Understanding Dust Formation around AGB Stars: Rethinking the Condensation Sequence around S Stars

Details Understanding Dust Formation around AGB Stars: Rethinking the Condensation Sequence around S Stars Understanding Dust Formation around AGB Stars: Rethinking the Condensation Sequence around S Stars

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008aas...212.0608a&link_type=abstract

American Astronomical Society, AAS Meeting #212, #6.08; Bulletin of the American Astronomical Society, Vol. 40, p.196

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Scientific paper

S Stars occupy a unique place in the parameter space that needs to be investigated for understanding dust formation. In these stars, C/O = 1 which is expected to have some interesting effects on dust formation. The shape, position and strength of dusty spectral features in S stars vary, but a commonly seen broad feature at 8-14 microns has been attributed to various forms of silicate and oxides (mostly alumina). In addition, the identification of these features has been largely qualitative, with little to no radiative transfer modeling applied. Furthermore, dust around S Stars need not be dominated by oxygen or carbon; a mixture of oxygen-rich and carbon-rich dust species is possible. We show a detailed comparison of this 8-14 micron feature is S star spectra to the 11 micron silicon carbide feature in carbon star spectra, and also to various features seen in O-rich AGB star spectra. Moreover, we present preliminary radiative transfer modeling of 2 S Stars with the 8-14 micron feature, which investigates a broad compositional/mineralogical parameter space for these stars.

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