudinal motion. The results show that the efficiency of angular momentum extraction by the CBR decreases exponentially with optical depth even if the radiative diffusion is effective. Bacause of the present effects, the distributions of the spin probability of early-formed disks could be significantly modified in the presence of the strong CBR.Also, the CBR force likely helps to enhance the effects of shear viscosity, thereby enabling a seed black hole form at z>10 to account for quasar formation.Also, we have examined the possibility that a population of relic massive black holes, perhaps constituting an important com … More ponent of the dark matter, might be indirectly detected via their occasional very strong gravitational lensing of individual luminous stars in distant external galaxies. For plausible, and in some respects conservative, values of the relevant physical parameters, we show that such events might be detected either in wide area surveys reaching routine CCD magnitude limits (such as the Sloan Digital Sky Survey) or in small field, very deep images (such as the HDF). Thus, it would be a challenging but not impossible task to detect or place limits on a cosmic population of relic massive black holes.Furthermore, we have proposed a novel mechanism for fuelling active galactic nuclei (AGNs), i.e., a radiative avalanche, which is mass-accretion driven by radiation drag exerted by stellar radiation from circumnuclear starburst regions. If a surface layr of a rotating gas disk is irradiated by intensive starlight, then it could lose angular momentum via radiation drag, resulting in an avalanche of the layr as an inevitable consequence. Analyzes show that in an optically thick regime, the mass-accretion rate via this radiative avalanche is in dependent of not only the extinction coefficient of photon absorbing matter but also the density distribution of the disk, and the maximal mass-accretion rate is simply described as M-L_m/c^2 with L_m being the bolometric luminosity of a starburst. In the present context, the intensity of radiative avalanche determines whether a starburst galaxy is destined to posses an AGN or not. The present model provides a solid physical mechanism deduced from first principles to account for the possible link between starburst activities and AGNs, which has been suggested by a number of observations. Less