Astronomy and Astrophysics – Astrophysics
Scientific paper
2007-03-28
Astronomy and Astrophysics
Astrophysics
2 pages, 2 figures, to appear in Communications in Asteroseismology, vol.150, 2007 (Proc. Vienna Workshop on the Future of Ast
Scientific paper
10.1553/cia150s207
The recent revision of the solar chemical composition (Asplund, Grevesse and Sauval 2005)is characterized by about 40 per cent decrease of C, N, O, Ne, Ar abundances and by 20 percent decrease of Fe and some other metal abundances. We tested the effect of these modifications on the instability of Beta Cephei models. For the opacities, the newest OP data from the Opacity Project (Seaton 2005) were used. We show that the Beta Cephei instability domain in the Hertzsprung-Russel diagram, when computed with new data for Z=0.012 (revised solar value), is very similar to the instability domain computed earlier using the OPAL opacities for the older solar composition with Z=0.02. Almost all observed Beta Cephei variables are located within the instability domain. Two effects are responsible for stronger instability when using the new data: (i) Metal opacity bump in the OP case is located slightly deeper in the star than that in the OPAL case, which results in more effective driving; (ii) at a fixed Z value, the new Fe-group abundances are higher than the older ones because the Z value is determined mainly by the abundances of C, N, 0, and Ne.
Pamyatnykh Alexey A.
Ziomek W.
No associations
LandOfFree
The Beta Cephei instability domain for the new solar composition and with new OP opacities does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The Beta Cephei instability domain for the new solar composition and with new OP opacities, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Beta Cephei instability domain for the new solar composition and with new OP opacities will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-271971