Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.9314a&link_type=abstract
American Astronomical Society, AAS Meeting #211, #93.14; Bulletin of the American Astronomical Society, Vol. 39, p.891
Astronomy and Astrophysics
Astronomy
Scientific paper
Intermediate mass stars (0.8 to 8 solar masses) evolve into an astronomically brief phase known as the asymptotic giant branch (AGB). In this phase, strong convection currents in the star dredge up the materials formed from processes occurring in the star interior, predominantly carbon from He-burning, and s-process elements. The subsequent stellar atmospheric chemistry depends on the C/O ratio. S Stars are commonly regarded as having evolved from oxygen-rich M stars through dredge-up of carbon and have C/O close to one. This results in most of the carbon and oxygen being locked up in carbon monoxide. Based on infrared spectroscopy, the dust around S Stars appears to be dominated by either alumina (which is oxygen-rich) or silicon carbide (SiC; which is carbon-rich). And it has been hypothesized that at precisely C/O=1, the dust should be dominated by nitrogen and/or sulphur. By modeling these spectra in detail and comparing the derived mineralogies to the C/O ratios we can test dust formation theories. We present preliminary models of the ISO SWS spectra of S stars and compare with previous derived mineralogies.
Arrant David J.
Speck Angela
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