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Fig. 1


Schematic structure of the CSE for an O-rich AGB star, which is divided into six regions for modeling purposes. (I): a degenerate C/O core and He/H burning shell; (II): a convective atmosphere; (III): a shocked inner wind where some parent species (mainly H2O, CO, and SiO) are formed; (IV): an intermediate expanding envelope where gas-phase chemistry may play a role; (V): an outer CSE where daughter species are formed primarily by photodissociation; (VI): the interstellar medium (ISM). This study focusses on the outer CSE where chemistry is mainly driven by the photodissociation and photoionization of molecules.

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