Stellar wind signatures in sdB stars?
| dc.creator | Heber, U. | |
| dc.creator | Maxted, P. F. L. | |
| dc.creator | Marsh, T. R. | |
| dc.creator | Knigge, C. | |
| dc.creator | Drew, J. E. | |
| dc.date | 2002-12-20 | |
| dc.date.accessioned | 2026-07-07T02:06:59Z | |
| dc.date.available | 2026-07-07T02:06:59Z | |
| dc.description | Subdwarf B (sdB) stars form the blue end of the horizonal branch. Their peculiar atmospheric abundance patterns are due to diffusion processes. However, diffusion models fail to explain these anomalies quantitatively. From a NLTE model atmosphere analysis of 40 sdB stars, we found that the more luminous (i.e. more evolved) stars have anomalous H alpha and HeI 6678Ang line profiles, i.e, the lines are too broad and shallow and may even show some emission. We interpret these anomalies as the signatures of a stellar wind, the first such detection in this class of star (if confirmed). Mass loss may also explain the peculiar abundance patterns seen in sdB stars. High-quality UV spectra are needed to confirm that these stars do have stellar winds. | |
| dc.description | 4 pages, 3 figures, To appear in: Stellar Atmosphere Modeling, eds. I. Hubeny, D. Mihalas, K. Werner, ASP Conference Series | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0212493 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0212493 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/5552 | |
| dc.subject | Astrophysics | |
| dc.title | Stellar wind signatures in sdB stars? | |
| dc.type | text |