SiS Formation in the Interstellar Medium through Si+SH Gas-phase Reactions

Abstract

Abstract Silicon monosulfide is an important silicon-bearing molecule detected in circumstellar envelopes and star-forming regions. Its formation and destruction routes are not well understood, partially due to the lack of detailed knowledge on the involved reactions and their rate coefficients. In this work we have calculated and modeled the potential energy surface (PES) of the HSiS system employing highly accurate multireference electronic structure methods. After obtaining an accurate analytic representation of the PES, which includes long-range energy terms in a realistic way via the DMBE method, we have calculated rate coefficients for the Si+SH → SiS+H reaction over the temperature range of 25–1000 K. This reaction is predicted to be fast, with a rate coefficient of ∼1 × 10−10 cm3 s−1 at 200 K, which substantially increases for lower temperatures (the temperature dependence can be described by a modified Arrhenius equation with α = 0.770 × 10−10 cm3 s−1, β = −0.756, and γ = 9.873 K). An astrochemical gas-grain model of a shock region similar to L1157-B1 shows that the inclusion of the Si+SH reaction increases the SiS gas-phase abundance relative to H2 from 5 × 10−10 to 1.4 × 10−8, which perfectly matches the observed abundance of ∼2 × 10−8.