Chemical inhomogeneities and pulsation
| dc.creator | Turcotte, S. | |
| dc.date | 2001-11-08 | |
| dc.date.accessioned | 2026-07-07T02:01:18Z | |
| dc.date.available | 2026-07-07T02:01:18Z | |
| dc.description | Major improvements in models of chemically peculiar stars have been achieved in the past few years. With these new models it has been possible to test quantitatively some of the processes involved in the formation of abundance anomalies and their effect on stellar structure. The models of metallic A (Am) stars have shown that a much deeper mixing has to be present to account for observed abundance anomalies. This has implications on their variability, which these models also reproduce qualitatively. These models also have implications for other chemically inhomogeneous stars such as HgMn B stars which are not known to be variable and lambda Bootis stars which can be. The study of the variability of chemically inhomogeneous stars can provide unique information on the dynamic processes occurring in many types of stars in addition to modeling of the evolution of their surface composition. | |
| dc.description | 8 pages, 3 figures, invited review IAU coll. 185 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0111179 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0111179 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/3694 | |
| dc.subject | Astrophysics | |
| dc.title | Chemical inhomogeneities and pulsation | |
| dc.type | text |