| People | Locations | Statistics |
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| Naji, M. |
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| Motta, Antonella |
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| Aletan, Dirar |
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| Mohamed, Tarek |
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| Ertürk, Emre |
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| Taccardi, Nicola |
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| Kononenko, Denys |
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| Petrov, R. H. | Madrid |
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| Alshaaer, Mazen | Brussels |
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| Bih, L. |
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| Casati, R. |
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| Muller, Hermance |
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| Kočí, Jan | Prague |
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| Šuljagić, Marija |
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| Kalteremidou, Kalliopi-Artemi | Brussels |
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| Azam, Siraj |
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| Ospanova, Alyiya |
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| Blanpain, Bart |
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| Ali, M. A. |
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| Popa, V. |
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| Rančić, M. |
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| Ollier, Nadège |
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| Azevedo, Nuno Monteiro |
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| Landes, Michael |
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| Rignanese, Gian-Marco |
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Oba, Yasuhiro
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (3/3 displayed)
- 2023The spatial distribution of soluble organic matter and their relationship to minerals in the asteroid (162173) Ryugucitations
- 2022Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relationcitations
- 2021Transmission Electron Microscopy Study of the Morphology of Ices Composed of H<sub>2</sub>O, CO<sub>2</sub>, and CO on Refractory Grainscitations
Places of action
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article
Diffusion Activation Energy and Desorption Activation Energy for Astrochemically Relevant Species on Water Ice Show No Clear Relation
Abstract
<jats:title>Abstract</jats:title><jats:p>The activation energies for desorption (<jats:italic>E</jats:italic><jats:sub>des</jats:sub>) and for surface diffusion (<jats:italic>E</jats:italic><jats:sub>sd</jats:sub>) of adsorbed molecules on dust grains are two of the most important parameters for the chemistry in the interstellar medium. Although <jats:italic>E</jats:italic><jats:sub>des</jats:sub> is often measured by laboratory experiments, the measurement of <jats:italic>E</jats:italic><jats:sub>sd</jats:sub> is sparse. Due to the lack of data, astrochemical models usually assume a simple scaling relation, <jats:italic>E</jats:italic><jats:sub>sd</jats:sub> = <jats:italic>f</jats:italic><jats:italic>E</jats:italic><jats:sub>des</jats:sub>, where <jats:italic>f</jats:italic> is a constant, irrespective of the adsorbed species. Here, we experimentally measure <jats:italic>E</jats:italic><jats:sub>sd</jats:sub> for CH<jats:sub>4</jats:sub>, H<jats:sub>2</jats:sub>S, OCS, CH<jats:sub>3</jats:sub>OH, and CH<jats:sub>3</jats:sub>CN on water-ice surfaces using an ultrahigh-vacuum transmission electron microscope. Compiling the measured <jats:italic>E</jats:italic><jats:sub>sd</jats:sub> values and <jats:italic>E</jats:italic><jats:sub>des</jats:sub> values from the literature, we find that the value of <jats:italic>f</jats:italic> ranges from ∼0.2 to ∼0.7, depending on the species. Unless <jats:italic>f</jats:italic> (or <jats:italic>E</jats:italic><jats:sub>sd</jats:sub>) for the majority of species is available, a natural alternative approach for astrochemical models is running multiple simulations, varying <jats:italic>f</jats:italic> for each species randomly. In this approach, ranges of molecular abundances predicted by multiple simulations, rather than abundances predicted by each simulation, are important. We here run 10,000 simulations of astrochemical models of molecular clouds and protostellar envelopes, randomly assigning a value of <jats:italic>f</jats:italic> for each species. In the former case, we identify several key species whose <jats:italic>E</jats:italic><jats:sub>sd</jats:sub> most strongly affects the uncertainties of the model predictions; <jats:italic>E</jats:italic><jats:sub>sd</jats:sub> for those species should be investigated in future laboratory and quantum chemical studies. In the latter case, uncertainties in the <jats:italic>E</jats:italic><jats:sub>sd</jats:sub> of many species contribute to the uncertainties in the model predictions.</jats:p>