The influence of the solar atmospheric stratification on the form of p-mode ridges

We investigate properties of non-radial solar p-modes of high angular degree. We consider linear adiabatic oscillations with the transition layer as an ideal reflector Ionization of hydrogen and helium and dissociation of hydrogen are included in the equation of state and consequently in the adiabatic sound speed. Because of the restriction to high-degree modes we use the plane layer approximation with constant gravity. Our standard atmospheric model is the VAL-C atmosphere. This atmosphere is joined to the upper part of a convection zone. A model corona is matched to the transition region. Boundary conditions are applied at the temperature maximum of the corona and at a depth in the convection zone far below the lower turning point of the non-radial p-modes determined by the Lamb-frequency, We vary the temperature stratification of the atmosphere and shift the position of the transition region to obtain a family of eight different equilibrium models. By this strategy we can study the formation of structures in the diagnostic diagram and we can take into account uncertainties of the VAL-chromosphere. It is shown how the classical p-modes of a convection zone with zero pressure boundary condition are deformed when the thickness of the overlying atmosphere is enlarged. In no case, the atmosphere generates additional modes. By strong bending, horizontally passing parts of the ridges are formed. These parts produce more or less pronounced chromospheric ridges or features. These chromospheric ridges appear at frequencies where observations show enhanced power in the diagnostic diagram. Their locations sensitively depend on the atmospheric model. A simple two layer model shows that the occurence of bending of the ridges in the diagnostic diagram is quite natural and independent of atmospheric details.