Institute of Chemistry, Eötvös Loránd University, Pázmány P. stny. 1/A, H-1117 Budapest, Hungary.
Department of Physical Chemistry and Materials Science, Budapest University of Technology and Economics, Budafoki út 8, H-1111 Budapest, Hungary.
J Chem Phys. 2022 May 14;156(18):184703. doi: 10.1063/5.0093561.
The adsorption of acetamide on low density amorphous (LDA) ice is investigated by grand canonical Monte Carlo computer simulations at the temperatures 50, 100, and 200 K, characteristic of certain domains of the interstellar medium (ISM). We found that the relative importance of the acetamide-acetamide H-bonds with respect to the acetamide-water ones increases with decreasing temperature. Thus, with decreasing temperature, the existence of the stable monolayer, characterizing the adsorption at 200 K, is gradually replaced by the occurrence of marked multilayer adsorption, preceding even the saturation of the first layer at 50 K. While isolated acetamide molecules prefer to lay parallel to the ice surface to maximize their H-bonding with the surface water molecules, this orientational preference undergoes a marked change upon saturation of the first layer due to increasing competition of the adsorbed molecules for H-bonds with water and to the possibility of their H-bond formation with each other. As a result, molecules stay preferentially perpendicular to the ice surface in the saturated monolayer. The chemical potential value corresponding to the point of condensation is found to decrease linearly with increasing temperature. We provide, in analogy with the Clausius-Clapeyron equation, a thermodynamic explanation of this behavior and estimate the molar entropy of condensed phase acetamide to be 34.0 J/mol K. For the surface concentration of the saturated monolayer, we obtain the value 9.1 ± 0.8 µmol/m, while the heat of adsorption at infinitely low surface coverage is estimated to be -67.8 ± 3.0 kJ/mol. Our results indicate that the interstellar formation of peptide chains through acetamide molecules, occurring at the surface of LDA ice, might well be a plausible process in the cold (i.e., below 50 K) domains of the ISM; however, it is a rather unlikely scenario in its higher temperature (i.e., 100-200 K) domains.
通过在 50、100 和 200 K 的温度下进行巨正则蒙特卡罗计算机模拟,研究了乙酰胺在低密度非晶冰(LDA)上的吸附,这些温度分别对应于星际介质(ISM)的某些区域。我们发现,相对于乙酰胺-水氢键,乙酰胺-乙酰胺氢键的相对重要性随着温度的降低而增加。因此,随着温度的降低,在 200 K 下吸附的稳定单层的存在逐渐被明显的多层吸附所取代,甚至在 50 K 下第一层达到饱和之前就已经出现了。虽然孤立的乙酰胺分子更喜欢平行于冰表面排列,以最大限度地与表面水分子形成氢键,但这种取向偏好会在第一层饱和时发生明显变化,因为吸附分子与水分子争夺氢键的竞争加剧,并且它们之间形成氢键的可能性也增加。结果,在饱和单层中,分子优先垂直于冰表面。与凝结点相对应的化学势值被发现随温度线性降低。我们提供了一个与克劳修斯-克拉珀龙方程类似的热力学解释,该解释估计了这种行为,并估计凝聚相乙酰胺的摩尔熵为 34.0 J/mol K。对于饱和单层的表面浓度,我们得到了 9.1 ± 0.8 µmol/m 的值,而无限低表面覆盖率下的吸附热估计为-67.8 ± 3.0 kJ/mol。我们的结果表明,通过乙酰胺分子在 LDA 冰表面形成肽链的星际形成过程很可能是在冷(即低于 50 K)ISM 区域中一个合理的过程;然而,在其更高温度(即 100-200 K)区域中,这是一个不太可能的情景。