摘要：When calculating the models discussed in the article, CO self-
shielding was erroneously not taken into account. The CO
photodissociation rates are therefore smaller than those used in
the article. The lower photodissociation rate leads to a lower
abundance of C and O close to the star, which influences our
results. While clumping and porosity still affects the chemistry
throughout the outflow, the formation of C-bearing species in
O-rich outflows and vice versa is not as large, as their forma-
tion depends on the abundance of the deficient element. The
chemistry of N- and S-bearing species is largely unaffected.
关键词：Key wordsenastrochemistrymolecular processescircumstellar matterstars: AGB and post-AGBISM: moleculeserrata, addenda
