Internal mixing and surface abundance of [WC]-CSPN
| dc.creator | Herwig, Falk | |
| dc.date | 1999-12-16 | |
| dc.date.accessioned | 2026-07-07T02:35:03Z | |
| dc.date.available | 2026-07-07T02:35:03Z | |
| dc.description | Recent advances in constructing stellar evolution models of hydrogen-deficient post-asymptotic giant branch (AGB) stars are presented. Hydrogen-deficiency can originate from mixing and subsequent convective burning of protons in the deeper layers during a thermal pulse on the post-AGB (VLTP). Dredge-up alone may also be responsible for hydrogen-deficiency of post-AGB stars. Models of the last thermal pulse on the AGB with very small envelope masses have shown efficient third dredge-up. The hydrogen content of the envelope is diluted sufficiently to produce H-deficient post-AGB stars (AFTP). Moreover, dredge-up alone may also cause H-deficiency during the Born-again phase (LTP). During the second AGB phase a convective envelope develops. A previously unknown lithium enrichment at the surface of Born-again stellar models may be used to distinguish between objects with different post-AGB evolution. The observed abundance ratios of C, O and He can be reproduced by all scenarios if an AGB starting model with inclusion of overshoot is used for the post-AGB model sequence. An appendix is devoted to the numerical methods for models of proton capture nucleosynthesis in the He-flash convection zone during a thermal pulse. | |
| dc.description | 12 pages, 7 figures, conference paper, workshop on "Low mass Wolf-Rayet stars: origin and evolution", 1999, Amsterdam | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9912353 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9912353 | |
| dc.identifier | Astrophys.Space Sci. 275 (2001) 15-26 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/15478 | |
| dc.subject | Astrophysics | |
| dc.title | Internal mixing and surface abundance of [WC]-CSPN | |
| dc.type | text |