O(He) Stars
| dc.creator | Rauch, T. | |
| dc.creator | Reiff, E. | |
| dc.creator | Werner, K. | |
| dc.creator | Kruk, J. W. | |
| dc.date | 2008-04-15 | |
| dc.date.accessioned | 2026-07-07T09:32:42Z | |
| dc.date.available | 2026-07-07T09:32:42Z | |
| dc.description | Spectral analyses of H-deficient post-AGB stars have shown that a small group of four extremely hot objects exists which have almost pure He absorption-line spectra in the optical. These are classified as O(He) stars. For their evolution there are two scenarios: They could be the long-sought hot successors of RCrB stars, which have not been identified up to now. If this turns out to be true, then a third post-AGB evolutionary sequence is revealed, which is probably the result of a double-degenerate merging process. An alternative explanation might be that O(He) stars are post early-AGB stars. These depart from the AGB just before they experience their first thermal pulse (TP) which will then occur as a late thermal pulse (LTP). This would be a link to the low-mass He-enriched sdO stars and low-mass, particularly He-rich PG1159 stars. | |
| dc.description | 4 pages, 1 figure | |
| dc.identifier | https://arxiv.org/abs/0804.2366 | |
| dc.identifier | http://arxiv.org/abs/0804.2366 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/158872 | |
| dc.subject | Astrophysics | |
| dc.title | O(He) Stars | |
| dc.type | text |