  It is generally believed that major galaxy mergers with mass ratios in the
range 1:1-3:1 result in remnants that have properties similar to elliptical
galaxies, and minor mergers below 10:1 result in disturbed spiral galaxies. The
intermediate range of mass ratios 4:1-10:1 has not been studied so far. Using
N-body simulations, we show that such mergers can result in very peculiar
systems, that have the morphology of a disk galaxy with an exponential profile,
but whose kinematics is closer to that of elliptical systems. These objects are
similar to those recently observed by Jog & Chitre (2002). We present two cases
with mass ratios 4.5:1 and 7:1, and show that the merging causes major heating
and results in the appearance of elliptical-type kinematics, while surprisingly
the initial spiral-like mass profile is conserved.
