Stability of sulphur dimers S2 in cometary ices

TL;DR

This study investigates the stability and formation conditions of S2 molecules in cometary ices, suggesting they form via irradiation in low-density environments and remain trapped until sublimation, consistent with observed comet compositions.

Contribution

It provides a new model for S2 formation and stability in cometary ices, linking irradiation processes to the presence of S2 and molecular oxygen in comets.

Findings

S2 stabilization energy is similar to H2O ice binding energy.

S2 formation occurs in low-density, cold environments like ISM or protosolar nebula.

S2 remains trapped in ices until sublimation, explaining its short vapor-phase lifetime.

Abstract

S2 has been observed for decades in comets, including comet 67P/Churyumov-Gerasimenko. Despite the fact that this molecule appears ubiquitous in these bodies, the nature of its source remains unknown. In this study, we assume that S2 is formed by irradiation (photolysis and/or radiolysis) of S-bearing molecules embedded in the icy grain precursors of comets, and that the cosmic ray flux simultaneously creates voids in ices within which the produced molecules can accumulate. We investigate the stability of S2 molecules in such cavities, assuming that the surrounding ice is made of H2S or H2O. We show that the stabilization energy of S2 molecules in such voids is close to that of the H2O ice binding energy, implying that they can only leave the icy matrix when this latter sublimates. Because S2 has a short lifetime in the vapor phase, we derive that its formation in grains via irradiation must occur only in low density environments such as the ISM or the upper layers of the protosolar nebula, where the local temperature is extremely low. In the first case, comets would have agglomerated from icy grains that remained pristine when entering the nebula. In the second case, comets would have agglomerated from icy grains condensed in the protosolar nebula and that would have been efficiently irradiated during their turbulent transport towards the upper layers of the disk. Both scenarios are found consistent with the presence of molecular oxygen in comets.