Observations and Interpretations of Stellar Pulsations

Abstract

The three most useful methods for the identification of the stellar pulsation modes are described: firstly, the method based on the values of the period P and/or pulsation quantity Q; secondly, the method using the profile variations of the photospheric lines; thirdly, the method using the amplitudes and phases of the light, colour and radial velocity curves. Some of the most significant examples are given for each method, taken among the Cepheid, RR Lyrae, ß Cephei and δ Scuti stars.

For two classes the complex variability of stars is described in detail: the 53 Persei stars and the supergiants. In these two classes non-radial modes have been identified and the complete mode identification has still to be largely improved.