No CrossRef data available.
Article contents
B Star Pulsation - Theory and Seismological Prospects
Published online by Cambridge University Press: 08 February 2017
Extract
Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.
Progress in understanding B-type pulsators has been reviewed at several recent meetings (e.g. Dziembowski, 1993, 1995; Moskalik, 1995). Not much happened afterwards. Owing to further improvement in the stellar opacity calculations (Iglesias and Rogers 1996), the theoretical pulsation-instability domain in the upper Main Sequence is now more precisely determined. In the next section I will compare the predicted domain with the positions of various B-type pulsators in the H-R diagram.
- Type
- VI. Asteroseismology II
- Information
- Symposium - International Astronomical Union , Volume 185: New Eyes to See Inside the Sun and Stars , 1998 , pp. 355 - 360
- Copyright
- Copyright © Kluwer 1998
References
Dziembowski, W.A., 1993, in Balona, L.A., Henrichs, H.F. and Le Contel, J.M. (eds), IAU Symposium No. 162 – Pulsation, Rotation and Mass Loss in Early-Type Stars, 55
Google Scholar
Dziembowski, W.A., 1995, in Adelman, S.J. and Wiese, W.L. (eds), Astrophysical Applications of Powerful New Databases, (ASP Conf. Ser.), 275
Google Scholar
Moskalik, P., 1995, in Stobie, R.S. and Whitelock, P.A. (eds), Astrophysical Application o, Stellar Pulsation, (ASP Conf. Ser), 44
Google Scholar
Pamyatnykh, A.A., 1997, in Bradley, P.A. and Guzik, J.A. (eds), A Half Century of Stellar Pulsation Interpretation, (ASP Conf. Ser), in press
Google Scholar
You have
Access