Microscopic diffusion and subdwarfs
| dc.creator | Morel, P. | |
| dc.creator | Baglin, A. | |
| dc.date | 1999-02-10 | |
| dc.date.accessioned | 2026-07-07T02:30:25Z | |
| dc.date.available | 2026-07-07T02:30:25Z | |
| dc.description | The recent distance determinations by HIPPARCOS have allowed to locate very precisely a reasonable set of subdwarfs in the HR diagram. A detailed comparison with evolutionary models is now possible and it has been recently claimed that the observed lower part of the main-sequence is cooler than the computed one. In this paper we show that microscopic diffusion could be the physical explanation of such a systematic shift. We emphazise the fact that, as diffusion alters surface abundances, the initial metal content of the stellar material is higher than the present one. A "calibration" procedure is necessary when comparing observed and theoretical HR diagram, to take into account this effect. | |
| dc.description | latex A&A, 8 pages, 8 figures, accepted by A&A | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9902160 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9902160 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/13807 | |
| dc.subject | Astrophysics | |
| dc.title | Microscopic diffusion and subdwarfs | |
| dc.type | text |