  High precision asteroseismic data provide a unique opportunity to test input
microphysics such as stellar opacities, chemical composition or equation of
state. These tests are possible because pulsational frequencies as well as
amplitudes and phases of the light variations are very sensitive to the
internal structure of a star. We can therefore compute pulsation models and
compare them with observations. The agreement or differences should tell us
whether some models are adequate or not, and which input data need to be
improved.
