The mass-loss and chemistry of S-stars

Details The mass-loss and chemistry of S-stars The mass-loss and chemistry of S-stars

Apr 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006atnf.prop..186r&link_type=abstract

ATNF proposal M177, Semester: April, 2006

Physics

Stellar, Mopra

Scientific paper

Stars of spectral type S are AGB stars with the unique property that the C/O ratio in their photospheres are close to unity. Eventhough S-stars are important as possible transition objects between the oxygen-rich M-stars and carbon stars, little attention has been given to study their properties. We have started a project to remedy this situation. CO radio-line emission and numerical radiative transfer calculations will be used to determine the mass-loss rates and circumstellar physical properties of our sample of 38 S-stars. We will further investigate the circumstellar molecular abundances, starting with SiO, HCN and SiS. This will hopefully shed light on the circumstellar chemistry, and also help to more firmly establish the evolutionary status of S-stars within the AGB.

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