气体吸积与Angular Momentum
Gas Accretion and Angular Momentum
摘要：
在这一章中，我们回顾了气体吸积的角动量的收购，在星系和它们的气体晕的作用。我们首先讨论角动量在暗物质晕，潮汐扭矩理论和合并的重要性进行了简要的回顾，然后在这个框架内，假设晕气体冲击热的维里温度的晕，以下相同的自旋分布的暗物质晕冷却到晕的中心，形成一个星系有一个典型的图片星系形成的讨论。在最近的观测证据表明存在的高角动量气体的星系晕的背景下，我们回顾最近的宇宙学流体动力学模拟，已经开始强调的作用，“冷流”吸积-各向异性气体吸积沿宇宙细丝，不冲击热下沉到中央星系。我们讨论了这些模拟的影响，回顾了一些最近的发展在文献中，并建议修订的正则模型，因为它涉及到预期的角动量含量的气体晕星系周围。
英文摘要：
In this chapter, we review the role of gas accretion to the acquisition of angular momentum, both in galaxies and in their gaseous halos. We begin by discussing angular momentum in dark matter halos, with a brief review of tidal torque theory and the importance of mergers, followed by a discussion of the canonical picture of galaxy formation within this framework, where halo gas is presumed to shock-heat to the virial temperature of the halo, following the same spin distribution as the dark matter halo before cooling to the center of the halo to form a galaxy there. In the context of recent observational evidence demonstrating the presence of high angular momentum gas in galaxy halos, we review recent cosmological hydrodynamic simulations that have begun to emphasize the role of "cold flow" accretion---anisotropic gas accretion along cosmic filaments that does not shock-heat before sinking to the central galaxy. We discuss the implications of these simulations, reviewing a number of recent developments in the literature, and suggest a revision to the canonical model as it relates to the expected angular momentum content of gaseous halos around galaxies.
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