White dwarf stars are the final evolutionary stage of the vast majority of stars, including our
Sun. Since the coolest white dwarfs are very old objects, the present population of white …

▪ Abstract Stars over essentially the whole mass domain can become pulsationally unstable
during various stages of their evolution. They will appear as variable stars with …

We present a summary of what is currently known about the three distinct families of isolated
pulsating white dwarfs. These are the GW Vir stars (He/C/O-atmosphere stars with T eff≃ …

We show that the opal opacities, in addition to explaining the origin of the pulsations of β
Cep stars, also predict the existence of a large region in the main-sequence band at lower …

We report on the analysis of 154 hours of early continuous high-speed photometry on the
pulsating DB white dwarf (DBV) GD 358, obtained during the Whole Earth Telescope (WET) …

Probing internal properties of white-dwarf stars has been amongst the earliest objectives of
asteroseismology, following the first discovery in the late 1960s of non-radial pulsations in …

Asteroseismology provides us with a unique opportunity to improve our understanding of
stellar structure and evolution. Recent developments, including the first systematic studies of …

Context. The recent arrival of continuous photometric observations of unprecedented quality
from space missions has strongly promoted the study of pulsating stars and caused great …

An adiabatic, nonradial pulsation study of GW Vir stars is presented. The pulsation
calculations were based on PG 1159 evolutionary sequences with different stellar masses …

Asteroseismology ADS Classic is now deprecated. It will be completely retired in October 2019.
This page will automatically redirect to the new ADS interface at that point. SAO/NASA ADS …