A novel framework for studying the impact of binding energy distributions on the chemistry of dust grains

Bovino, S.; Caselli, P.; Bovolenta, Giulia; Vogt-Geisse, Stefan; Ercolano, Barbara

doi:10.1051/0004-6361/202039087

Cited by 27 publications

(23 citation statements)

References 56 publications

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“…However, the microphysics during the desorption involve the structure of the water ice and how the COMs reside in the ice matrix, requiring further understanding of how the chemical evolution takes place on the grain surface. Furthermore, the distribution of the binding energy can have a crucial effect on the estimate of the desorbed species (Ferrero et al 2020;Grassi et al 2020).…”

Section: Origin Of the Ch 3 Oh/ch 3 Cn Correlationmentioning

confidence: 99%

The Perseus ALMA Chemistry Survey (PEACHES). I. The Complex Organic Molecules in Perseus Embedded Protostars

Yang

Sakai

Zhang

et al. 2021

ApJ

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To date, about two dozen low-mass embedded protostars exhibit rich spectra with lines of complex organic molecules (COMs). These protostars seem to possess a different enrichment in COMs. However, the statistics of COM abundance in low-mass protostars are limited by the scarcity of observations. This study introduces the Perseus ALMA Chemistry Survey (PEACHES), which aims at unbiasedly characterizing the chemistry of COMs toward the embedded (Class 0/I) protostars in the Perseus molecular cloud. Of the 50 embedded protostars surveyed, 58% of them have emission from COMs. 56%, 32%, and 40% of the protostars have CH 3 OH, CH 3 OCHO, and N-bearing COMs, respectively. The detectability of COMs depends neither on the averaged continuum brightness temperature, a proxy of the H 2 column density, nor on the bolometric luminosity and the bolometric temperature. For the protostars with detected COMs, CH 3 OH has a tight correlation with CH 3 CN, spanning more than two orders of magnitude in column densities normalized by the continuum brightness temperature, suggesting a chemical relation between CH 3 OH and CH 3 CN and a large chemical diversity in the PEACHES samples at the same time. A similar trend with more scatter is also found between all identified COMs, which hints at a common chemistry for the sources with COMs. The correlation between COMs is insensitive to the protostellar properties, such as the bolometric luminosity and the bolometric temperature. The abundance of larger COMs (CH 3 OCHO and CH 3 OCH 3 ) relative to that of smaller COMs (CH 3 OH and CH 3 CN) increases with the inferred gas column density, hinting at an efficient production of complex species in denser envelopes.

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Section: Origin Of the Ch 3 Oh/ch 3 Cn Correlationmentioning

confidence: 99%

The Perseus ALMA Chemistry Survey (PEACHES). I. The Complex Organic Molecules in Perseus Embedded Protostars

Yang

Sakai

Zhang

et al. 2021

ApJ

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“…The freeze-out of H 2 that occurs for high H 2 binding energies gives access to different parts of the reaction network, leading to a more methane-rich ice, instead of a methanol-rich ice that is found for lower binding energies. Grassi et al 158 found that the surface chemistry drastically changes when multiple binding sites are considered, instead of a single value binding site. They covered a range of different conditions, typical for the surroundings of a proto-star or in the disk mid-plane.…”

Section: Astrochemical Modelsmentioning

confidence: 99%

Thermal desorption of interstellar ices. A review on the controlling parameters and their implications fromsnowlines to chemical complexity

Minissale¹,

Aikawa²,

Bergin³

et al. 2022

Preprint

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The evolution of star-forming regions and their thermal balance are strongly influenced by their chemical composition, that, in turn, is determined by the physicochemical processes that govern the transition between the gas phase and the solid state, specifically icy dust grains (e.g., particles adsorption and desorption). Gas-grain and grain-gas transitions as well as formation and sublimation of interstellar ices are thus essential elements of understanding astrophysical observations of cold environments (e.g., pre-stellar cores) where unexpected amounts of a large variety of chemical species have been observed in the gas phase. Adsorbed atoms and molecules also undergo chemical reactions which are not efficient in the gas phase. Therefore the parameterization of the physical properties of atoms and molecules interacting with dust grain particles is clearly a key aspect to interpret astronomical observations and to build realistic and predictive astrochemical models. In this consensus evaluation, we focus on parameters controlling the thermal desorption of ices and how these determine pathways towards molecular complexity and define the location of snowlines, which ultimately influence the planet formation process.We review different crucial aspects of desorption parameters both from a theoretical and experimental point of view. We critically assess the desorption parameters (the binding energies E b and the pre-exponential factor ν) commonly used in the astrochemical community for astrophysically relevant species and provide tables with recommended values. The aim of these tables is to provide a coherent set of critically assessed desorption parameters for common use in future work. In addition, we show that a non-trivial determination of the pre-exponential factor ν using the Transition State Theory can affect the binding energy value. The primary focus is on pure ices, but we also discuss the desorption behavior of mixed, i.e. astronomically more realistic ices. This allows discussion of segregation effects. Finally, we conclude this work by discussing the limitations of theoretical and experimental approaches currently used to determine the desorption properties with suggestions for future improvements.

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“…However, the microphysics during the desorption involve the structure of the water ice and how the COMs reside in the ice matrix, requiring further understanding of how the chemical evolution takes place on the grain surface. Also, the distribution of the binding energy can have crucial effect on the estimate of the desorbed species (Ferrero et al 2020;Grassi et al 2020).…”

Section: Origin Of the Ch 3 Oh/ch 3 Cn Correlationmentioning

confidence: 99%

The Perseus ALMA Chemistry Survey (PEACHES). I. The Complex Organic Molecules in Perseus Embedded Protostars

Yang,

Sakai,

Zhang

et al. 2021

Preprint

View full text Add to dashboard Cite

To date, about two dozen low-mass embedded protostars exhibit rich spectra with complex organic molecule (COM) lines. These protostars seem to possess different enrichment in COMs. However, the statistics of COM abundance in low-mass protostars are limited by the scarcity of observations. This study introduces the Perseus ALMA Chemistry Survey (PEACHES), which aims at unbiasedly characterizing the chemistry of COMs toward the embedded (Class 0/I) protostars in the Perseus molecular cloud. Among the 50 embedded protostars surveyed, 58% of them have emission from COMs. A 56%, 32%, and 40% of protostars have CH 3 OH, CH 3 OCHO, and N-bearing COMs, respectively. The detectability of COMs depends on neither the averaged continuum brightness temperature, a proxy of the H 2 column density, nor the bolometric luminosity and the bolometric temperature. For the protostars with detected COMs, CH 3 OH has a tight correlation with CH 3 CN, spanning more than two orders of magnitude in column densities normalized by the continuum brightness temperature, suggesting a chemical relation between CH 3 OH and CH 3 CN and large chemical diversity among the PEACHES samples at the same time. A similar trend with more scatter is also found between all identified COMs, hinting at common chemistry for the sources with COMs. The correlation between COMs is insensitive to the protostellar properties, such as the bolometric luminosity and the bolometric temperature. The abundance of larger COMs (CH 3 OCHO and CH 3 OCH 3 ) relative to that of smaller COMs (CH 3 OH and CH 3 CN) increases with the inferred gas column density, hinting at an efficient production of complex species in denser envelopes.

show abstract

A novel framework for studying the impact of binding energy distributions on the chemistry of dust grains

Cited by 27 publications

References 56 publications

The Perseus ALMA Chemistry Survey (PEACHES). I. The Complex Organic Molecules in Perseus Embedded Protostars

The Perseus ALMA Chemistry Survey (PEACHES). I. The Complex Organic Molecules in Perseus Embedded Protostars

Thermal desorption of interstellar ices. A review on the controlling parameters and their implications fromsnowlines to chemical complexity

The Perseus ALMA Chemistry Survey (PEACHES). I. The Complex Organic Molecules in Perseus Embedded Protostars

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