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The recent revision of the solar chemical composition (Asplund, Grevesse andSauval 2005)is characterized by about 40 per cent decrease of C, N, O, Ne, Arabundances and by 20 percent decrease of Fe and some other metal abundances. Wetested the effect of these modifications on the instability of Beta Cepheimodels. For the opacities, the newest OP data from the Opacity Project (Seaton2005) were used. We show that the Beta Cephei instability domain in theHertzsprung-Russel diagram, when computed with new data for Z=0.012 (revisedsolar value), is very similar to the instability domain computed earlier usingthe OPAL opacities for the older solar composition with Z=0.02. Almost allobserved Beta Cephei variables are located within the instability domain. Twoeffects 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 thanthat in the OPAL case, which results in more effective driving; (ii) at a fixedZ value, the new Fe-group abundances are higher than the older ones because theZ value is determined mainly by the abundances of C, N, 0, and Ne.Comment: 2 pages, 2 figures, to appear in Communications in Asteroseismology,  vol.150, 2007 (Proc. Vienna Workshop on the Future of Asteroseismology, held  in Vienna, Sept. 20-22, 2006, eds. G. Handler and G. Houdek

The β Cephei instability domain for the new solar composition and with new OP opacities