The Maser-emitting Structure and Time Variability of the SiS Lines J=14−13 and 15-14 in IRC+10216

Abstract

AGB stars are important contributors of processed matter to the ISM. However, the physical and chemical mechanisms involved in its ejection are still poorly known. This process is expected to have remarkable effects in the innermost envelope, where the dust grains are formed, the gas is accelerated, the chemistry is active, and the radiative excitation becomes important. A good tracer of this region in C-rich stars is SiS, an abundant refractory molecule that can display maser lines, very sensitive to changes in the physical conditions. We present high angular resolution interferometer observations (HPBW ≳0.″.25) of the v = 0 J = 14 – 13 and 15 – 14 SiS maser lines towards the archetypal AGB star IRC+10216, carried out with CARMA and ALMA to explore the inner 1” region around the central star. We also present an ambitious monitoring of these lines along one single pulsation period carried out with the IRAM 30 m telescope.

(Sub)mm Observations of Evolved Stars

“…For water masers, results have included those for terahertz masers (Neufeld et al 2021) and 658 GHz masers (Baudry et al 2018). For HCN masers, recent results have included those of Menten et al (2018), Wong et al (2019), Fonfría et al (2019) and Jeste et al (2022). SiS masers have been imaged using ALMA towards IRC+10216 (Fonfría et al 2018).…”