Sulfur chemistry: 1D modeling in massive dense cores

TL;DR

This study models sulfur chemistry in massive dense cores using 1D simulations to compare observed molecular abundances with chemical evolution, aiming to infer the evolutionary stages of these cores.

Contribution

It applies a 1D chemical model with gas-grain interactions to high-mass cores, providing insights into sulfur molecule abundances and core ages, highlighting the importance of physical conditions.

Findings

CS is underproduced in the model compared to observations.

Abundance ratios like OCS/SO2 can trace protostar age, but are limited by observational uncertainties.

W43-MM1 appears to be chemically younger than other cores.

Abstract

The main sulfur-bearing molecules OCS, H2S, SO, SO2, and CS have been observed in four high mass dense cores (W43-MM1, IRAS 18264, IRAS 05358, and IRAS 18162). Our goal is to put some constraints on the relative evolutionary stage of these sources by comparing these observations with time-dependent chemical modeling. We used the chemical model Nahoon, which computes the gas-phase chemistry and gas-grain interactions of depletion and evaporation. Mixing of the different chemical compositions shells in a 1D structure through protostellar envelope has been included since observed lines suggest nonthermal supersonic broadening. Observed radial profiles of the temperature and density are used to compute the chemistry as a function of time. With our model, we underproduce CS by several orders of magnitude compared to the other S-bearing molecules, which seems to contradict observations, although some uncertainties in the CS abundance observed at high temperature remain. The OCS/SO2, SO/SO2, and H2S/SO2 abundance ratios could in theory be used to trace the age of these massive protostars since they show a strong dependence with time, but the sources are too close in age compared to the accuracy of chemical models and observations. Our comparison between observations and modeling may, however, indicate that W43-MM1 could be chemically younger than the three other sources. Turbulent diffusivity through the protostellar envelopes has to be less efficient than 2e14 cm2s-1. Otherwise, it would have smoothed out the abundance profiles, and this would have been observed. The sulfur chemistry depends strongly on the 1D physical conditions. In our case, no conclusion can be given on the relative age of IRAS 18264, IRAS 18162 and IRAS 05358 except that they are very close. W43-MM1 seems younger than the other sources.