2017
DOI: 10.1017/s1743921317009929
View full text | Cite
|
Sign up to set email alerts
|

Abstract: Molecules in space are synthesized via a large variety of gas-phase reactions, and reactions on dust-grain surfaces, where the surface acts as a catalyst. Especially, saturated, hydrogen-rich molecules are formed through surface chemistry. Astrochemical models have developed over the decades to understand the molecular processes in the interstellar medium, taking into account grain surface chemistry. However, essential input information for gas-grain models, such as binding energies of molecules to the surface… Show more

Help me understand this report
View preprint versions

Search citation statements

Order By: Relevance

Paper Sections

Select...
4
1

Citation Types

0
5
0

Year Published

2019
2019
2022
2022

Publication Types

Select...
3

Relationship

0
3

Authors

Journals

citations
Cited by 3 publications
(5 citation statements)
references
References 32 publications
(40 reference statements)
0
5
0
Order By: Relevance
“…Microscopic Monte Carlo simulation, which records the position of each adsorbed species in ice mantle, is suitable for such cold ice chemistry (e.g. Cuppen et al 2018) (see also Garrod & Clements on page 429). Microscopic Monte Carlo simulation is, however, computationally expensive; most of the CPU time is consumed to follow the thermal hopping of very volatile species such as H atom, once the temperature starts to rise.…”
Section: Com Formation Mechanismsmentioning
confidence: 99%
“…The interested reader can found more about modeling interstellar ice in the recent papers by Zamirri et al 14 and Cuppen et al 32 …”
Section: Introductionmentioning
confidence: 99%
“…The interested reader can found more about modeling interstellar ice in the recent papers by Zamirri et al 14 and Cuppen et al 32 In this paper, we will describe a new approach to automatically building up an amorphous icy grain model constituted by several hundreds of water molecules. We labeled our models as "realistic", not based on a size criterion only but requiring the following essential features: (i) the grain should not be minimal, i.e., envisaging 20−30 water molecules only, as usually found in the literature, but includes at least few hundreds water molecules; (ii) the hydrogen bond features within the icy grain should be accurately represented by adopting a proper quantum level of theory; (iii) the ice should be amorphous by construction, avoiding the usual approach of heating at high T and sudden cooling of a crystalline ice model, which has no counterpart in the grain evolution in the ISM.…”
Section: ■ Introductionmentioning
confidence: 99%
“…Ice-covered grains found in interstellar and prestellar nebulae offer active sites for chemistry to occur that are often both different and more favorable than the limited gas phase chemistry that can occur at the very cold temperatures (∼15 K) and low densities (as low as 10 3 m –3 ) that exist in these sources . A wide variety of heterogeneous pathways to form small compounds have been characterized via both theory and experiment that involve neutral and charged systems. There is great interest in the formation of complex organic molecules (COMs) or their precursors, particularly in protostellar sources, since they may provide insight into how the compounds necessary for biopoiesis made their way to the primordial Earth. Ice chemistry is thought to contribute significantly to COM formation. ,, …”
Section: Introductionmentioning
confidence: 99%
“…A wide variety of heterogeneous pathways to form small compounds have been characterized via both theory and experiment that involve neutral and charged systems. There is great interest in the formation of complex organic molecules (COMs) or their precursors, particularly in protostellar sources, since they may provide insight into how the compounds necessary for biopoiesis made their way to the primordial Earth. Ice chemistry is thought to contribute significantly to COM formation. ,, …”
Section: Introductionmentioning
confidence: 99%