  We study the effect of non-radial motions, originating from the gravitational
interaction of the quadrupole moment of a protogalaxy with the tidal field of
the matter of the neighboring protostructures, on the angular correlation
function of galaxies. We calculate the angular correlation function using a
Standard Cold Dark Matter (hereafter SCDM) model (Omega=1, h=0.5, n=1) and we
compare it with the angular correlation function of the APM galaxy survey
(Maddox et al. 1990; Maddox et al. 1996). We find that taking account of
non-radial motions in the calculation of the angular correlation function gives
a better agreement of the theoretical prediction of the SCDM model to the
observed estimates of large-scale power in the galaxy distribution.
