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Fig. 17


Same as Fig. 11 for a thick disc stellar particle evolution in the orbits integration (first row and thin lines ofthird row) and in the simulation (second row and thick lines of third row) in which the stellar particle is an extreme migrator. The lack dash-dotted line shows time evolution of the corotation radius (bottom left panel) and of Ωp (bottom right panel) in the simulations.

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