Simulation of CH3OH ice UV photolysis under laboratory conditions

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dc.contributor.authorRocha, Will Robson Monteiro
dc.contributor.authorWoitke, Peter
dc.contributor.authorPilling, Sergio
dc.contributor.authorThi, Wing-Fai
dc.contributor.authorJørgensen, Jes Kristian
dc.contributor.authorKristensen, Lars Egstrøm
dc.contributor.authorPerotti, Giulia
dc.contributor.authorKamp, Inga
dc.date.accessioned2025-02-27T14:46:16Z
dc.date.available2025-02-27T14:46:16Z
dc.date.issued22023
dc.description.abstractContext. Methanol is the most complex molecule that is securely identified in interstellar ices. It is a key chemical species for understanding chemical complexity in astrophysical environments. Important aspects of the methanol ice photochemistry are still unclear, such as the branching ratios and photodissociation cross sections at different temperatures and irradiation fluxes. Aims. This work aims at a quantitative agreement between laboratory experiments and astrochemical modelling of the CH3OH ice UV photolysis. Ultimately, this work allows us to better understand which processes govern the methanol ice photochemistry present in laboratory experiments. Methods. We used the code ProDiMo to simulate the radiation fields, pressures, and pumping efficiencies characteristic of laboratory measurements. The simulations started with simple chemistry consisting only of methanol ice and helium to mimic the residual gas in the experimental chamber. A surface chemical network enlarged by photodissociation reactions was used to study the chemical reactions within the ice. Additionally, different surface chemistry parameters such as surface competition, tunnelling, thermal diffusion, and reactive desorption were adopted to check those that reproduce the experimental results. Results. The chemical models with the code ProDiMo that include surface chemistry parameters can reproduce the methanol ice destruction via UV photodissociation at temperatures of 20, 30, 50, and 70 K as observed in the experiments. We also note that the results are sensitive to different branching ratios after photolysis and to the mechanisms of reactive desorption. In the simulations of a molecular cloud at 20 K, we observed an increase in the methanol gas abundance of one order of magnitude, with a similar decrease in the solid-phase abundance. Conclusions. Comprehensive astrochemical models provide new insights into laboratory experiments as the quantitative understanding of the processes that govern the reactions within the ice. Ultimately, these insights can help us to better interpret astronomical observations.
dc.description.physical38 p.
dc.description.sponsorshipFundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP)
dc.description.uriFAPESP (No 16/23054-7)
dc.format.mimetypePDF
dc.identifier.affiliationLeiden University
dc.identifier.affiliationUniversity of Copenhagen
dc.identifier.affiliationAustrian Academy of Sciences
dc.identifier.affiliationUniversidade do Vale do Paraíba
dc.identifier.affiliationMax-Planck-Institut für extraterrestrische Physik
dc.identifier.affiliationMax Planck Institute for Astronomy
dc.identifier.affiliationUniversity of Groningen
dc.identifier.bibliographicCitationROCHA, Will Robson Monteiro et al. Simulation of CH3OH ice UV photolysis under laboratory conditions. Astronomy & Astrophysics, v. 673, p. 1-38, 2023. Disponível em: https://www.aanda.org/10.1051/0004-6361/202142570.
dc.identifier.doi10.1051/0004-6361/202142570
dc.identifier.urihttps://repositorio.univap.br/handle/123456789/606
dc.language.isoen_US
dc.publisherEDP Sciences
dc.rights.holderWill Robson Monteiro Rocha et al.
dc.subject.keywordAstrochemistry
dc.subject.keywordISM: molecules
dc.subject.keywordSolid state: volatile
dc.titleSimulation of CH3OH ice UV photolysis under laboratory conditions
dc.typeArtigos de Periódicos

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