| Issue |
A&A
Volume 423, Number 2, August IV 2004
|
|
|---|---|---|
| Page(s) | 705 - 715 | |
| Section | Stellar atmospheres | |
| DOI | https://doi.org/10.1051/0004-6361:20041012 | |
| Published online | 06 August 2004 | |
The spectroscopic signature of roAp stars*
1
Department of Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria e-mail: first_name@astro.univie.ac.at
2
Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya 48, 109017 Moscow, Russia e-mail: ryabchik@inasan.rssi.ru
3
European Southern Observatory, Casilla 19001, Santiago 19, Chile
4
Uppsala Astronomical Observatory, Box 515, 751 20 Uppsala, Sweden
Received:
2
April
2004
Accepted:
10
May
2004
To reliably determine the spectroscopic signature of rapidly oscillating chemically peculiar (roAp) stars it is also necessary to investigate a sample of non pulsating chemically peculiar (noAp) as well as presumably “normal” stars. We describe in this study the sample of spectroscopically investigated stars and comment on the techniques used for the analysis. In particular we discuss ionization disequilibria of rare earths in roAp stars that distinguish them from noAp stars. In the light of the recently discovered pulsation of β CrB we see arguments that all magnetic CP2 stars up to a transition temperature of about 8100 K may be pulsating.
Key words: stars: abundances / stars: atmospheres / stars: chemically peculiar / stars: oscillations
© ESO, 2004
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