In Paper I we decribed in detail the basic disk model and properties of the m=1 eigenmodes in equatorial disks of Be stars. The disk model adopted in this paper is the same as that adopted in Paper I, except that the present model includes the quadrupole contribution to the potential of a rotationally distorted central star, according to Papaloizou et al. (1992) and Savonije and Heemskerk (1993). As shown below, however, including the quadrupole contribution to the potential does not affect the eigenmodes qualitatively. Hence, in this section we give only a brief summary of the unperturbed disk model and the m=1 perturbation patterns.