  We expand our pervious numerical study of the properties of the stellar
velocity distribution within the disk of a two-armed spiral galaxy by
considering spiral stellar density waves with different global Fourier
amplitudes, C_2. We confirm our previous conclusion that the ratio
\sigma_1:\sigma_2 of smallest versus largest principal axes of the stellar
velocity ellipsoid becomes abnormally small near the outer edges of the stellar
spiral arms. The extent to which the stellar velocity ellipsoid is elongated
(as compared to the unperturbed value typical for the axisymmetric disk)
increases with the strength of the spiral density wave. In particular, the
C_2=0.06 spiral can decrease the unperturbed value of \sigma_1:\sigma_2 by 20%,
while the C_2=0.13 spiral can decrease the unperturbed \sigma_1:\sigma_2 by a
factor of 3. The abnormally small values of the \sigma_1:\sigma_2 ratio can
potentially be used to track the position of {\it stellar} spiral density
waves. The \sigma_{\phi\phi}:\sigma_{rr} ratio is characterized by a more
complex behaviour and exhibits less definite minima near the outer edges of the
spiral arms. We find that the epicycle approximation is violated near the
spiral arms and cannot be used in spiral galaxies with C_2 >= 0.05-0.06 or in
galaxies with the amplitude of the spiral stellar density wave (relative to the
unperturbed background) of order 0.1 or greater.
