The 8-14 Micron Feature in S Stars: O Positive or O Negative

Details The 8-14 Micron Feature in S Stars: O Positive or O Negative The 8-14 Micron Feature in S Stars: O Positive or O Negative

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21543101a&link_type=abstract

American Astronomical Society, AAS Meeting #215, #431.01; Bulletin of the American Astronomical Society, Vol. 42, p.362

Astronomy and Astrophysics

Astronomy

Scientific paper

S Stars are Asymptotic Giant Branch (AGB) stars with a carbon-to-oxygen ratio of approximately one. AGB stars expel gas that forms into dust as the gas cools and moves away from the star. Because of the stability of CO, AGB star chemistry is dictated by the C-to-O ratio, such that it determines which element (C or O) is available to form molecules and dust. For S stars, C and O should be equally depleted and unavailable for dust formation. However, the spectral features of S Stars closely resemble those of low mass-loss rate O-rich AGB stars. We investigate whether these apparently similar features can be explained by the same set of minerals, or whether S Stars produce different minerals. In particular we investigate 8-14 micron spectral feature. In addition we examine weak features in the far-IR (>20 microns), which have been used recently to determine detailed mineralogy in low mass-loss rate O-rich AGB stars.

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