compare two very close modes: the unstable one with $\nu=0.160$ c/d and $\eta=0.067$ and the stable one with $\nu=0.162$ c/d and $\eta=-1.000$. Their kinetic energy densities and differential work integrals are shown in the right group of panels in Fig.\[fig5\]. The behavior of $E_k$ is different for these modes than for the modes from the Model1. The entire energy of the stable mode is confined to the radiative zone in-between the convective core and the ICZ (there is strong damping in this region of the star), whereas the unstable mode has almost all of its energy trapped in the outer radiative zone. That means that the unstable modes of the blue loop models have to be almost entirely reflected at the ICZ. This fact might be the explanation why we do have far fewer unstable modes from models burning helium in its core than from models before core helium ignition and also the lack of the structure of $\eta$ observed in Model1. The behaviour of kinetic energy density depicted in Fig.\[fig5\] is typical for all unstable and stable modes both during hydrogen shell burning and on the blue loops.

Photometric amplitudes and phases of pulsations in early B-type supergiants {#identification}
