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Fig. 1

image

l = 2 perturbation mode of a spherical harmonics (central) over the unperturbed axisymmetric system (left). We exclude perturbation modes other than l = 2 because, although every perturbed 3D surface can be realized by a superposition of spherical harmonics modes, no common evidence exists for the type of symmetries as presented on the right (e.g. l = 3 mode). The dashed-green line provides an example of a star cluster orbit. Note that the tidal tails (yellow zone bordered by the black contours) do not necessarily lie along the orbits, i.e., O(t) ≠ 1 in the formalism of this paper, see, e.g. Pasetto et al. (2010, their Fig. 7) or Dehnen et al. (2004), Capuzzo Dolcetta et al. (2005) for globular cluster cases.

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