Acoustic and buoyancy modes throughout stellar evolution: Seismic properties of stars at different stellar ages and masses

Parameter regions in which stars can become pulsationally unstable are found throughout the Hertzsprung-Russell diagram. Stars of high, intermediate, low, and very low masses may cross various instability regions along their paths of evolutionary sequences. In describing them, I give special consideration to hybrid pulsational characteristics that are particularly valuable for asteroseismic investigations, to (P) over dot measurements that allow us to directly follow the stellar evolutionary changes in some stars, and to new research results that stand out with respect to previous consensus ((c) 2012 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)