2005ApJ...634..602R

Asteroseismology has successfully been applied to our Sun, white dwarfs, Cepheids, and a few other classes of variable stars to discern their internal properties. However, the success of applying asteroseismology depends on the determination of pulsation spherical harmonics, which is often difficult. To facilitate mode identifications, we investigate a new tool for asteroseismology: pulsating stars in close binaries, with an emphasis on pulsating subdwarf B stars. In this work we consider variations in the inclination of the pulsation spherical harmonics to the rotation axis and the impact of changing viewing geometry caused by eclipses (eclipse mapping).