Chemical desorption versus energy dissipation: insights from ab-initio molecular dynamics of HCO formation
arXiv:2004.11758 · doi:10.3847/1538-4357/ab8a4b
Abstract
Molecular clouds are the cold regions of the Milky Way where stars form. They are enriched by rather complex molecules. Many of these molecules are believed to be synthesized on the icy surfaces of the interstellar submicron-sized dust grains that permeate the Galaxy. At 10 K thermal desorption is ineffcient and, therefore, why these molecules are found in the cold gas has tantalized astronomers for years. The assumption of the current models, called chemical desorption, is that the molecule formation energy released by the chemical reaction at the grain surface is partially absorbed by the grain and the remaining one causes the ejection of the newly formed molecule into the gas. Here we report an accurate ab-initio molecular dynamics simulations aimed to study the fate of the energy released by the first reaction of the H addition chain on CO, CO + H HCO, occurring on a crystalline ice surface model. We show that about 90% of the HCO formation energy is injected towards the ice in the first picosecond, leaving HCO with an energy content (10-15 kJ mol) more than a factor two lower than its adsorption energy (30 kJ mol). As a result, in agreement with laboratory experiments, we conclude that chemical desorption is ineffcient for this specific system, namely H + CO on crystalline ice. We suspect this behavior to be quite general when dealing with hydrogen bonds, which are responsible of both the cohesive energy of the ice mantle and the interaction with adsorbates, as the HCO radical, even though ad hoc simulations are needed to draw specific conclusions on other systems.
Appendix not included. Submitted to ApJ
References in corpus (8)
- Formation of methyl formate and other organic species in the warm-up phase of hot molecular cores
- Non-thermal desorption from interstellar dust grains via exothermic surface reactions
- The origin of complex organic molecules in prestellar cores
- The Spatial Distribution of Complex Organic Molecules in the L1544 Pre-stellar Core
- Modeling Complex Organic Molecules in dense regions: Eley-Rideal and complex induced reaction
- Seeds Of Life In Space (SOLIS): The organic composition diversity at 300--1000 au scale in Solar-type star forming regions
- The Detection of Hot Cores and Complex Organic Molecules in the Large Magellanic Cloud
- Mechanism of Atomic Hydrogen Addition Reactions on np-ASW
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