H2S ice sublimation dynamics: experimentally constrained binding energies, entrapment efficiencies, and snowlines
arXiv:2504.14010 · doi:10.1051/0004-6361/202554068
Abstract
Hydrogen sulfide (H2S) is thought to be an important sulfur reservoir in interstellar ices. It serves as a key precursor to complex sulfur-bearing organics, and has been proposed to play a significant role in the origin of life. Although models and observations both suggest H2S to be present in ices in non-negligible amounts, its sublimation dynamics remain poorly constrained. In this work, we present a comprehensive experimental characterization of the sublimation behavior of H2S ice under astrophysically-relevant conditions. The sublimation behavior of H2S was monitored with a quadrupole mass spectrometer (QMS) during temperature-programmed desorption (TPD) experiments. These experiments are used to determine binding energies and entrapment efficiencies of H2S, which are then employed to estimate its snowline positions in a protoplanetary disk midplane. We derive mean binding energies of 3159\pm46 K for pure H2S ice and 3392\pm56 K for submonolayer H2S desorbing from a compact amorphous solid water (cASW) surface. These values correspond to sublimation temperatures of around 64 K and 69 K in the disk midplane, placing its sublimation fronts at radii just interior to the CO2 snowline. We also investigate the entrapment of H2S in water ice and find it to be highly efficient, with ~75-85% of H2S remaining trapped past its sublimation temperature for H2O:H2S mixing ratios of ~5-17:1. We discuss potential mechanisms behind this efficient entrapment. Our findings imply that, in protoplanetary disks, H2S will mostly be retained in the ice phase until water crystallizes, at radii near the water snowline, if it forms mixed into water ice. This has significant implications for the possibility of H2S being incorporated into icy planetesimals and its potential delivery to terrestrial planets, which we discuss in detail.
Accepted for publication in A&A on April 18th, 2025. 15 pages, 15 figures, 4 tables
References in corpus (25)
- Non-thermal desorption from interstellar dust grains via exothermic surface reactions
- Photochemistry and astrochemistry: photochemical pathways to interstellar complex organic molecules
- An Ice Age JWST inventory of dense molecular cloud ices
- Complex organic molecules in protoplanetary disks
- Binding energies: new values and impact on the efficiency of chemical desorption
- Modeling Sulfur Depletion in Interstellar Clouds
- Atom addition reactions in interstellar ice analogues
- Sensitivity analysis of grain surface chemistry to binding energies of ice species
- Thermal desorption of circumstellar and cometary ice analogs
- Sulphur-bearing molecules in diffuse molecular clouds: new results from SOFIA/GREAT and the IRAM 30 m telescope
- Sulphur-bearing species in the star forming region L1689N
- Modelling the sulphur chemistry evolution in Orion KL
- A new look at sulphur chemistry in hot cores and corinos
- Abundant ammonium hydrosulphide embedded in cometary dust grains
- The complex chemistry of outflow cavity walls exposed: the case of low-mass protostars
- Pore evolution in interstellar ice analogues: simulating the effects of temperature increase
- Laboratory and Computational Studies of Interstellar Ices
- Bottlenecks to interstellar sulfur chemistry: Sulfur-bearing hydrides in UV-illuminated gas and grains
- Ammonium hydrosulfide (NH4SH) as a potentially significant sulfur sink in interstellar ices
- Desorption Kinetics and Binding Energies of Small Hydrocarbons
- Formation of S-bearing complex organic molecules in interstellar clouds via ice reactions with C2H2, HS, and atomic H
- AB Aur, a Rosetta stone for studies of planet formation (II): HS detection and sulfur budget
- HS observations in young stellar disks in Taurus
- Formation of carbonyl sulfide (OCS) via SH radicals in interstellar CO-rich ice under dense cloud conditions
- Computational Estimation of the Binding Energies of POx and HPOx (x=2,3) Species