星际介质中富碳结构的成核和稳定
Nucleation and stabilization of carbon-rich structures in interstellar media
摘要：
我们研究的条件下，不同大小的碳簇形成和稳定。{We描述一种通过长时间模拟稀薄碳气体动力学来达到平衡的方法。首先，我们使用反应分子动力学模拟来描述在富含碳氢的星际气体相中长链、大团簇和复杂笼状结构的成核。我们研究如何温度，粒子密度，氢的存在下，和碳流入影响成核的分子部分具有不同的特性，根据天体物理条件。我们扩展的模拟密度比目前的实验室密度低的数量级，相关的行星状星云的星周环境的温度，和长期（微秒）形成的时间尺度。我们关联集群大小分布从动力学模拟与热力学平衡的直觉，在低温和气体密度，熵起着重要的作用。
英文摘要：
We study conditions under which carbon clusters of different sizes form and stabilize. {We describe an approach to equilibrium by simulating tenuous carbon gas dynamics to long times.} First, we use reactive molecular dynamics simulations to describe the nucleation of long chains, large clusters, and complex cage structures in carbon and hydrogen rich interstellar gas phases. We study how temperature, particle density, presence of hydrogen, and carbon inflow affect the nucleation of molecular moieties with different characteristics, in accordance with astrophysical conditions. We extend the simulations to densities which are orders of magnitude lower than current laboratory densities, to temperatures relevant to circumstellar environments of planetary nebulae, and to longtime (microsecond) formation timescales. We correlate cluster size distributions from dynamical simulations with thermodynamic equilibrium intuitions, where at low temperatures and gas densities, entropy plays a significant role.
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