  High-resolution numerical simulations of galaxy mergers are analysed. The
global structure and isophotal shapes of the merger remnants are in good
agreement with the observations. Whereas equal-mass mergers lead to
anisotropic, boxy ellipticals, unequal-mass mergers result in disky and
isotropic systems. The line-of-sight velocity distributions show small
deviations from a Gaussian distribution. In all cases we find that the
retrograde wings are steeper and that the prograde wings are broader than a
Gaussian distribution. This is in contradiction with the observations which
show broader retrograde and steeper prograde wings in all ellipticals. This
fundamental difference between observation and theory can be explained if all
ellipticals, even anistropic boxy ones, contain extended stellar disk
components with luminosities of order 10 to 20 percent the total luminosity and
scale radii of order the effective radii of the spheroids.
