Evolution and mass loss of AGB stars in the Magellanic clouds

Details Evolution and mass loss of AGB stars in the Magellanic clouds Evolution and mass loss of AGB stars in the Magellanic clouds

Mar 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999esasp.427..273b&link_type=abstract

The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 273

Physics

1

Carbon Stars, Agb Stars, Mass-Loss, Circumstellar Matter, Magellanic Clouds

Scientific paper

We used ISOCAM and ISOPHOT to observe the spectral energy distribution (SED) between 3.6 and 60 μm of Asymptotic Giant Branch (AGB) stars in the Magellanic Clouds (MCs) detected by IRAS. PHT-S and CAM-CVF spectra are made which enable us to establish the carbon- or oxygen-rich nature of the stars. The 9.7 μm silicate feature gives a measure of the optical depth of the dust shell. Ground-based near-infrared data has been obtained for the full sample. We are analysing the SEDs using radiative transfer models which provide accurate determinations of the luminosities and mass-loss rates of the objects. Combining the data on the SMC, LMC and existing data on the Galaxy will answer the open question of the metallicity dependence of mass loss in late-type stars. This in turn is important in the ejection of matter by AGB stars to the interstellar medium over the age of the Galaxy.

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