relative velocities. The numerical realization of the dwarf galaxy is the same as used previously in simulations of tidal stirring by @lo14bar and @lo15. The model was generated following the method described in @wid05 and @wid08 which allows to create self-consistent, equilibrium $N$-body models of galaxies with an exponential disk and an NFW halo [@nfw97].

Our dwarf galaxy had a dark matter component in the form of the NFW halo of total mass $M_{\mathrm{h}}=10^9$M$_{\sun}$ and concentration parameter $c=20$. The exponential disk had the mass of $M_{\mathrm{d}}=2\times10^7$M$_{\sun}$, the scale-length $R_{\mathrm{d}}=0.41$kpc and thickness $z_{\mathrm{d}}/ R_{\mathrm{d}}=0.2$. Each component of the dwarf contained $10^6$ particles (which makes the total of $4\times10^6$ particles per simulation). The mergers were followed using the $N$-body simulation code GADGET-2 [@sp05] with the adopted softening scale lengths of $0.02$kpc and $0.06$kpc for the disk and halo particles, respectively. Each merger was evolved for 10Gyr with positions and velocities of the particles stored every 0.05Gyr.

We chose the coordinate system of the simulation box so that its origin was at the center of gravity of the two dwarfs. Dwarf1 was always placed at coordinates $(X,Y,Z)=(-25,0,0)$kpc and Dwarf2 at $(25,0,0)$kpc. For radial mergers $X$ is the original collision axis, for the other 