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FIR/sub-mm/mm线辐射的演变星爆模拟。II。适用于M 82

Evolving Starburst Modeling of FIR/sub-mm/mm Line Emission. II. Application to M 82

Lihong Yao

备注：
Accepted for publication in the ApJ, 56 pages, 14 figures, 3 tables
发表信息：
Astrophys.J.705:766-785,2009
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摘要：

我们提出了星爆模型的远红外/亚毫米/毫米（FIR/亚毫米/毫米）线发射的分子和原子气体在不断发展的星爆区域，这被视为一个合奏的非相互作用的热气泡驱动球壳扫起气体到周围的均匀气体介质。这些气泡和外壳是由恒星风和超新星驱动的，这些恒星风和超新星是在瞬间的恒星爆发中形成的。来自演化星系团的恒星辐射影响着壳层中光解离区的性质和结构，因此这些掠起的壳层和相关的母巨分子云的分子和原子谱线辐射的光谱能量分布（SED）包含了星暴演化阶段的特征。壳层的物理和化学性质及其结构的计算使用一个简单的众所周知的壳层膨胀的相似性解决方案，一个恒星星族合成代码，和一个随时间变化的PDR化学模型。使用非局部热力学平衡（非LTE）线辐射传输模型计算了几种分子和原子线（$^{12}$ CO及其同位素$^{13}$ CO、HCN、HCO $^+$、C、O和C $^+$）的SED。通过比较我们的模型与附近的红外亮星系，特别是M 82的观测数据，我们约束的模型，并在M 82的情况下，我们提供的年龄（5 - 6百万年，10百万年）的估计最近的星暴活动。我们还导出了M 82中心1 kpc星爆盘观测区域的总H $_2$气体质量为$\sim$ 2 - 3.4 $\times$ 10 $^8$ M $_{\odot}$。

英文摘要：

We present starburst models for far-infrared/sub-millimeter/millimeter (FIR/sub-mm/mm) line emission of molecular and atomic gas in an evolving starburst region, which is treated as an ensemble of non-interacting hot bubbles which drive spherical shells of swept-up gas into a surrounding uniform gas medium. These bubbles and shells are driven by stellar winds and supernovae within massive star clusters formed during an instantaneous starburst. The underlying stellar radiation from the evolving clusters affects the properties and structure of photodissociation regions (PDRs) in the shells, and hence the spectral energy distributions (SEDs) of the molecular and atomic line emission from these swept-up shells and the associated parent giant molecular clouds (GMCs) contains a signature of the stage of evolution of the starburst. The physical and chemical properties of the shells and their structure are computed using a a simple well known similarity solution for the shell expansion, a stellar population synthesis code, and a time-dependent PDR chemistry model. The SEDs for several molecular and atomic lines ($^{12}$CO and its isotope $^{13}$CO, HCN, HCO$^+$, C, O, and C$^+$) are computed using a non-local thermodynamic equilibrium (non-LTE) line radiative transfer model. By comparing our models with the available observed data of nearby infrared bright galaxies, especially M 82, we constrain the models and in the case of M 82, we provide estimates for the ages (5 - 6 Myr, 10 Myr) of recent starburst activity. We also derive a total H$_2$ gas mass of $\sim$ 2 - 3.4 $\times$ 10$^8$ M$_{\odot}$ for the observed regions of the central 1 kpc starburst disk of M 82.

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