We note that Dwarf1 of I90VY2 (on the right side of the panel) is notably more deformed than Dwarf2. In the second-column panels dwarfs are located near their first apocenters and the third-column snapshots roughly correspond to the time when the centers of the dwarfs have just merged, but the merger remnant is still far from equilibrium. The last-column panels are the final snapshots from the simulations, after 10 Gyr of evolution.

Kinematics and shape
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Prolate rotation {#sub:rot}
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In order to check how much prolate rotation is present in each merger remnant, we found the principal axes of the stellar component of each dwarf separately and computed the mean rotation velocity around the major axis in the sphere of radius 2kpc centered on the center of the respective dwarf. We plot the evolution of this rotation in time for Dwarf1 for all simulations in Fig. \[fig:rot\].

Due to the symmetry of the initial conditions in radial mergers, the evolution of this rotation in Dwarf1 is the same as for Dwarf2 in the same simulation. For I90VY1, the asymmetry is too small to lead to significant differences between the two dwarfs. On the other hand, in the case of 