A chemical study of the inner winds of asymptotic giant branch stars

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Mass loss of stars on the asymptotic giant branch (2018, background): “Further possible sources of uncertainty are non-equilibrium effects in the gas-phase chemistry, introduced by strong atmospheric shock waves (e.g., Cherchneff 2006, 2011, 2012), or non-LTE radiative cooling of the shocked gas (e.g., Willson 2000; Schirrmacher et al. 2003).”
Production of dust by massive stars at high redshift (2011, background): “Apart from the molecules formed only in specific environments (C- or O-rich), species such as CO, SiO, HCN andCS have been found theoretically and observationally in all types of AGB stars (e.g., Cherchneff, 2006; Decin et al,”
Dust formation in the oxygen-rich AGB star IK Tauri (2015, methodology): “…environments and carbon atoms in oxygen-rich environments, leading to a dual chemistry that forms O-bearing species like water, H2O, in the wind of carbon stars, and C-bearing species in the wind of O-rich AGBs (Willacy & Cherchneff 1998; Duari et al. 1999; Cherchneff 2006, 2011a, 2012).”