Dust around evolved stars in the Magellanic Clouds

Details Dust around evolved stars in the Magellanic Clouds Dust around evolved stars in the Magellanic Clouds

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aas...206.0603r&link_type=abstract

American Astronomical Society Meeting 206, #06.03; Bulletin of the American Astronomical Society, Vol. 37, p.435

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We present newly reduced ISO mid-IR spectra of a selection of (Small and Large) Magellanic Cloud evolved stars and derive their mineralogies. The spectra are classified according to the morphology of the observed spectral features and their derive mineralogies. Sequences in this classification scheme can then be used to determine the effects of density, chemistry and metallicity on dust formation mechanisms.
Correlating the observed spectral trends with previously determined mass-loss rates for these evolved stars allows us to assess the effect of the density of the circumstellar shell on dust formation processes. Furthermore, the mineralogical sequences will be compared with the positions of these stars in color-color and color-magnitude diagrams in order to assess the effect of the chemistry in the circumstellar shells on dust formation. Finally, we will compare the results of these studies for the LMC and SMC, as well as with Milky Way objects, to determine the effect of metallicity on dust formation processes.

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