超新星爆发驱动的气盘粘性演化。II。高红移恒星形成星系的结构和辐射
Evolution of gaseous disk viscosity driven by supernova explosion. II. Structure and emissions from star-forming galaxies at high redshift
摘要：
高红移星系正经历着强烈的动力学结构和形态演化。我们将反馈到动力学方程通过质量脱落和角动量输运驱动的SNexp激发湍流粘性。我们数值求解的方程，并表明，可以有密集的演变的气体盘的结构。盘的长期演化表现出以下有趣的特征：1）SNexp激发的高粘度气体可以有效地将10 kpc的气体输送到$\sim 1$ kpc，形成星盘，而低粘度的情况下形成星环：2）星暴触发SMBH活动，其滞后$\sim 10^8$ yr取决于恒星形成速率，促使SMBH和凸起的联合演化;（3）气盘中的速度色散高达$\sim 100~\kms$。为了比较现有的模型与观测到的动力学结构和图像，我们使用从简单的恒星合成（GALAXEV）和云的入射连续计算H $α$，H $β$，$\OIII$和$\NII$的发射线比，和H $α$亮度的气体光电离的年轻的大质量恒星上形成的磁盘。这些模型能给出恒星形成星系辐射的主要特征以及观测到的湍流速度与H $α$亮度的关系。我们成功地将本模型应用于在高密度$-z$样品中观测到的BX 389和BX 482，这两个样品分别是凸起和盘状的。由SNexp激发的高粘度能够有效地将气体输送到凸起中，以保持高的恒星形成率，或者形成足够接近凸起的恒星环，以便它迁移到其宿主星系的凸起中。这导致了快速增长的膨胀。目前的模型的意义和未来的工作已被广泛讨论的星系形成。
英文摘要：
(Abridged) High redshift galaxies are undergoing intensive evolution of dynamical structure and morphologies. We incorporate the feedback into the dynamical equations through mass dropout and angular momentum transportation driven by the SNexp-excited turbulent viscosity. We numerically solve the equations and show that there can be intensive evolution of structure of the gaseous disk. Secular evolution of the disk shows interesting characteristics that are 1) high viscosity excited by SNexp can efficiently transport the gas from 10kpc to $\sim 1$kpc forming a stellar disk whereas a stellar ring forms for the case with low viscosity; 2) starbursts trigger SMBH activity with a lag $\sim 10^8$yr depending on star formation rates, prompting the joint evolution of SMBHs and bulges; 3) the velocity dispersion is as high as $\sim 100~\kms$ in the gaseous disk. In order to compare the present models with the observed dynamical structure and images, we use the incident continuum from the simple stellar synthesis (GALAXEV) and CLOUDY to calculate emission line ratios of H$α$, H$β$, $\OIII$ and $\NII$, and H$α$ brightness of gas photoionized by young massive stars formed on the disks. The models can produce the main features of emission from star forming galaxies and the observed relation between turbulent velocity and the H$α$ brightness. We successfully apply the present model to BX 389 and BX 482 observed in SINS high$-z$ sample, which are bulge and disk-dominated, respectively. High viscosity excited by SNexp is able to efficiently transport the gas into a bulge to maintain high star formation rates, or, to form a stellar ring close enough to the bulge so that it immigrates into the bulge of its host galaxy. This leads to a fast growing bulge. Implications and future work of the present models have been extensively discussed for galaxy formation.
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