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

摘要

Parameter regions in which stars can become pulsationally unstable are foundthroughout the Hertzsprung-Russel diagram. Stars of high, intermediate, low andvery low masses may cross various instability regions along their paths ofevolutionary sequences. In describing them, I give special consideration tohybrid pulsational characteristics that are particularly valuable forasteroseismic investigations, to Pdot measurements that allow us to directlyfollow the stellar evolutionary changes in some stars, and to new researchresults that stand out with respect to previous consensus.