referred to as rapidly oscillating ?² Canum Venaticorum variables. Both the roAp stars and some ?² CVn variables lie on the ? Scuti instability strip and are magnetic chemically peculiar stars, but the roAp stars have very short periods less than an hour.

Oscillations

The roAp stars oscillate in high-overtone, low-degree, non-radial pressure modes. The usual model that is used to explain the behavior

1.Previous
3.Next