Building formamide and N-substituted formamides from isocyanates on hydrogenated water ices

IF 5.4 2区 物理与天体物理 Q1 ASTRONOMY & ASTROPHYSICS Astronomy & Astrophysics Pub Date : 2025-03-17 DOI:10.1051/0004-6361/202450614
N. Tieppo, P. Redondo, F. Pauzat, O. Parisel, J.-C. Guillemin, Y. Ellinger
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Abstract

Context. Many complex organic molecules (COMs) observed in the interstellar medium (ISM) are probably not formed in the gas phase. A large consensus has developed that it could be related to the icy surfaces in this environment.Aims. We investigate the process of building N-substituted formamides in the ISM by successive additions of atomic hydrogen to isocyanates. The key point is to see whether the pre-adsorption of the atomic hydrogen on the ice surface is a driving vector as it is for the formation of CH3OH from CO.Methods. We use quantum numerical simulations, namely density functional theory (DFT) and post Hartree–Fock (p-HF) methods derived from coupled-cluster implementations. Several chemical models are presented: the addition of H directly to the isocyanate in the gas phase, the addition of H to the isocyanate pre-adsorbed on ices, the addition of the isocyanate to the hydrogen pre-adsorbed on ices. These ices are successively simulated by a few water molecules up to full bi-layers of them.Results. The formation of formamide (NH2CHO) from the isocyanic acid (HNCO) is taken as a case study. Whatever the level of the calculation and the size of the water cluster supporting the adsorbed isocyanate, the addition of the incoming atomic hydrogen reveals no opportunity to eliminate the energy barrier found in the gas phase. By contrast, the formation of H2NCHO, as well as CH3NHCHO or C2H5NHCHO, is possible without any barrier on the same ice surfaces, with the express condition that the H atom to be added is already attached to the ice, prior to the attack by the isocyanate species.Conclusions. There is a way for the N-substituted formamides to be easily built by two successive hydrogenations on ices starting from the isocyanates HNCO, CH3NCO, and C2H5NCO. Some of those species are already detected; if not, they appear as strong candidates worth considering for future observation campaigns. Moreover, this suggests that other hydrogenation processes neglected to date, could be considered when similar pre-conditions are satisfied.
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背景。在星际介质(ISM)中观测到的许多复杂有机分子(COMs)可能不是在气相中形成的。人们普遍认为这可能与该环境中的冰表面有关。我们研究了在异氰酸酯中连续加入原子氢在 ISM 中形成 N-取代甲酰胺的过程。关键是看原子氢在冰表面的预吸附是否是一个驱动矢量,就像CO形成CH3OH的驱动矢量一样。我们使用了量子数值模拟,即密度泛函理论(DFT)和耦合簇实现的后哈特里-福克(p-HF)方法。我们提出了几种化学模型:在气相中将 H 直接加入异氰酸酯,将 H 加入预吸附在冰上的异氰酸酯,将异氰酸酯加入预吸附在冰上的氢。这些冰先后由几个水分子到完整的双层水分子模拟而成。以异氰酸(HNCO)生成甲酰胺(NH2CHO)为例进行研究。无论计算水平如何,支持吸附异氰酸酯的水团的大小如何,加入原子氢都无法消除气相中的能量障碍。相比之下,H2NCHO 以及 CH3NHCHO 或 C2H5NHCHO 的形成在相同的冰表面没有任何障碍,明确的条件是要加入的氢原子在受到异氰酸酯物种攻击之前已经附着在冰上。有一种方法可以从异氰酸酯 HNCO、CH3NCO 和 C2H5NCO 开始,在冰上通过两次连续氢化反应轻松生成 N-取代甲酰胺。其中一些物种已经被探测到;如果没有,它们也是值得在未来的观测活动中考虑的有力候选物种。此外,这还表明,如果满足类似的先决条件,还可以考虑迄今为止被忽视的其他氢化过程。
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来源期刊
Astronomy & Astrophysics
Astronomy & Astrophysics 地学天文-天文与天体物理
CiteScore
10.20
自引率
27.70%
发文量
2105
审稿时长
1-2 weeks
期刊介绍: Astronomy & Astrophysics is an international Journal that publishes papers on all aspects of astronomy and astrophysics (theoretical, observational, and instrumental) independently of the techniques used to obtain the results.
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