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![image](fig6a.eps){width="88mm"} ![image](fig6b.eps){width="88mm"}

![image](fig7a.eps){width="85mm"} ![image](fig7b.eps){width="85mm"}

In our previous paper (D2013), we have shown that one should not expect regular patterns in the oscillation spectra of blue supergiants which the asymptotic theory predicts for g-mode pulsations. However, it turned out that there is a prospect for identification of the degree, $\ell$, for modes excited in the blue supergiant models before core helium ignition from photometric diagnostic diagrams (D2013). Here, we will check whether the photometric amplitudes and phases of pulsations in models after core helium ignition have similar properties.

The expression for the complex amplitudes of the light variations in a given passband within the linear and zero-rotation approximation can be found, e.g., in Daszyńska-Daszkiewicz et al. (2002), and need not be repeated here. To compute the values of these observables, we used the nonadiabatic pulsational code of Dziembowski (1977) and tables of the fluxes in photometric passbands and nonlinear limb-darkening coefficients computed by Daszyńska-Daszkiewicz & Szewczuk (2011) on the basis of the NLTE atmosphere models of Lanz & Hubeny (2007).

In Fig.\[fig6\], we show positions of unstable modes with the degree $\ell=0-2$ excited in the supergiant models in the photometric diagnostic diagrams employing the $B$ and $R$ Johnson filters. These 