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We present a diagnostic tool to determine the forsterite abundance of thedust ejected by AGB stars. Our method is based on a comparison between theobserved strength of spectral bands of forsterite and model calculations. Weshow that the 11.3 {\mu}m forsterite band is a robust indicator of theforsterite abundance of the current mass-loss period for AGB stars with anoptically thick dust shell. The 33.6 {\mu}m band of forsterite is sensitive tochanges in the density and the geometry of the emitting dust shell, and so aless robust indicator. We apply this method to six high mass-loss rate AGBstars, showing that AGB stars can have forsterite abundances of 12% by mass andhigher, which is more than the previously found maximum abundance of 5%.

Determining the forsterite abundance of the dust around AGB stars