Black Hole Spin and Galactic Morphology
Black Hole Spin and Galactic Morphology
复制标题
DOI：
10.1086/521186
复制
发表时间：
2007-06
期刊：
影响因子：
--
通讯作者：
M. Volonteri;M. Sikora;J. Lasota
中科院分区：
文献类型：
--
作者：
M. Volonteri;M. Sikora;J. Lasota
我们研究了Sikora，Stawarz和Lasota的猜想，即观测到的活动星系核(AGN)射电响度双峰性可以用星系中心黑洞自旋分布的与形态有关的双峰性来解释：巨型椭圆星系中的中心黑洞(BHS)的自旋(平均)可能比螺旋/盘状星系中的黑洞大得多。我们研究了来自翘曲盘的吸积如何影响黑洞自转的演化，并得出结论：在宇宙学框架内，最大质量的黑洞是通过合并驱动的吸积而增加质量的，人们确实预计椭圆星系中的大多数超大质量黑洞的自转平均比螺旋星系中的黑洞高，在螺旋星系中，随机的小吸积事件(例如，潮汐破裂的恒星，分子云的吸积)可能发挥了更重要的作用。
We investigate the conjecture by Sikora, Stawarz, and Lasota that the observed active galactic nuclei (AGNs) radio loudness bimodality can be explained by the morphology-related bimodality of black hole spin distribution in the centers of galaxies: central black holes (BHs) in giant elliptical galaxies may have (on average) much larger spins than black holes in spiral/disk galaxies. We study how accretion from a warped disk influences the evolution of black hole spins and conclude that within the cosmological framework, where the most massive BHs have grown in mass via merger-driven accretion, one indeed expects most supermassive black holes in elliptical galaxies to have on average higher spin than black holes in spiral galaxies, where random, small accretion episodes (e.g., tidally disrupted stars, accretion of molecular clouds) might have played a more important role.