in all outputs almost all particles inside 2kpc have current total angular momentum smaller than 1M$_{\sun}$kpc$^{2}$Myr$^{-1}$). When the figure rotation is present the box orbits acquire some net angular momentum [@schw82] thus we call this group just *low angular momenta* orbits. It is worth noting that $L_{y'}$ and $L_{z'}$ of most of the particles average out to zero and $L_{xy'z'}$ is typically dominated by the average value of $L_x$.

The rest of the particles, which do not fall into one of the above categories, are marked as *other*. These particles have $L_{xy'z'}>0.1$M$_{\sun}$kpc$^{2}$Myr$^{-1}$ and at the same time they do not keep a constant sign of $L_x$ for the duration of the last 4Gyr of the simulation.

Fig. \[fig:orbfra\] shows fractions of the three types of orbits as a function of radius in the final outputs of the simulations. The fraction of long-axis tubes correlates tightly with the amount of the mean rotation velocity of particles discussed in section \[sub:rot\]. Galaxies with higher rotation have faster increase of the fraction of long-axis tubes with radius, mainly at the expense of the low angular momenta orbit family.

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Orbital frequencies
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For the long-axis tubes we computed the average angular 