THE 10 μm FEATURE OF M-TYPE STARS IN THE LARGE MAGELLANIC CLOUD AND THE DUST CONDENSATION SEQUENCE

摘要

We present 7-14 μm 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 μm 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 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 betweenM and the peak wavelength position of the broad dust feature. Our data suggest a strong dependence of the dust mineralogy on the temperature at the dust condensation radius.