Water in IRC+10216: a genuine formation process by shock-induced chemistry in the inner wind

TL;DR

This study demonstrates that water forms in the inner wind of IRC+10216 through shock-induced chemistry, matching observations and suggesting a universal process in AGB stars regardless of their C/O ratio.

Contribution

It introduces a detailed chemical kinetic model showing water formation via shocks in the inner wind of carbon stars, a process previously not fully understood.

Findings

Water abundance at 5 R* is 1.4×10^-7, matching Herschel data.

Non-equilibrium chemistry dominates in the dust-formation zone.

Water formation occurs regardless of the stellar C/O ratio.

Abstract

Context: 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 \geq 15 R\ast. Aims: 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. Methods: 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 5 R\ast. We solve for a system of stiff, coupled, ordinary, and differential equations. Results: 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 5 R\ast is 1.4\times10-7, which excellently agrees 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.