  N-body simulations of major spiral-spiral mergers with different mass ratios
q <= 4:1 are presented. All mergers lead to spheroidal stellar systems with de
Vaucouleurs-like surface density profiles, resembling elliptical galaxies. The
internal dynamical structure of the remnants does however depend critically on
the adopted mass ratio. Equal-mass mergers with q <= 2:1 form radially
anisotropic, slowly rotating systems with preferentially boxy isophotes.
Unequal-mass mergers with q > 2:1 result in the formation of rotationally
supported ellipticals with disky isophotes and small minor axis rotation.
Projection effects lead in general to a large scatter in the kinematical and
isophotal properties. If the observed dichotomy between boxy and disky
ellipticals is a result of different mass ratios of the merger components
massive ellipticals must have formed preferentially from equal-mass mergers in
contrast to low-mass ellipticals which had to form from unequal-mass mergers.
