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doi: 10.1086/498415We present 7-14 mm Infrared Space Observatory (ISO) spectroscopy of 12 M-type evolved stars in the Large Magellanic Cloud (LMC), in order to study the dust mineralogy and condensation process around these stars. The sample stars show a broad dust feature in the 7-14 mm region, which is seen in either emission or (self-) absorption. The shape of the feature changes with increasing mass-loss rate, M, suggesting a change in dust ˙M mineralogy as the central star evolves. At low mass-loss rates amorphous alumina and amorphous silicates are observed, while at high mass- loss rates only amorphous silicates are seen, in agreement with the classical condensation sequence expected for these materials.We find a clear correlation between and the peak wavelength ˙M position of the broad dust feature. Our data suggest a strong dependence of the dust mineralogy on the temperature at the dust condensation radius.This work was supported by the NASA Astrophysical Data Program (NAG 5-12675) and the University of Missouri Research Board

The 10 μm Feature of M-Type Stars in the Large Magellanic Cloud and the Dust Condensation Sequence