GALAXY FORMATION WITH SELF-CONSISTENTLY MODELED STARS AND MASSIVE BLACK HOLES. I. FEEDBACK-REGULATED STAR FORMATION AND BLACK HOLE GROWTH
GALAXY FORMATION WITH SELF-CONSISTENTLY MODELED STARS AND MASSIVE BLACK HOLES. I. FEEDBACK-REGULATED STAR FORMATION AND BLACK HOLE GROWTH
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具有自洽模型恒星和大质量黑洞的星系形成。
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发表时间：
2011
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通讯作者：
Tom Abel
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作者：
Ji;J. Wise;M. Alvarez;Tom Abel
越来越多的证据表明，星系及其嵌入的大质量黑洞（MBH）在分层结构形成范式中共同演化。为了解决星系与MBH相互作用的非线性过程，我们描述了一个包含星系和MBH的自洽数值框架。高分辨率自适应网格细化 (AMR) 代码 Enzo 经过修改，可模拟 15.2 pc 特征尺度分子云的形成和反馈以及气体在 MBH 上的吸积。采用了 MBH 反馈的两个主要通道：辐射反馈（X 射线光子通过完整的三维自适应射线追踪）和机械反馈（以高分辨率 AMR 解析的双极射流）。我们在宇宙学 ΛCDM 模拟中研究了 9.2 × 1011 M☉ 银河晕及其 105 M☉ 嵌入红移 3 的 MBH 的协同演化。 MBH 反馈通过光电离和康普顿加热将周围的星际介质 (ISM) 加热至 106 K，并局部抑制银河系内核中的恒星形成。反馈极大地改变了那里的恒星分布。这种来自缓慢增长的 MBH 的新反馈通道特别有趣，因为它仅在局部占主导地位，并且不需要在磁盘上全局加热气体。 MBH 还通过在较长时间内保持周围 ISM 的热度来自我调节其增长。
There is mounting evidence for the coevolution of galaxies and their embedded massive black holes (MBHs) in a hierarchical structure formation paradigm. To tackle the nonlinear processes of galaxy—MBH interaction, we describe a self-consistent numerical framework which incorporates both galaxies and MBHs. The high-resolution adaptive mesh refinement (AMR) code Enzo is modified to model the formation and feedback of molecular clouds at their characteristic scale of 15.2 pc and the accretion of gas onto an MBH. Two major channels of MBH feedback, radiative feedback (X-ray photons followed through full three-dimensional adaptive ray tracing) and mechanical feedback (bipolar jets resolved in high-resolution AMR), are employed. We investigate the coevolution of a 9.2 × 1011 M☉ galactic halo and its 105 M☉ embedded MBH at redshift 3 in a cosmological ΛCDM simulation. The MBH feedback heats the surrounding interstellar medium (ISM) up to 106 K through photoionization and Compton heating and locally suppresses star formation in the galactic inner core. The feedback considerably changes the stellar distribution there. This new channel of feedback from a slowly growing MBH is particularly interesting because it is only locally dominant and does not require the heating of gas globally on the disk. The MBH also self-regulates its growth by keeping the surrounding ISM hot for an extended period of time.