Shaping Planetary Nebulae: is it different for [WR] stars?
| dc.creator | Mellema, Garrelt | |
| dc.date | 1999-10-19 | |
| dc.date.accessioned | 2026-07-07T02:33:56Z | |
| dc.date.available | 2026-07-07T02:33:56Z | |
| dc.description | This review discusses the physics of the formation of planetary nebulae around low mass WR stars, or [WR] stars. It especially focuses on the differences which can be expected due to the different character of the fast winds from these [WR] stars. Their fast winds are more massive and are highly H deficient and metal enriched compared to the winds of normal central stars of planetary nebulae. This is expected to lead to faster expansion velocities for the nebulae and a longer momentum-driven phase in the evolution of the wind-driven bubble, leading to more turbulent nebulae. The observational evidence also shows that the process which produces the [WR] stars is unlikely to influence the onset of aspherical mass loss, something which can be used as a test for models for aspherical mass loss from AGB and post-AGB stars. Finally it is shown that the nebular characteristics rule out a very late He shell flash as the origin of most [WR] stars. | |
| dc.description | 11 pages, 2 figures, to appear in the proceedings of "Low mass Wolf-Rayet Stars: origin and evolution", eds. L.B.F.M. Waters, A.A. Zijlstra (Astrophysics and Space Science) | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9910343 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9910343 | |
| dc.identifier | Astrophys.Space Sci. 275 (2001) 147-157 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/15047 | |
| dc.subject | Astrophysics | |
| dc.title | Shaping Planetary Nebulae: is it different for [WR] stars? | |
| dc.type | text |