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Title:
The brightest carbon stars
Authors:
Frost, C. A.; Cannon, R. C.; Lattanzio, J. C.; Wood, P. R.; Forestini, M.
Affiliation:
AA( Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK; Department of Mathematics, Monash University, Clayton, Victoria, 3168, Australia), AB( Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK; Department of Physiology and Pharmacology, School of Biological Sciences, University of Southampton, SO16 7PX, UK), AC( Institute of Astronomy, Madingley Road, Cambridge, CB3 0HA, UK; Department of Mathematics, Monash University, Clayton, Victoria, 3168, Australia; Laboratoire d'Astrophysique, Observatoire de Grenoble, UniversiteJoseph Fourier, B.P. 53, F-38041 Grenoble Cedex 9, France), AD(Mount Stromlo and Siding Spring Observatories, The Australian National University, Private Bag, Weston Creek P.O., A.C.T. 2611, Australia), AE(Laboratoire d'Astrophysique, Observatoire de Grenoble, UniversiteJoseph Fourier, B.P. 53, F-38041 Grenoble Cedex 9, France)
Publication:
Astronomy and Astrophysics, v.332, p.L17-L20 (1998) (A&A Homepage)
Publication Date:
04/1998
Origin:
A&A
A&A Keywords:
STARS: AGB, STARS: CARBON STARS, STARS: NUCLEOSYNTHESIS
Bibliographic Code:
1998A&A...332L..17F

Abstract

It is currently accepted that Hot-Bottom-Burning (HBB) in intermediate-mass asymptotic giant branch (AGB) stars prevents the formation of C stars. Nevertheless, we present the results of some detailed evolutionary calculations which show that even with HBB we obtain C stars at the highest luminosities reached on the AGB. This is due to mass-loss reducing the envelope mass so that HBB ceases but dredge-up continues. The high mass-loss rate produces an optically thick wind before the star reaches C/O>1. This is consistent with the recent results of van Loon et al. (1997a,b) who find obscured C stars in the Magellanic Clouds at luminosities up to Mbol =3D -6.8.

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