Simulation of the Formation and Morphology of Ice Mantles on Interstellar Grains

By H. Cuppen, E. Herbst. 2007

235 citations recorded by the source corpus.

Although still poorly understood, the chemistry that occurs on the surfaces of interstellar dust particles profoundly affects the growth of molecules in the interstellar medium. An important set of surface reactions produces icy mantles of many monolayers in cold and dense regions. The monolayers are dominated by water ice, but also contain CO, CO2, and occasionally methanol, as well as minor constituents. In this paper, the rate of production of water-ice-dominated mantles is calculated for different physical conditions of interstellar clouds and for the first time images of the morphology of interstellar ices are presented. For this purpose, the continuous-time random-walk Monte Carlo simulation technique has been used. The visual extinction, density, and gas and grain temperatures are varied. It is shown that our stochastic approach can reproduce the important observation that ice mantles only grow in the denser regions.

Subfields: Astronomy and Astrophysics, Atmospheric Science, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/b151b55a0f4395719c2d43c79bc1204f3fddd96e

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. R. Garrod
2. E. Dishoeck
3. E. Herbst
4. V. Wakelam
5. A. Tielens
6. M. Ruaud
7. H. Linnartz
8. H. Cuppen

In Atmospheric Science

1. R. Garrod
2. E. Dishoeck
3. V. Wakelam
4. E. Herbst
5. A. Tielens
6. H. Cuppen
7. S. Ioppolo
8. M. Ruaud

In Statistical and Nonlinear Physics

1. E. Dishoeck
2. V. Wakelam
3. M. Ruaud
4. A. Tielens
5. S. Ioppolo
6. F. Hersant
7. H. Linnartz
8. C. Romanzin

Citations in the corpus

• Laboratory Evidence for Efficient Water Formation in Interstellar Ices (2008, methodology): “H2O ð4Þ According to Cuppen & Herbst (2007), this channel is, together with the O3 channel, responsible for water formation in cold, dense clouds.”
• Ice structures, patterns, and processes: A view across the icefields (2012, background): “What are the morphologies of the water ice and the other ices present in the interstellar gas clouds (Cartwright et al., 2008; Collings et al., 2006; Cuppen and Herbst, 2007)?”
• H$_2$ formation on interstellar dust grains: the viewpoints of theory, experiments, models and observations (2017, background): “The sticking of H 2 onto multi-layers, i.e. on o itself, is much less efficient ( Cuppen and Herbst, 2007 ) slowing own the depletion of H 2 from the gas.”
• Grain Surface Models and Data for Astrochemistry (2017, background): “…and to take all relevant processes into account in the modeling, e.g., inter-lattice diffusion, mobility/immobility of reactants, desorption, porosity trapping (see Cuppen and Herbst 2007; Chang et al. 2007; Kalvāns and Shmeld 2010; Wolff et al. 2011; Taquet et al. 2012; Vasyunin and Herbst 2013).”
• Binding energies: New values and impact on the efficiency of chemical desorption (2017, background): “However, these calculations are relatively complex and astrochemical models use rather additive law considering, for example, that ED(O3) = ED(O2) + ED(O), which is a very rough approximation (see for instance Cuppen & Herbst 2007).”
• Complex organic molecules in protoplanetary disks (2013, background): “(1) Collings et al. (2004); (2) Garrod & Herbst (2006); (3) Cuppen & Herbst (2007). from both UV and X-ray photons; however, cosmic rays are able to penetrate the entire disk.”
• Gas and grain chemical composition in cold cores as predicted by the Nautilus three-phase model (2016, methodology): “The same formation path was found by Cuppen & Herbst (2007) using the CTRW Monte Carlo code technique and Garrod & Pauly (2011) that also accounts for this competition.”
• Hydrogenation reactions in interstellar CO ice analogues A combined experimental/theoretical approach (2009, methodology): “For a detailed description of the method and program, we refer to Cuppen & Herbst (2007).”
• Photodesorption of water ice - A molecular dynamics study (2008, background): “Therefore, the exact ice morphology that results from such a chemical build-up of the iceis not yet clear (see however Cuppen & Herbst (2007)).”
• Microscopic simulation of methanol and formaldehyde ice formation in cold dense cores (2009, methodology): “In previous CTRW Monte Carlo studies (Chang et al. 2007; Cuppen & Herbst 2007), we treated reactions with barriers solely by tunnelling through a square potential and ignored any small temperature dependence at low temperatures.”
• Experimental evidence for water formation on interstellar dust grains by hydrogen and oxygen atoms (2009, background): “Recent Monte Carlo simulations (Cuppen and Herbst 2007) show that while the main route to water formation on cosmic dust grains in diffuse and translucent clouds is the reaction H+ OH, in dense clouds the principal source of H2O is the reaction between H2 and OH.”
• ON THE FORMATION OF CO2 AND OTHER INTERSTELLAR ICES (2011, background): “As found by Cuppen & Herbst (2007), the reaction H2 + OH → H2O (EA = 2100 K, Baulch et al., 1984) is the main mechanism for the conversion of OH to water, rather than reaction with atomic H, because of the large H2 abundance on the grains (∼3 % of surface coverage).”