Asteroseismological Models with Rotation

The low frequency NRP oscillations are considered in the case of differential rotation. Partial differential equations for adiabatic oscillations are reduced to a system of ordinary equations by means of a truncated spherical-harmonic expansion. The numerical method for solving the system is described. The final model also includes line profile variations (lpv) and posttheoretical mass (pth) calculations for the complete determinations of the physical, chemical, rotational and seismological properties of the stars.