2011A&A...526L..11C

The presence of water in the wind of the extreme carbon star IRC+10216 has been confirmed by the Herschel telescope. The regions where the high-J H₂O lines have been detected are close to the star at radii r≤15R_*. We investigate the formation of water and related molecules in the periodically-shocked inner layers of IRC+10216 where dust also forms and accelerates the wind. We describe the molecular formation by a chemical kinetic network involving carbon-and oxygen-based molecules. We then apply this network to the physical conditions pertaining to the dust-formation zone which experiences the passage of pulsation-driven shocks between 1 and 5R_*. We solve for a system of stiff, coupled, ordinary, and differential equations. Non-equilibrium chemistry prevails in the dust-formation zone. H₂O forms quickly above the photosphere from the synthesis of hydroxyl OH induced by the thermal fragmentation of CO in the hot post-shock gas. The derived abundance with respect to H₂ at 5R_* is 1.4x10^–7, which excellently agrees with the values derived from Herschel observations. The non-equilibrium formation process of water will be active whatever the stellar C/O ratio, and H₂O should then be present in the wind acceleration zone of all stars on the Asymptotic Giant Branch.