The Brightest Carbon Stars
| dc.creator | Frost, Cheryl | |
| dc.creator | Cannon, Robert | |
| dc.creator | Lattanzio, John | |
| dc.creator | Wood, Peter | |
| dc.creator | Forestini, Manuel | |
| dc.date | 1997-10-06 | |
| dc.date.accessioned | 2026-07-07T02:24:25Z | |
| dc.date.available | 2026-07-07T02:24:25Z | |
| dc.description | 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 in this paper 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 M_{bol} = -6.8. | |
| dc.description | 4 pages, 2 figures included. Note that these are quality-reduced figures for net transmission. If you want best quality figures, these are available from http://www.maths.monash.edu.au/~johnl/preprints/preprints.html | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9710054 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9710054 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/11614 | |
| dc.subject | Astrophysics | |
| dc.title | The Brightest Carbon Stars | |
| dc.type | text |