恒星形成分子云中水和甲醇的形成
Formation of water and methanol in star forming molecular clouds
摘要：
我们研究了形成的水和甲醇在稠密的云条件下，找到其生产率的结合能，反应机制，温度和晶粒网站数量的依赖。我们希望找到有效的晶粒表面积可用于化学反应和有效的复合时间尺度作为粮食和气体参数的函数。我们使用了蒙特卡罗模拟来跟踪发生在晶粒表面上的化学过程。我们发现，各种分子的形成速率强烈依赖于结合能。当结合能高时，很难产生大量的分子种类。相反，发现颗粒充满了原子种类。生产率被发现依赖于在气相中的数密度。我们表明，有效晶粒表面积的概念，我们在我们的早期工作中介绍，发挥了重要作用，在粮食化学。我们计算的丰富的水和甲醇，并表明，结果强烈依赖于在气相中的密度和成分，以及各种晶粒参数。在速率方程中，通常假设复合效率与晶粒参数和表面覆盖度无关。目前，我们计算的参数$α$为每个产品被发现依赖于吸积率，晶粒参数和晶粒的表面覆盖度。我们比较了从速率方程和从有效速率方程得到的结果，其中包括$α$。最后，我们将我们的结果与观测到的丰度进行了比较。
英文摘要：
We study the formation of water and methanol in the dense cloud conditions to find the dependence of its production rate on the binding energies, reaction mechanisms, temperatures, and grain site number. We wish to find the effective grain surface area available for chemical reaction and the effective recombination timescales as functions of grain and gas parameters. We used a Monte Carlo simulation to follow the chemical processes occurring on the grain surface. We find that the formation rate of various molecules is strongly dependent on the binding energies. When the binding energies are high, it is very difficult to produce significant amounts of the molecular species. Instead, the grain is found to be full of atomic species. The production rates are found to depend on the number density in the gas phase. We show that the concept of the effective grain surface area, which we introduced in our earlier work, plays a significant role in grain chemistry. We compute the abundance of water and methanol and show that the results strongly depend on the density and composition in the gas phase, as well as various grain parameters. In the rate equation, it is generally assumed that the recombination efficiencies are independent of the grain parameters, and the surface coverage. Presently, our computed parameter $α$ for each product is found to depend on the accretion rate, the grain parameters and the surface coverage of the grain. We compare our results obtained from the rate equation and the one from the effective rate equation, which includes $α$. At the end we compare our results with the observed abundances.
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