HCN in the inner envelope of chi Cygni
Debiprosad Duari, Jennifer Hatchell
Abstract
We have detected the (0,11c,0)J=3-2 and (0,0,0)J=8-7 transitions of HCN towards the S star chi Cygni. The excitation requirements of these transitions are too high to be satisfied in the outer envelope of the star, and the emission must originate within solar20 stellar radii, ie. the molecule must be forming close to the star. This conclusion is supported by a model for AGB stars in which molecules including HCN form in a shocked wind close to the stellar surface.
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