The effect of selective desorption mechanisms during interstellar ice formation

TL;DR

This study models the effects of selective desorption mechanisms on interstellar ice formation, revealing the role of photodesorption and reactive desorption in chemical complexity and molecule distribution in molecular clouds.

Contribution

It introduces a layered ice model with specific desorption processes, highlighting the importance of subsurface chemistry and desorption in explaining observed molecular abundances.

Findings

Photodesorption governs initial ice accumulation.

Reactive desorption affects complex organic molecule abundances.

Model reproduces observed H2O:CO:CO2 ratios in dark cores.

Abstract

Major components of ices on interstellar grains in molecular clouds - water and carbon oxides - occur at various optical depths. This implies that selective desorption mechanisms are at work. An astrochemical model of a contracting low-mass molecular cloud core is presented. Ice was treated as consisting of the surface and three subsurface layers (sublayers). Photodesorption, reactive desorption, and indirect reactive desorption were investigated. The latter manifests itself through desorption from H+H reaction on grains. Desorption of shallow subsurface species was included. Modeling results suggest the existence of a "photon-dominated ice" during the early phases of core contraction. Subsurface ice is chemically processed by interstellar photons, which produces complex organic molecules. Desorption from the subsurface layer results in high COM gas-phase abundances at Av = 2.4...10mag. This may contribute towards an explanation for COM observations in dark cores. It was found that photodesorption mostly governs the onset of ice accumulation onto grains. Reaction-specific reactive desorption is efficient for small molecules that form via highly exothermic atom-addition reactions. Higher reactive desorption efficiency results in lower gas-phase abundances of COMs. Indirect reactive desorption allows to closely reproduce the observed H2O:CO:CO2 ratio towards a number of background stars. Presumably this can be done by any mechanism whose efficiency fits with the sequence CO > CO2 >> H2O. After the freeze-out has ended, the three sublayers represent chemically distinct parts of the mantle. 8...10.5mag is the likely AV threshold for the appearance of CO ice. The lower value is supported by observations.