用二维流体动力学模型研究原恒星形成过程中的化学演化
Chemical evolution during the process of proto-star formation by considering a two dimensional hydrodynamic model
摘要：
分子云的化学成分对云的物理性质非常敏感。为了获得恒星形成区周围的化学成分，我们对原恒星的坍缩阶段进行了二维流体动力学模拟。采用总变差递减格式（TVD）求解流体动力学方程组。这种流体动力学代码能够模拟原恒星形成过程中物理性质的演变。我们耦合我们的相当大的气体颗粒化学网络，研究化学演化过程中的坍缩阶段的原恒星。为了对生物分子在星际介质中的丰度有一个现实的估计，我们将最近计算的几种星际生物分子形成的速率系数纳入我们的气相网络。通过在整个模拟过程中保持谷物在恒定温度下以及通过使用从流体动力学模型获得的温度变化来详细研究化学演化。通过考虑一个大的气体颗粒网络与复杂的流体动力学模型更现实的丰度预测。我们发现，化学成分是高度敏感的动力学行为的坍缩云，特别是对密度和温度分布。
英文摘要：
Chemical composition of a molecular cloud is highly sensitive to the physical properties of the cloud. In order to obtain the chemical composition around a star forming region, we carry out a two dimensional hydrodynamical simulation of the collapsing phase of a proto-star. A total variation diminishing scheme (TVD) is used to solve the set of equations governing hydrodynamics. This hydrodynamic code is capable of mimicking evolution of the physical properties during the formation of a proto-star. We couple our reasonably large gas-grain chemical network to study the chemical evolution during the collapsing phase of a proto-star. To have a realistic estimate of the abundances of bio-molecules in the interstellar medium, we include the recently calculated rate coefficients for the formation of several interstellar bio-molecules into our gas phase network. Chemical evolution is studied in detail by keeping grain at the constant temperature throughout the simulation as well as by using the temperature variation obtained from the hydrodynamical model. By considering a large gas-grain network with the sophisticated hydrodynamic model more realistic abundances are predicted. We find that the chemical composition are highly sensitive to the dynamic behavior of the collapsing cloud, specifically on the density and temperature distribution.
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