0.8 and 0.9 for all simulations. The evolution of $c/a$ is more interesting. It grows from the original value of 0.12 up to the value ranging from 0.43 for I90VY2 (Dwarf1) to 0.86 for I60R. For radial mergers, there is a simple rule for the behavior of $c/a$: the final ratio decreases when the initial angle between the angular momenta of the dwarfs increases, i.e. the merger remnants become thinner. For merger I90VY2 $b/a$ remains similar for both dwarfs but $c/a$ is significantly different (0.43 for Dwarf1 and 0.73 for Dwarf2). In the later stages of the simulations, all dwarfs can be classified as triaxial. Only I90VY1 crosses the line of the oblate shape in several time steps and Dwarf2 of I90VY2 has more prolate values of triaxiality.

Referring again to Fig. \[fig:maps\] we note that the shapes of the merger remnants also differ in terms of their boxiness. In this respect, the dependence seems to be the strongest for the radial mergers. Clearly, the simulation with the dwarf disks oriented most vertically (I60R) with respect to the merger axis the isodensity contours are most boxy. In order to make this statement more quantitative we calculated the Fourier mode $A_4$ 